Post on 22-Aug-2020
Submitted to the National Science Foundation under Cooperative Agreement No. 0946422
and Cooperative Support Agreement No. 0950946
This report is also published on the NSO Web site: http://www.nso.edu
The National Solar Observatory is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under
cooperative agreement with the National Science Foundation
NATIONAL SOLAR OBSERVATORY
NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
MISSION
The mission of the National Solar Observatory (NSO) is to provide
leadership and excellence in solar physics and related space, geophysical,
and astrophysical science research and education by providing access to
unique and complementary research facilities as well as innovative
programs in research and education and to broaden participation in
science.
NSO accomplishes this mission by:
providing leadership for the development of new ground‐based facilities that
support the scientific objectives of the solar and space physics community;
advancing solar instrumentation in collaboration with university researchers,
industry, and other government laboratories;
providing background synoptic observations that permit solar investigations from
the ground and space to be placed in the context of the variable Sun;
providing research opportunities for undergraduate and graduate students, helping
develop classroom activities, working with teachers, mentoring high school
students, and recruiting underrepresented groups;
innovative staff research.
RESEARCH OBJECTIVES
The broad research goals of NSO are to:
o Understand the mechanisms generating solar cycles – Understand mechanisms
driving the surface and interior dynamo and the creation and destruction of
magnetic fields on both global and local scales.
o Understand the coupling between the interior and surface – Understand the
coupling between surface and interior processes that lead to irradiance variations
and the build‐up of solar activity.
o Understand the coupling of the surface and the envelope: transient events –
Understand the mechanisms of coronal heating, flares, and coronal mass
ejections which lead to effects on space weather and the terrestrial atmosphere.
o Explore the unknown – Explore fundamental plasma and magnetic field
processes on the Sun in both their astrophysical and laboratory context.
NATIONAL SOLAR OBSERVATORY
NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
TABLE OF CONTENTS
EXECUTIVE SUMMARY ....................................................................................................................... 1
1 INTRODUCTION............................................................................................................................... 5
2 FY 2013 SCIENTIFIC RESEARCH & DEVELOPMENT HIGHLIGHTS ................................... 6
2.1 Full‐Disk Nonlinear Force‐Free Field Extrapolation – Comparing SOLIS/VSM
and SDO/HMI Magnetograms .......................................................................................... 6
2.2 The Quasi‐Biennial Periodicity as a Window on the Solar Magnetic Dynamo
Configuration (the Sunʹs Two‐Year Period and Its Drivers) ......................................... 7
2.3 Active Regions with Superpenumbral Whirls and Their Subsurface
Kinetic Helicity ..................................................................................................................... 8
2.4 He I Vector Magnetometry of Field‐Aligned Superpenumbral Fibrils ........................ 8
2.5 1565 nm Observations of the Transit of Venus, Proxy for a Transiting Exoplanet ...... 9
2.6 Velocity and Magnetic Field Distribution in a Forming Penumbra ............................ 10
2.7 The Properties of Flare Kernels Observed by the Dunn Solar Telescope ................... 11
3 SCIENTIFIC AND KEY MANAGEMENT STAFF ..................................................................... 13
4 SUPPORT TO PRINCIPAL INVESTIGATORS AND THE SOLAR‐TERRESTRIAL
PHYSICS COMMUNITY ................................................................................................................ 16
4.1 Dunn Solar Telescope ......................................................................................................... 17
4.1.1 Adaptive Optics ................................................................................................................ 18
4.1.2 DST Instrumentation ....................................................................................................... 19
4.1.3 Replacements and Upgrades .......................................................................................... 21
4.1.4 Current and Future Use of the DST ............................................................................... 22
4.1.5 Divestiture Planning ........................................................................................................ 22
4.2 McMath‐Pierce Solar Telescope ................................................................................. 22
4.2.1 Diverse Observing Capabilities ....................................................................................... 23
4.2.2 Divestment or Closure of the McMP ............................................................................. 23
4.2.3 Impacts of Early Closure of the McMP .......................................................................... 24
4.2.4 Collaboration with the New Solar Telescope Cyra Development ............................. 24
4.2.5 Current Programs .............................................................................................................. 25
4.3 NSO Integrated Synoptic Program ................................................................................... 26
4.3.1 NISP Instrumentation ...................................................................................................... 26
4.3.2 NISP Data Products ........................................................................................................ 27
4.3.3 NISP Status ..................................................................................................................... 28
4.3.4 NISP 2014 Goals .............................................................................................................. 30
4.4 Evans Solar Facility ............................................................................................................. 31
4.5 Access to NSO Data ............................................................................................................ 31
NATIONAL SOLAR OBSERVATORY
NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
5 INITIATIVES: THE ATST AND THE NEW SYNOPTIC NETWORK ................................... 34
5.1 Advanced Technology Solar Telescope (ATST) ............................................................. 34
5.1.1 ATST Science Working Group and Science Requirements ........................................ 36
5.1.2 ATST Project Engineering and Design Progress .......................................................... 38
5.1.3 Funding ..................................................................................................................... 41
5.2 A Multi‐Purpose Global Network .................................................................................... 43
6 EDUCATION AND PUBLIC OUTREACH AND BROADENING PARTICIPATION ....... 47
6.1 Goals and Metrics ............................................................................................................... 47
6.2 Recruiting a New Generation of Scientists ...................................................................... 50
6.3 Increasing Diversity ............................................................................................................ 51
6.3.1 Near‐Term Goals: .............................................................................................................. 52
6.3.2 Long(er)‐Term Goals: ....................................................................................................... 52
6.4 Public Outreach ................................................................................................................... 54
6.4.1 Visitor Centers ................................................................................................................... 54
6.4.2 Internet Resources and Public Web Pages .................................................................... 54
7 FY 2014 PROGRAM IMPLEMENTATION ................................................................................... 55
7.1 NSO Organization ............................................................................................................. 55
7.1.1 Director’s Office ................................................................................................................ 55
7.1.2 NSO/Sacramento Peak ..................................................................................................... 55
7.1.3 NSO Tucson and NSO Synoptic Program .................................................................... 56
7.1.4 NSO ATST ..................................................................................................................... 57
7.2 Planning for the Future Organization of NSO ................................................................ 57
7.3 FY 2014 Spending Plan ....................................................................................................... 58
7.3.1 Total Budget ..................................................................................................................... 58
7.3.2 Work Package Break Out ................................................................................................ 61
7.4 Infrastructure Plan and Strategic Needs .......................................................................... 65
7.4.1 FY 2014 Unfunded Infrastructure Improvement Requests ....................................... 66
APPENDICES ......................................................................................................................................... 69
APPENDIX A:. NATIONAL SOLAR OBSERVATORY 2020–2025 VISION ......................... 70
APPENDIX B: OBSERVING AND USER STATISTICS .............................................................. 72
APPENDIX C: ORGANIZATIONAL PARTNERSHIPS ............................................................... 75
C1. Community Partnerships and NSO Leadership Role .............................................. 75
C2. Operational Partnerships .............................................................................................. 76
NATIONAL SOLAR OBSERVATORY
NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
APPENDIX D: PUBLICATIONS (OCTOBER 2012 THROUGH SEPTEMBER 2013) ............. 77
APPENDIX E: MILESTONES FY 2014 ............................................................................................. 90
APPENDIX F: STATUS OF FY 2013 MILESTONES ..................................................................... 94
APPENDIX G: NSO FY 2014 STAFFING SUMMARY ................................................................ 103
APPENDIX H: SCIENTIFIC STAFF RESEARCH AND SERVICE ........................................... 104
APPENDIX I: ACRONYM GLOSSARY ......................................................................................... 129
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1 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
EXECUTIVE SUMMARY
The National Solar Observatory (NSO) is the primary provider of key ground‐based solar
facilities to the US solar community. NSO currently provides a range of assets that allow solar
astronomers to probe all aspects of the Sun, from the deep interior to its interface in the corona
with the interplanetary medium. NSO provides scientific and instrumentation leadership in
helioseismology, synoptic observations of solar variability, and high‐resolution studies of the
solar atmosphere in the visible and infrared.
Major components of the National Solar Observatory strategic planning include:
Developing the 4‐meter Advanced Technology Solar Telescope (ATST) on behalf of, and
in collaboration with, the solar community.
Development of the adaptive optics (AO), multi‐conjugate AO (MCAO), and infrared (IR)
technology needed for the ATST.
Operating the Dunn Solar Telescope (DST) and maintaining its competitiveness through
adaptive optics, MCAO and state‐of‐the‐art instrumentation until the ATST nears first
light.
Helping the scientific consortium that plans to assume operation of the McMath‐Pierce
Solar Telescope (McMP) in a timely fashion to meet the NSF mandate to divest or close
the facility.
Finding organizations (such as the Southern Rockies Education Centers or universities
with potential interest) to assume operation of Sacramento Peak and a logical transition
for the Dunn Solar Telescope.
Operating a suite of instruments comprising the NSO Integrated Synoptic Program
(NISP). This includes the Synoptic Optical Long‐term Investigation of the Sun (SOLIS)
and the Global Oscillation Network Group (GONG).
Establishing funding partners for the operation of NISP.
Developing partnerships to establish a multi‐station synoptic network.
Increasing diversity of the solar workforce.
An orderly transition to a new NSO structure, which can efficiently operate ATST and
NISP and continue to advance the frontiers of solar physics. This new structure will have
its headquarters collocated with the University of Colorado, Boulder and will integrate
the NSO staff currently divided between sites at Sunspot, New Mexico and in Tucson,
Arizona. Some of the programmatic highlights of the NSO program in FY 2014 include:
Continuation of ATST construction on Haleakalā.
Increasing the NSO footprint at the University of Colorado, Boulder (CU‐Boulder).
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Delivery of several ATST key components such as the telescope enclosure and the high‐
order AO real‐time hardware.
Continue the Service Mode tests at the Dunn Solar Telescope and study possible ways to
improve user experience, providing help to the PIs with the data reduction pipelines.
Appointment of a new ATST Data Center Project Manager.
Appointment of a transition team and a single point of contact with CU.
A few of the major actions to advance solar physics that NSO will undertake in FY 2014 include:
Continuing the construction of ATST through the NSF Major Research Equipment
Facilities Construction (MREFC) program.
Developing a complete transition plan for NSO during the period 2015‐2017 that
describes the various steps and milestones needed to have the institution relocated to the
Boulder and Maui facilities.
Working toward the responsible divestiture of the McMath‐Pierce Telescope Facility and
Sacramento Peak.
Continuing early moves to Boulder by leasing office space at the CU‐Boulder Laboratory
for Atmospheric and Space Physics (LASP).
Providing specifications to LASP for the NSO needs in remodeling the 3rd floor of the new
LASP building.
Continuing to work with CU‐Boulder on faculty appointments.
Conducting additional testing of service‐mode observations at the Dunn Solar Telescope.
Finishing the SOLIS program by reaching full functionality of the vector spectromagneto‐
graph (VSM) guider and installing and calibrating the visible tunable filter (VTF).
Initiating the upgrade of the SOLIS VSM for chromospheric vector magnetic field
measurements as requested by the solar community
Figure 1 summarizes NSO’s FY 2014 program plans. In the President’s budget released in
February 2013, NSO’s FY 2014 budget remains flat at $8M. This will continue to put pressure
on current operations. Implementation of the NSF Portfolio Review made it clear that we
should work toward divestiture of current facilities by the end of FY 2017. Closure of the DST
before ATST is on line leaves a gap in US high‐resolution capabilities. We will work with the
Big Bear Solar Observatory (BBSO) and the European community to obtain access for the US
community to their facilities, and we will work with the NSF to understand how to pay for such
access. A DST Data Center that contains the observations compiled during the service‐ mode
activities is being studied as a possible way to offer the community access to high‐spatial
resolution data during the gap until ATST becomes fully functional. Early closure of the McMP eliminates NSO capabilities beyond ~2 microns, which will be an
important wavelength regime for the ATST. Until the advent of the ATST, these capabilities
will only be accessible to tha US community at the NJIT BBSO New Solar Telescope (NST).
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The ATST project has begun construction on Maui and has contracts in place for all of its major
components. Rapid progress on the enclosure is being made. Its shipment is expected to occur
in 2014. Delivery of some items has begun. The Visible Broadband Imager (VBI), which serves
as a pathfinder for the other ATST instruments, had its final design review (FDR) and many of its
parts have been manufac‐tured and tested. Critical design reviews (CDR) for other ATST
instruments have been scheduled in 2014.
The NSO Integrated Synoptic Program was formed in July 2011, and combines the GONG and
SOLIS programs. These programs have similar scientific goals and share a number of technical
approaches; thus the merger has resulted in improved system efficiency and increased scientific
synergy. Bringing NISP from a budget level of over $4M to $2M will seriously reduce the level
of support NSO can provide this important program. Additional non‐astronomy funding is
being actively sought.
NSO’s FY 2014 spending plan (Section 7) attempts to accommodate the reduced budget while
still supporting the user community and an ATST operations model. To ensure that the next
generation that will form the core of ATST users is well trained, NSO will support the
resurgence of significant interest in producing high‐resolution images with existing facilities
using adaptive optics and new diffraction‐limited instruments. To support the importance the
Solar and Space Physics Decadal Survey placed on synoptic measurements, NSO will work with
other agencies to find the funding needed to support a robust NISP program.
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NSO 2014 Program
ATST
o Continue construction on Haleakalā.
o Develop concepts for ATST data center.
Dunn Solar Telescope (all ATST related activities)
o Continue development of multi-conjugate adaptive optics (MCAO). o Test bed for ATST instrument development. o Conduct PI and service mode observations for the solar
community.
McMath-Pierce Solar Telescope
o Begin to implement transition to consortium of users.
o Continue IR observations.
o Continue synoptic sunspot magnetic field strength measurements.
NSO Integrated Synoptic Program (NISP)
o Operate SOLIS and GONG instruments.
o Develop partnerships for a synoptic network.
o Continue to seek outside operation funding.
Digital Library and Virtual Solar Observatory
o Begin transition of data storage to Boulder.
New NSO Directorate Site and Staff Consolidation
o Negotiate with the University of Colorado, Boulder terms for the lease of building space.
o Develop plans for relocation of staff.
Education and Outreach and Broadening Participation
o Train the next generation of solar astronomers (REU's, SRA's, thesis students, postdocs).
o Coordinate with the Akamai Workforce Initiative and University of Hawai‘i Maui College on workforce development on Maui.
o Increase outreach to underrepresented minorities.
Figure 1. Planned and ongoing programs and projects at NSO.
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1 INTRODUCTION
While solar research continues to make progress in many areas of observation and theory, there
remains many unanswered questions about how solar activity and variability are driven. The
extreme difficulty of measuring and modeling the solar magnetic field underlies many of these
questions.
NSO remains on a path to achieve these objectives as outlined in its strategic Long Range Plan
(LRP). These include bringing the ATST on line, establishing a new NSO directorate site where
we can consolidate our scientific staff, and developing a robust synoptic program. This Annual
Progress Report and Program Plan highlights the progress during implementation of NSO’s FY
2013 program and plans for FY 2014. Part of our efforts in FY 2013 included the development of
a ten‐year Cooperative Agreement proposal.
Section 2 provides a brief description of both science and development highlights achieved with
NSO facilities and projects. Section 3 provides a description of scientific and key management
staff. Section 4 describes NSO tools and facilities and the support they provide the solar user
community. Section 5 describes our major initiatives and Section 6 presents the major aspects of
our Educational and Public Outreach (EPO) plan and our plan to increase diversity at NSO and
in the solar community. Finally, Section 7 lays out the FY 2014 organization and spending plan
needed to carry out the NSO program. The appendices contain user statistics, list of
publications, status of 2013 project milestones and milestones for FY 2014, a staffing table, and
descriptions of scientific staff research.
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2 FY 2013 SCIENTIFIC RESEARCH & DEVELOPMENT HIGHLIGHTS
2.1 Full‐Disk Nonlinear Force‐Free Field Extrapolation – Comparing SOLIS/VSM and
SDO/HMI Magnetograms The magnetic field configuration is essential for understanding solar explosive phenomena, such
as flares and coronal mass ejections. To compensate for the unavailability of coronal magnetic field
measurements, which are extremely difficult to make, photospheric magnetic field vector data are
often used to reconstruct the coronal field by extrapolation. The use of full‐disk vector magneto‐
grams allows the extrapolation models to better represent the global magnetic connectivity
between separate active regions and to estimate free magnetic energy and large‐scale distribution
of electric currents—key parameters that characterize the flare potential of solar active regions.
T. Tadesse, T. Wiegelmann, B. Inhester, P. MacNeice, A. A. Pevtsov, and X. Sun (A&A 550, A14,
2013) used photospheric magnetic field measurements from the SOLIS Vector Spectromagneto‐
graph (VSM) and the SDO Helioseismic and Magnetic Imager (HMI) to model the coronal field
above multiple solar active regions, assuming magnetic forces to dominate. They solved the
nonlinear force‐free field (NLFFF) equations by minimizing a functional in spherical coordinates
over a full disk and compared the models with the coronal images from the SDO Atmospheric
Imaging Assembly (AIA). Tadesse and colleagues found that magnetic field lines obtained from
nonlinear force‐free extrapolation based on VSM and HMI data show good agreement. The
average vector correlation between the NLFFF fields of HMI and VSM data is 0.94. There are some
differences, however. For example, extrapolated field lines from SDO/HMI magnetogram (Figure
2.1‐1) do not show transequatorial loops connecting trailing polarity of NOAA AR 11339 (west of
central meridian in northern hemisphere) and trailing polarity of AR11338 (southern hemisphere).
These transequatorial loops are well represented by NLFFF extrapolation based on SOLIS/VSM.
This difference can be attributed to presence of a patch of weak fields between two active regions
(in SDO/HMI data). With this weak field patch, SDO/HMI model tends to close field lines
originating in trailing polarity of AR11339, while SOLIS/VSM model extends them to AR11338.
Overall coronal connectivity observed in SDO/AIA images is well represented by both models.
Figure 2.1‐1. a) SOLIS (left) and b)
HMI (right) magnetograms using NLFFF
modeling. The gray‐scale color coding
shows radial component Br of magnetic
field on the photosphere (white/black
corresponds to positive/negative polarity).
Yellow lines represent closed field lines,
while field lines changing in color from
yellow to brown (from bottom to the top)
represent the open ones. The gray area
indicates the region where magnetic field
values are close to zero.
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Reconstructed magnetic field based on SDO HMI data yield larger total magnetic energy and
about 14.4% more free magnetic energy as compared with SOLIS VSM data. The density of surface
electric currents is also larger for the model based on SDO HMI data. The disagreement in the
energy content and density of electric currents is attributed to stronger transverse fields in SDO
HMI measurements.
2.2 The Quasi‐Biennial Periodicity as a Window on the Solar Magnetic Dynamo
Configuration (the Sunʹs Two‐Year Period and Its Drivers)
Manifestations of the solar magnetic activity through periodicities of about 11 and 2 years are now
clearly seen in all solar activity indices. R. Simoniello, K. Jain, S. Tripathy, S. Turck‐Chièze, C.
Baldner, W. Finsterle, F. Hill, and M. Roth (ApJ 765, 2013) investigated the mechanism driving the
two‐year period by studying the time and latitudinal properties of acoustic modes that are
sensitive probes of the subsurface layers. Almost 17 years of high‐quality resolved data provided
by NISP/GONG have been used in this investigation to provide a better understanding of the solar
cycle related changes in p‐mode frequencies. For both periodic components of solar activity, the
origin of the frequency shift is found to be located in the subsurface layers with evidence of a
sudden enhancement in amplitude occurring in just the last few hundred kilometers. It is also
shown that, in both cases, the magnitude of the shift increases toward equatorial latitudes and
from minimum to maximum solar activity, in agreement with previous findings. The quasi‐
biennial periodicity (QBP), however, causes a weaker shift in mode frequencies and a slower
enhancement than that caused by the 11‐year cycle. These observational findings are compared
with the features predicted by different models to explain the origin of this QBP, and it is
concluded that the observed properties could result from the beating between a dipole and
quadrupole magnetic configuration of the solar dynamo.
Figure 2.2‐1. a) Temporal variation of mean frequency shifts (symbols). The errors in frequency shifts are smaller than the
size of the symbols. The solid line represents the dominant 11‐year signal of the solar cycle as calculated by applying a
boxcar filter of width of about two years. b) The top panel shows the residual shifts after removing the 11‐year signal, while
the bottom panel depicts the local wavelet power spectrum; white representing areas of little power, red with the largest
power. c) Global wavelet power spectrum. The dotted line is 90% confidence level.
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Figure 2.3‐1. In this GONG H‐alpha image, NOAA
11092 is a medium region in the northern hemisphere
with a counter‐clockwise whirl.
2.3 Active Regions with Superpenumbral
Whirls and Their Subsurface Kinetic Helicity
R. Komm, S. Gosain, A. Pevtsov (SoPh Online
First (18 pp.), 2013) search for a signature of
helicity flow from the solar interior to the photo‐
sphere and chromosphere. For this purpose, they
study two active regions, NOAA 11084 and 11092,
that show a regular pattern of superpenumbral
whirls in chromospheric and coronal images.
These two regions are good candidates for com‐
paring magnetic/current helicity with subsurface
kinetic helicity because the patterns persist
throughout the disk passage of both regions. They
use photospheric vector magnetograms from the
SOLIS Vector Spectromagnetograph and SDO
Helioseismic and Magnetic Imager to determine a
magnetic helicity proxy, the spatially averaged
signed shear angle (SASSA). The SASSA parameter
produces consistent results, leading to positive values for NOAA 11084 and negative ones for
NOAA 11092, consistent with the clockwise and counter‐clockwise orientation of the whirls. They
then derive the properties of the subsurface flows associated with these active regions. They
measure subsurface flows using a ring‐diagram analysis of GONG high‐resolution Doppler data
and derive their kinetic helicity. The sign of the subsurface kinetic helicity is negative for NOAA
11084 and positive for NOAA 11092; the sign of the kinetic helicity is thus anticorrelated with that
of the SASSA parameter. As a control experiment, Komm and colleagues study the subsurface
flows of six active regions without a persistent whirl pattern. Four of the six regions show a
mixture of positive and negative kinetic helicity, resulting in small average values, while two
regions are clearly dominated by kinetic helicity of one sign or the other, as in the case of regions
with whirls. The regions without whirls follow overall the same hemispheric rule in their kinetic
helicity as in their current helicity with positive values in the southern and negative values in the
northern hemisphere.
2.4 He I Vector Magnetometry of Field‐Aligned Superpenumbral Fibrils
Atomic‐level polarization and Zeeman effect diagnostics in the neutral helium triplet at 10830 Å in
principle allow full vector magnetometry of fine‐scaled chromospheric fibrils. T. A. Schad, M.
Penn, and H. Lin (ApJ 768:111 (17pp), 2013) present high‐resolution spectropolarimetric obser‐
vations of super‐penumbral fibrils in the He I triplet with sufficient polarimetric sensitivity to infer
their full magnetic field geometry. He I observations from the Facility Infrared Spectropolarimeter
(FIRS) are paired with high‐resolution observations of the Hα 6563 Å and Ca II 8542 Å spectral
lines from the Interferometric Bidimensional Spectrometer (IBIS) at the Dunn Solar Telescope.
Linear and circular polarization signatures in the He I triplet were measured and analyzed with
the advanced inversion capability of the “Hanle and Zeeman Light” modeling code (HAZEL, A.
Ramos, J. Trujillo Bueno, & E. Landi Degl’Innocenti, E., ApJ 683, 542, 2008). Their analysis provides
direct evidence for the often assumed field alignment of fibril structures.
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Figure 2.4‐1. Thirty‐nine fibrils
manually traced by inspection of the
entire observed He I spectral data
cube using CRISPEX. The fibrils
traced constitute curvilinear features
of greater absorption and account for
lateral variations of the Doppler shift
and width of the He I triplet.
Figure 2.4‐2. Photospheric magnetic field vector in local solar coordinates for the entire FIRS field of view derived from a Milne–
Eddington analysis of the Si I 10827.089 Å spectral line. The selected fibrils are also overplotted. The arrows denote the locations of
the photospheric magnetic field with opposite polarity with regard to the sunspot umbra.
The projected angle of the fibrils and the inferredmagnetic field geometry align within an error of
±10◦ (Figures 2.4‐1 and 2.4‐2). They describe changes in the inclination angle of these features that
reflect their connectivity with the photospheric magnetic field. Evidence for an accelerated flow
(∼40 m s−2) along an individual fibril anchored at its endpoints in the strong sunspot and weaker
plage in part supports the magnetic siphon flow mechanism’s role in the inverse Evershed effect.
However, the connectivity of the outer endpoint of many of the fibrils cannot be established.
2.5 1565 nm Observations of the Transit of Venus, Proxy for a Transiting Exoplanet
The transit of Venus in June 2012 provided a unique chance to view a well studied planetary
atmosphere as we might see that of a transiting exoplanet, through scattered and refracted
illumination of its parent star. This is the second time that the IR atmospheric transmission of
Venus has been measured during a transit; previous observations were made with the Tenerife
Infrared Polarimeter during the 2004 transit by Hedelt et al. (2011), who confirmed well
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established isotopic abundances and atmospheric scale height. S. Jaeggli, K. Reardon, J. Pasachoff,
G. Schneider, T. Widemann, and P. Tanga (AAS SPD meeting #44, Bozeman, MT, 2013), performed
spectroscopy and polarimetry during the transit of Venus, focusing on extracting signatures of CO2
absorption. Observations were taken during the first half of the transit using the Facility InfraRed
Spectropolarimeter (FIRS) on the Dunn Solar Telescope. An average spectrum of the off‐limb arc,
or aureole, was taken while Venus was crossing onto the solar limb. The spectra in the figure were
produced by averaging over the aureole (top panel), the average off‐limb stray light spectrum was
subtracted and the residual solar spectrum was divided (middle panel), and a line spectrum was
made by averaging over the spatial extent of the arc (bottom panel). A synthetic spectrum of the
Venus model atmosphere provided by Pascal Hedelt was resampled and convolved with the FIRS
spectrograph profile determined from laser measurements by Jaeggli (2011) to produce the model
spectrum shown in violet. The strong agreement between the observed and model spectra is
highly encouraging for further analysis of this dataset. Polarimetry was performed after Venus
had moved onto the
solar disk, however no
polarization signal from
Venus is apparent even
in highly averaged data. The transit also pro‐
vided the opportunity
to characterize stray
light and other instru‐
mental properties of
FIRS. The off‐limb scans
during the transit
revealed that the ap‐
parent uniform stray
light background is
actually a faint and
spatially offset version
of the image, probably
due to a back‐
reflection upstream
from the spectrograph
in the telescope. The analysis of the Venus data also leads to further analysis of optical and digital
fringes due to the infrared optics and array detector respectively. More rigorous analysis and
removal of the fringe patterns will greatly improve analysis of this and other datasets from FIRS.
2.6 Velocity and Magnetic Field Distribution in a Forming Penumbra
The formation process of the penumbra in sunspots presents several aspects that are not yet well
understood because of the difficulty of observing this rather fast process, which has a duration of
a few hours, with high spectral, spatial, and temporal resolution. P. Romano, D. Frasca, S.
Figure 2.5‐1. Spectra produced by averaging over the aureole (top panel); the average off‐limb
stray light spectrum was subtracted and the residual solar spectrum was divided (middle
panel); a line spectrum (bottom panel) was made by averaging over the spatial extent of the arc.
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Figure 2.6‐1. Snapshots of the emerging part of NOAA AR 11490 as seen in the broadband image (left panel), in the Ca II line
center image (middle panel), and in the circular polarization map (right panel) taken by IBIS at ~14:20 UT. North is at the top,
west is on the right. The contours indicate the edge of the pore as seen in the corresponding broadband image.
Guglielmino, I. Ermolli, A. Tritschler, K. Reardon, and F. Zuccarello, (ApJ 771, L3, 2013) present
results from the analysis of high‐resolution spectropolarimetric and spectroscopic observations of
the solar photosphere and chromosphere, obtained shortly before the formation of a penumbra in
one of the leading polarity sunspots of NOAA active region 11490. The observations were performed at the Dunn Solar Telescope on 28 May 2012, using the
Interferometric Bidimensional Spectrometer (IBIS). The dataset comprises a one‐hour time
sequence of measurements in the Fe I 617.3 nm and Fe I 630.25 nm lines (full Stokes polarimetry)
and in the Ca II 854.2 nm line (Stokes I only). Romano and colleagues performed an inversion of
the Fe I 630.25 nm Stokes profiles to derive magnetic field parameters and the line‐of‐sight (LOS)
velocity at the photospheric level. They characterized chromospheric LOS velocities by the
Doppler shift of the centroid of the Ca II 854.2 nm line. They found that, before the formation of
the penumbra, an annular zone of 3ʺ‐ 5ʺ width is visible around the sunspot. In the photosphere,
they found that this zone is characterized by an uncombed structure of the magnetic field,
although no visible penumbra has formed yet. They also found that the chromospheric LOS
velocity field shows several elongated structures characterized by downflow and upflow motions
in the inner and outer parts of the annular zone, respectively.
2.7 The Properties of Flare Kernels Observed by the Dunn Solar Telescope
A. Kowalski, L. Fletcher, G. Cauzzi, S. Hawley, and H. Hudson (presented by Fletcher at AAS
SPD meeting #44, Bozeman, MT, 2013), conducted a campaign at the Dunn Solar Telescope which
resulted in successful imaging and spectroscopic obser‐vations of a C1.1 solar flare on 18 August
2011 using the IBIS instrument and the Horizontal Spectrograph in a custom setup. The majority
of a flare’s energy is radiated in the optical and UV part of the spectrum, and the goal of the
campaign was to obtain the flare’s optical spectrum over a wide spectral range, to characterize
the continuum and search for evidence of a Balmer jump. This feature would indicate free‐bound
NATIONAL SOLAR OBSERVATORY
12 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Figure 2.7‐1. Shown here are the finely structured ribbons observed
by IBIS in the continuum near H‐alpha, crossing into a sunspot
umbra. The arrow indicates the kernel where the HSG spectrum is obtained.
emission, one of the mechanisms
proposed for generating a flare’s
white‐light radiation.
The flare exhibited ribbons with
complicated fine structure at the
resolution of the DST/IBIS
instrument, and a number of bright
kernels with sizes comparable to the
smallest scales sampled by IBIS,
around 2‐4 pixels (0.ʺ3‐0.ʺ6) FWHM.
Kowalski et al. focus on these bright
kernels, describing their spatial
characteristics in the core and wing of
H‐alpha and Ca II 8542, and in the
UV and EUV with the Solar
Dynamics Observatory. Preliminary
broadband spec‐troscopy of the kernels shows clearly the presence of an optical continuum in
this small flare, as well as strong high‐order Balmer lines, although a clear Balmer jump is
entirely missing. Some of these characteristics are strikingly similar to the spectral behavior
observed during large flares on active M dwarfs, suggesting physical processes and atmospheric
conditions in common. Detailed calculations are required to fully understand the spectra which
will provide new plasma diagnostics of the ill‐understood lower chromospheric and
photospheric plasma response in solar flares.
Figure 2.7‐2. Shown here is the flare
minus pre‐flare excess spectrum in the
kernel indicated in Figure 2.7‐1, with the
positions of lines, and expected Balmer
jump (BJ). The spectral hump between 3600
and 3700 Å is one of the features observed
in M‐dwarf flares.
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13 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
3 SCIENTIFIC AND KEY MANAGEMENT STAFF
The NSO staff provides support to users including observational support, developing and
supporting state‐of‐the‐art instrumentation to ensure that users obtain the best data, and
maintaining data archives and the means to accessing the data. Members of the scientific staff
are defining how ATST will be operated and how NSO will handle the data. In addition, both
scientific and engineering staff serve as mentors for undergraduate and graduate students and
postdoctoral fellows. They also organize community workshops on critical areas of solar
research and planning. Staff science and instrument development allows NSO to stay at the
forefront of solar physics and play a crucial role in fulfilling user support. The current NSO scientific and management staff, as well as affiliated scientific staff, are listed
below with their primary areas of expertise and key observatory responsibilities.
Scientific Staff
Christian Beck DST visitor and instrument support; solar magnetic fields and
convection; ATST operations development.
Thomas E. Berger Astronomer; ATST Project Scientist.; solar magnetoconvection; high‐
resolution observations.
Luca Bertello NISP/SOLIS Data Scientist; solar vector magnetic fields; helioseismology.
Serena Criscuoli DST visitor and instrument support; solar magnetic fields and
convection; ATST operations development.
David F. Elmore ATST Instrument Scientist; ground‐based spectrograph and filter‐
based polarimeter development.
Mark S. Giampapa Current NSO Deputy Director; stellar dynamos and magnetic activity;
asteroseis‐mology; astrobiology; Ch., NSO/KP Telescope Allocation
Committee; Ch., Scientific Personnel Committee.
Irene E. González
Hernández
Solar Interior Data Scientist; local helioseismology; seismic imaging;
ring‐diagram analysis.
John W. Harvey NISP; solar magnetic and velocity fields; helioseismology; instrumentation.
Frank Hill NSO Associate Director for NISP; solar oscillations; data management.
Stephen L. Keil Solar variability; convection.
Shukur Kholikov Helioseismology; data analysis techniques; time‐distance methods.
John W. Leibacher NISP; helioseismology; atmospheric dynamics.
Valentín Martínez Pillet NSO Director; solar activity; magnetic field measurements;
spectroscopy; polarimetry; astronomical instrumentation.
NATIONAL SOLAR OBSERVATORY
14 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Key Management Staff
Craig Gullixson DST Technical and Project Manager.
Rex G. Hunter NSO budget management; ATST business support; Support Facilities
and Business Manager.
Joseph P. McMullin ATST Project Manager.
Priscilla Piano Administrative Manager: Director’s office and Tucson site support;
NSO grants and NSO budget management.
Kim V. Streander NISP Program Manager; NSO/KP Technical Program & Telescope Manager.
Postdoctoral Fellows
James Lewis Fox Imaging spectroscopy; spectropolarimetric studies of solar prominences.
Sanjay Gosain Spectropolarimetry; solar magnetic fields; instrumentation.
Brian Harker Stokes spectropolarimetry and inversion techniques; automated tracking
and classification of sunspot and active‐region structure; parallel
processing computational techniques for data reduction.
Dirk Schmidt Multi‐conjugate adaptive optics.
Fraser T. Watson Sunspot identification and evolution.
Matthew J. Penn Solar atmosphere; solar oscillations; polarimetry; near‐IR instrumentation;
ATST near‐IR; McMath‐Pierce Facility Scientist.
Gordon J. D. Petrie NISP; solar magnetism; helioseismology.
Alexei A. Pevtsov NISP/SOLIS Atmosphere section Program Scientist; solar activity;
coronal mass ejections; solar magnetic helicity, Sun‐as‐a‐star.
Kevin P. Reardon Data Center Scientist; high‐resolution solar data acquisition and analysis;
ATST data handling, storage and processing.
Thomas R. Rimmele NSO Associate Director for ATST; ATST PI and Project Director; solar
fine structure and fields; adaptive optics; instrumentation.
Alexandra Tritschler ATST operations development; solar fine structure; magnetism; Stokes
polarimetry.
Han Uitenbroek DST Program Scientist; atmospheric structure and dynamics; radiative
transfer modeling of the solar atmosphere; ATST Visible Broadband
Imager
Friedrich Wöger ATST Data Handling Scientist; ATST Visible Broadband Imager PI; high‐
resolution convection; solar fine structure; magnetic fields.
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15 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Thesis Students
Teresa Monsue (Fisk/Vanderbilt U.) Solar flares.
Matthew Richardson (Fisk University) Helioseismology.
Thomas Schad (University of Arizona) IR spectropolarimetry. Grant‐Supported Scientific Staff
Olga Burtseva Time‐distance analysis; global helioseismology; leakage matrix.
Kiran Jain NISP Interior Program Scientist; helioseismology; solar cycle variations;
ring‐diagram analysis; sub‐surface flows.
Rudolf W. Komm Helioseismology; dynamics of the convection zone.
Jose Marino ATST wavefront correction; image restoration.
Sushanta C. Tripathy Helioseismology; solar activity.
Name Adm/Mgt1 Research2 EPO3 Project Support
User Support
Internal Comm.
External Comm.
TOTAL
Beck, C. 52.7 13.5 33.8 100.0
Berger, T.E. 82.0 5.0 1.0 12.0 100.0
Bertello, L. 51.0 31.0 18.0 100.0
**Burtseva, O. 56.7 29.2 14.1 0.0 0.0 100.0
Criscuoli, S. 59.5 1.0 19.2 20.3 100.0
Elmore, D.F. 1.0 1.0 94.0 2.0 2.0 100.0
**Fox, L.J. 66.0 4.0 30.0 100.0
Giampapa, M.S. 57.0 37.7 0.4 0.2 1.6 3.1 100.0
González Hernández , I. 6.0 48.0 24.0 22.0 100.0
Gosain, S. 82.0 10.0 8.0 100.0
**Harker-Lundberg, B.J. 47.0 3.0 50.0 100.0
Harvey, J.W. 27.0 55.0 15.0 1.0 2.0 100.0
Hill, F. 42.0 15.7 3.0 37.0 1.3 1.0 100.0
**Jain, K. 6.0 39.0 55.0 100.0
Keil, S.L. 50.0 5.0 5.0 30.0 5.0 5.0 100.0
Kholikov, S.S. 63.0 23.0 14.0 100.0
**Komm, R.W. 85.0 10.0 5.0 100.0
Leibacher, J.W. 1.0 2.7 2.0 62.7 7.5 24.1 100.0
**Marino, J. 10.0 90.0 100.0xMartinez Pillet, V.
Penn, M.J. 48.6 31.4 12.4 3.0 0.5 4.1 100.0
Petrie, G.J.D. 62.0 8.0 30.0 100.0
Pevtsov, A.A. 48.3 1.7 43.9 1.3 1.0 3.8 100.0
Reardon, K.P. 22.1 51.8 26.1 100.0
Rimmele, T.R. 75.8 1.0 1.0 22.2 100.0
Schmidt, D. 10.0 90.0 100.0
**Tripathy, S.C. 75.0 2.0 20.0 2.0 1.0 100.0
Tritschler, A. 8.7 1.0 85.1 3.1 2.1 100.0
Uitenbroek, H. 47.5 1.0 13.5 16.8 10.8 10.4 100.0
Watson, F. 80.5 0.5 19.0 100.0
Woeger, F. 43.0 6.0 51.0 100.0
Table 3.1 NSO Scientific Staff Estimated Percent FTE by Activity (FY 2013)
x New NSO Director; started 01 Aug. 2013. **Grant supported staff.
1Administrative and/or Management Tasks. 2Research, including participation in scientific conferences. 3Educational and Public Outreach.
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16 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
4 SUPPORT TO PRINCIPAL INVESTIGATORS AND THE SOLAR‐
TERRESTRIAL PHYSICS COMMUNITY
Fulfilling NSO’s mission of providing opportunities to the scientific community and training
the next generation of solar researchers for forefront observations of the Sun require that first‐
class ground‐based solar facilities remain available on a continuous basis. Thus NSO developed
Long‐Range Plans with the flexibility to transition from current facility operations to the period
when new facilities are in place without seriously impacting the US solar user community.
Through advancements in instrumentation and the implementation of adaptive optics at its
focal planes, NSO has maintained its telescopes at the cutting edge of solar physics. They play a
key role in the support of US and international solar research and research‐based training.
NSO telescopes remain extremely productive and are among the most accessed solar telescopes
in the world. Facility usage is given in Appendix B. We note that 25 US and 4 international
groups used the Dunn Solar Telescope (DST) in FY 2013 and 22 US and 2 international groups
used the McMath‐Pierce Solar Telescope (McMP). This indicates a strong ongoing interest in
high‐resolution and infrared solar observing. Although the major NSO telescopes are four or
more decades old, their advanced instrumentation enables the DST and McMP to continue as
key ground‐based facilities in support of US and international solar research. The NSO
telescope upgrade and instrument development program is guided by the scientific and
technical imperatives of the new ATST. Therefore, telescope and instrument upgrades and
operations are reviewed and supported on the basis that they serve as necessary preludes to the
ATST initiative, while concurrently serving the goals of the scientific community. Table 4
provides a list of the instruments available at NSO operated facilities.
Both as a necessary prelude to the ATST and as indispensable facilities for current research in
solar physics, NSO planned for the operation of the Dunn Solar Telescope and the McMath‐
Pierce Solar Telescope until the ATST is commissioned. NSF/AST, however, has stated that the
McMath‐Pierce Telescope should enter a minimal operations phase by the end of 2013 and the
DST should be divested in 2017, two years before the ATST is scheduled for commissioning.
Neither closure is optimal for maintaining and continuing to build a strong user community for
ATST.
These early closures make it imperative that we find organizational entities interested in
continuing the operation of these facilities, and we have started searching for such in earnest.
A workshop on Sac Peak/DST divestiture was held on 25 October 2012 and a similar workshop
for the McMP was held in February 2013. Divestiture of Sac Peak is crucial, since closing it and
restoring the site to natural forest would be very expensive (tens of millions of dollars), and
depending on how it is divested, there may be opportunity for joint calibration operations with
ATST. Until the ATST is online, the solar community relies on the DST for high‐resolution
spectropolarimetry and the McMP for high‐resolution spectro‐polarimetry and imaging
infrared observations beyond two microns. With closure of the McMath‐Pierce by 2017, the
latter capability will be lost for two years before ATST is on line. A gap of only two years
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17 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
between divestiture of the DST and the commissioning of ATST is perhaps less serious for the
community, but still will impact high‐resolution users. While time may be available on the Big
Bear Solar Telescope (BBSO) New Solar Telescope (NST) and the European telescopes, those
will be “pay‐for‐use,” which most US solar users will be unable to afford.
The following sections describe status and plans for NSO facilities for FY 2014 and beyond.
4.1 Dunn Solar Telescope
The 76‐cm Richard B. Dunn Solar Telescope, located on Sacramento Peak, is a diffraction‐
limited solar telescope with strong user demand and excellent scientific output. The DST has
two identical AO systems—well matched to seeing conditions—that feed two different
instrument ports. These ports accommodate a variety of diffraction‐limited, facility‐class
instrumentation, including the Diffraction‐Limited Spectro‐Polarimeter (DLSP), the Spectro‐
Polarimeter for Infrared and Optical Regions (SPINOR), the Interferometric BIdimensional
Spectrometer (IBIS), the Facility Infrared Spectrograph (FIRS), the Rapid Oscillations of the
Solar Atmosphere (ROSA). This has made the DST the most powerful facility available in terms
of post‐focus instrumentation. In addition to supporting the solar community and the science discussed in Section 2, the DST
supports observations that will drive ATST high‐resolution requirements at visible and near‐
infrared wavelengths, and refine ATST science goals. The DST also supports the development
of future technologies such as multi‐conjugate AO (MCAO), and experimental wavefront
sensing on off‐limb targets in H‐alpha. The first successful on‐sky MCAO experiment was
performed in 2009 at the DST and further efforts are ongoing. The DST supports the US and international high‐resolution and polarimetry communities and is
often used in collaboration with space missions to develop global pictures of magnetic field
evolution. While competing European telescopes have emerged, they have not supplanted the
need for the DST. Many Europeans still compete for time on the DST and provide instruments,
such as IBIS (Italy) and ROSA (Northern Ireland, UK), that are available to all users. The DST
will continue to play the major role in supporting US high‐resolution spectropolarimetry and
the development of instruments needed for progress in this important field. Most DST
instruments will have higher resolution analogues in the ATST instrument suite.
The NSO instrumentation program is focused on the development of enabling technologies that
will be central to the ATST and a strong program of understanding solar magnetic variability.
The primary areas of instrumental initiatives at NSO are high‐resolution vector polarimetry in
the visible and near‐IR. In many ways instruments developed for the DST can be considered
prototypes for ATST first‐light instruments. For example, FIRS (Facility Infrared Spectro‐
polarimeter) and the new fiber‐optic spectrograph SPIES (Spectro‐Polarimetric Imager for the
Eneregetic Sun) implement and verify state‐of‐the‐art technologies that will be used for the DL‐
NIRSP (Diffraction‐Limited Near‐Infrared Spectropolarimeter) of ATST. SPINOR is a precursor
to ATST’s ViSP (Visible Spectropolarimeter) and ROSA implements and tests concepts that
drive the design of the ATST VBI (Visible Broadband Imager) and camera systems. IBIS, a
partner instrument provided to the DST by Italy is operated by NSO with support from the
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18 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Italian community. This collaboration does not only provide experience with the design,
operations, data handling and processing of such a complex instrument but also teaches
valuable lessons on making international partnerships work successfully and with mutual
benefit. IBIS can be regarded as a prototype for the Visible Tunable Filter (VTF), which will be
provided to ATST by an international partner as well. Instrument development and scientific
applications in these areas rely on the unique capabilities of the DST and its science, technical
and operations staff and strong collaborations with university and international partners. ATST operational concepts are tested at the DST with the DST Service Mode Operations (SMO).
Service mode is an operational mode in which the PI of the observing request does not travel to
the telescope. Instead, observations are ranked, scheduled and performed by a team of telescope
scientists at the DST. This mode of scheduling is more efficient, allows a flexible schedule that
maximizes adaptation to solar target availability and atmospheric conditions, and wastes less
time waiting for opportunities and changing instrumentation. It is expected that the ATST will
be run in Service Mode for a significant fraction of its operational time. Lessons that need to be
learned include how to rank proposals, how to plan and react to target availability, and how to
disseminate the acquired data. Two SMO experiments have been conducted for one month
each in January/February and October 2013. Both experiments saw high interest from the
community, with 21 and 19 observing requests, respectively.
4.1.1 Adaptive Optics
Adaptive optics is essential for the new generation of ground‐based solar telescopes because the
science is driven by the quest for the highest spatial resolution observations. AO and MCAO are
essential technologies for obtaining the full benefit from existing telescopes and are critical to
the operation of the ATST. The NSO is continuing AO and MCAO development in primary partnership with the New
Jersey Institute of Technology (NJIT) and the Kiepenheuer Institute (KIS) in Freiburg, Germany.
A 357‐ actuator system (compared to the 97 actuators for the current system) for the 1.6‐m Big
Bear Solar Observatory New Solar Telescope has been developed jointly between NSO and NJIT
personnel and is now operational (funded by NSF‐AST‐ATI 0905279). In addition to providing
the highest resolution imagery to date (Figure 4.1‐1), this effort is also serving as a prototype for
scaling up the current 100‐actuator systems operated at the DST to a system that meets ATST
requirements (a 1900‐actuator system). The lab facility at Sacramento Peak (NSO/SP) has been
retrofitted with a clean‐room tent and a solar light feed to enable system integration and testing
of the sensitive and costly optical components needed for both the BBSO and ATST AO
systems. Essential laboratory space and test equipment can be provided to the ATST project at
NSO/SP in a very cost effective manner. The ATST high‐order AO (HOAO) system development is progressing on schedule. Major
components and subsystems are in production, or have been received, and have undergone
testing and requirements verification in the lab or at the DST. These include the wavefront
sensor camera, the field programmable gate array (FPGA) processor system prototype, the
tip/tilt mirror, the deformable mirror (in production), and various opto‐mechanical
components.
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19 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Figure 4.1‐1. A sunspot image taken at the BBSO NST with
the 357‐actuator AO system.
In addition to the ATST HOAO system
development, the development of MCAO is
progressing. The Sun is an ideal object for
the development of MCAO because solar
structure provides the “multiple guide stars”
needed to determine the wavefront
information in different parts of the field of
view. The NSO system was one of the first
successful on‐sky MCAO experiments (the
Kiepenheuer MCAO system being the other).
The NSO’s main goal, however, is to develop
MCAO technology for future implemen‐
tation at the ATST. Close collaborations
between NSO, NJIT and the Kiepenheuer
Institute exist. Dirk Schmidt, an NSO/ATST
postdoctoral fellow, is working at NSO, at
the BBSO NST and at the GREGOR telescope
on Tenerife on the implementation of MCAO systems. As of November 2013, final integration
and testing of MCAO is progressing at both the 1.5‐m GREGOR and the 1.6‐m NST and first
on‐sky results are expected very soon. The NSTʹs MCAO is strongly based on the concepts of
the MCAO system of the German GREGOR telescope which are the results of the pioneering
and continuous solar MCAO research at NSO and KIS. The MCAO work at BBSO is funded by
an NSF Major Research Instrumentation (MRI) grant (NSF‐MRI 0959187). The fruitful
collaboration between NSO, a university (NJIT) and an international partner (KIS), in addition
to providing MCAO at current large‐aperture solar telescopes, results in development of crucial
technology and prototyping for the ATST MCAO system that NSO expects to implement at the
ATST during the first few years of operations. Following the strong desire expressed by the community to have an AO system available that
can work on off‐limb structure, such as prominences and filaments, the NSO has begun a small
development effort at the DST. Making adaptive optics function using the faint prominence
structure that can be observed only with narrow‐band (0.5 Å) filters (e.g., H‐alpha) is a
challenge. A prototype system has recently been tested successfully at the DST. The project is
led by a New Mexico State University (NMSU) graduate student, who is supervised by Dr. T.
Rimmele. The ongoing AO efforts are educating and training the personnel needed to support these
efforts in the future. 4.1.2 DST Instrumentation
4.1.2.1 Diffraction‐Limited Spectro‐Polarimeter (DLSP)
The Diffraction‐Limited Spectro‐Polarimeter is fully integrated with one of the high‐order AO
systems (Port 2). In addition, a 1 Å K‐line imaging device and a high‐speed 2K 2K G‐band imager with speckle reconstruction capability as well as a slit‐jaw imager have been integrated
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20 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
with the DLSP. A diffraction‐limited resolution mode (0.09 arcsec/pixel, 60 arcsec FOV) and a
medium‐resolution mode (0.25 arcsec/pixel, 180 arcsec FOV) are available. The Universal
Birefringent Filter (UBF) can be combined with the DLSP/imaging system. This full‐up
instrumentation set is available for users. The DLSP has been used to implement a “solar queue observing mode” at the DST. Predefined
observations, or observations of targets of opportunity, are carried out by the observing support
staff. Implementation of this mode allows for more efficient use of the best seeing conditions.
A similar operating model is envisioned for the ATST, and the DST/DLSP experience will be
crucial for developing an efficient operations strategy for the ATST.
4.1.2.2 Facility Infrared Spectropolarimeter (FIRS)
This is a collaborative project between the National Solar Observatory and the University of
Hawai‘i Institute for Astronomy (IfA) to provide a facility‐class instrument for infrared
spectropolarimetry at the Dunn Solar Telescope. H. Lin (IfA) is the principal investigator of this
NSF/MRI‐funded project. This instrument takes advantage of the diffraction‐limited resolution
provided by the AO system for a large fraction of the observing time at infrared wavelengths.
Many of the solar magnetic phenomena occur at spatial scales close to or beyond the diffraction‐
limited resolution of the telescope. Diffraction‐limited achromatic reflecting Littrow spectro‐
graph allows for the required diverse wavelength coverage. A unique feature of FIRS is the
multiple‐slit design, which allows high‐cadence, large FOV scans (up to four times more
efficient than SPINOR and DLSP), a vital feature for studying dynamic solar phenomena such
as flares. The high‐order Echelle grating allows for simultaneous multi‐wavelength
observations sensing different layers of the solar atmosphere, and thus enabling 3‐D vector
polarimetry. The two detectors are a 1K × 1K MgCdTe IR camera and a 2K × 2K camera with
Kodak CCD for the visible arm, both synced to their own liquid crystal modulator. FIRS has
been fully commissioned as a supported user instrument since 2009. FIRS also serves as a
prototype for the Diffraction‐Limited Near‐IR Spectro Polarimeter (DL‐NIRSP), a major ATST
first‐light instrument.
4.1.2.3 Spectro‐Polarimeter for Infrared and Optical Regions (SPINOR)
SPINOR is a joint HAO/NSO instrument that replaced the advanced Stokes polarimeter (ASP)
at the Dunn Solar Telescope with a much more capable system. The ASP has been the premier
solar research spectropolarimeter for the last decade. SPINOR extends the wavelength of the
former ASP from 450 nm to 1600 nm with new cameras and polarization optics, provides
improved signal‐to‐noise and field‐of‐view, and replaces obsolete computer equipment.
Software control of SPINOR into the DST camera control and data handling systems has been
completed and the instrument is fully commissioned as a user instrument.
SPINOR and IBIS, are the primary instruments for joint observations with Hinode, SDO, and
IRIS. They augment capabilities for research at the DST and extend the lifetime of state‐of‐the‐
art research spectropolarimetry at the DST for another decade. SPINOR is also the forerunner
of the Visible Spectro‐Polarimeter (ViSP) that is being developed by HAO for the ATST.
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21 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
4.1.2.4 Interferometric BIdimensional Spectrometer (IBIS)
IBIS is an imaging spectrometer built by the solar group of the University of Florence in Arcetri,
Italy. IBIS delivers high spectral resolution (25 mA in the visible, and 45 mA in the infrared),
high throughput, and consequently high cadence. In collaboration with NSO and the High
Altitude Observatory, the Arcetri group has upgraded IBIS to a vector polarimeter. The
wavelength range of IBIS extends from the visible to near‐IR and allows spectroscopy and
polarimetry of photospheric and chromospheric layers of the atmosphere. NSO has a
Memorandum of Understanding with the University of Florence for continued operation and
support of IBIS at the DST. Two new identical Andor 1K × 1K cameras have replaced the
slower Princeton narrow‐band and Dalsa wide‐band cameras for improved data rates. IBIS has
been integrated into the DST SAN. IBIS and ROSA (described below) also serve as prototypes
for the Visible Tunable Filter (VTF) and Visible Broadband Imager (VBI) on ATST and are
providing experience in reducing the large data sets ATST will provide.
4.1.2.5 Rapid Oscillations of the Solar Atmosphere (ROSA)
ROSA is a fast camera system developed and built by Queens University (QU) in Belfast,
Northern Ireland. It consists of up to 7 1K 1K Andor cameras, including one especially blue‐
sensitive camera, and a computer system capable of registering up to 30 frames per second. The
computer system has an internal storage capacity of 20 Tb, enough for a few days of
observations, even at the extremely high data rates the system is capable of. Typically, the
cameras are fed through some of NSOʹs wide band filters in the blue, while the red light is fed
to IBIS. The DST observers have been instructed on operating ROSA and are capable of running
the instrument without assistance from QU.
4.1.3 Replacements and Upgrades
Critical Hardware
Given the finite time frame for DST operations, replacement and upgrades of hardware and
software are limited to the necessary minimum. The Critical hardware upgrade (CHU) is aimed
at reducing unscheduled downtime by replacing obsolete and unreliable hardware, such as the
vintage 1970s CAMAC, with modern hardware. Critical hardware is defined as follows:
hardware elements that fail repeatedly, and/or, hardware elements that cannot be repaired or
replaced without significant downtime or re‐engineering. Significant downtime (total) is
defined as more than two weeks per year. These upgrades will be limited to supporting
existing capabilities rather than offering enhanced capabilities.
Storage Area Network (SAN)
The high data volumes produced by existing and new instrumentation such as IBIS, SPINOR,
FIRS, and ROSA, an instrument to measure Rapid Oscillations in the Solar Atmosphere, require
an expansion in data storage and handling capabilities at the DST. The DST data handling
system is currently 4 Tb for storage of daily observations, and 20 Tb for long‐term (21 days or
more) storage. A 10 Gbs network switch allows instruments to write to the SAN at the
sustained high data rates required by high‐spatial resolution, high‐cadence spectropolarimetry.
Furthermore, the obsolete standard storage media, DLT tape, which was used to transfer data to
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22 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
users, has been completely replaced by removable hard drive with the eSATA transfer protocol
for much higher throughput.
4.1.4 Current and Future Use of the DST
NSO users and staff will continue to vigorously pursue the opportunities presented by high‐
resolution, diffraction‐limited imaging at the DST, with a goal of testing models of magneto‐
convection and solar magnetism, while refining ATST science objectives and ensuring the
growth of expertise needed to fully exploit ATST capabilities. The advent of high‐order AO has
increased the demand for DST time and has given ground‐based solar astronomy the
excitement shared by space missions. Currently, part of DST scheduling is devoted to testing the main envisioned ATST operation
mode (often referred to as Service Mode), where PIs no longer visit the telescope, but rather
submit proposals that are then put in a queue that is executed by NSO staff, based on scientific
ranking, prevailing observing conditions, and solar conditions. These experiments will provide
important information on the adjustments the new observing mode requires of the proposal
submission process, the evaluation of proposals, scheduling, and change in staff roles,
compared to the PI driven and fixed scheduling that now is standard at the DST.
4.1.5 Divestiture Planning
When ATST is complete, the high‐resolution capabilities of the DST will be surpassed and NSO
will cease operations and either close the DST or, preferably, find a group or groups interested
in exploiting the unique capabilities of the DST for their own use. Because NSO plans to ramp down its operation of the DST over several years, we will seek (a)
group(s) willing to ramp up their presence in Sunspot over the same time frame. In order to
work out a divestment plan, a series of workshops will be held, bringing together interested
parties. The first workshop was held on 25 October 2012 with six groups present. Interest was
expressed in assuming operation of Sunspot as an education and training center by two of the
groups (Southern Rockies Education Centers (SREC) and CU‐Boulder). More recently, NMSU
has become interested in joinig the efforts to turn the DST into a training facility for the younger
generations of astronomers and engineers. The next step is to work out potential business plans
and to coordinate with NSF on legal issues.
4.2 McMath‐Pierce Solar Telescope
The McMath‐Pierce solar facility is a set of three all‐reflecting telescopes, with the main
telescope having a primary diameter of 1.6 m, and the two auxiliary telescopes (East and West)
with diameters of about 0.8 m. The McMP provides large‐aperture all‐reflecting systems that
can observe across nearly two orders of magnitude, from 350 to 23000 nm; the telescopes are
very configurable with light beams that can feed a number of large, laboratory‐style optics
stations for easy and flexible instrument setup. The McMP is unique since it is the only 1.6 m
aperture solar telescope fully available to any scientist, the only solar telescope with
instrumentation that routinely observes in the infrared beyond 2500 nm, and the only solar
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23 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
facility in the world with instrumentation to observe the Sun at 12000 nm and beyond. Recent
joint observations in 2011 with the BBSO/NST illustrate the unique ability of the McMP to collect
longer time series observations (factor of 2 or longer) with a much wider field‐of‐view (covering
five times the area or more) than can be obtained by the NST. Consistent with the NSF budget
assumptions and the recommendations of the Portfolio Review, NSO has begun the process of
identifying potential community user groups that could take over the operation of the McMP. If
a suitable alternative is not identified, NSO will begin the process of shutting down operations.
4.2.1 Diverse Observing Capabilities
As recognized by the decadal report (NWNH, p. 34) solar physics research draws support from
diverse sources and the research recently conducted at the McMP uniquely encapsulates this
scientific diversity. Among this work are several infrared studies of the Sun, which range from
the long‐term (13 years of data) sunspot magnetic field strength observations to the studies of the
solar atmospheric dynamics of the cold chromosphere that span just several hours of
observations. Unique spectral observations of sodium emission from Mercury and the Lunar
CRater Observation and Sensing Satellite (LCROSS) impact event as well as the ultra‐high
spectral resolution infrared measurements of the atmospheric temperature on Venus illustrate the
planetary astronomy applications of the McMP and its instruments. Measurements of terrestrial
HCl molecules have verified the effectiveness of the Montreal protocol. Finally the laboratory
determination of new spectroscopic parameters of the 13C14N molecule will enable better analysis
of cometary and cool star spectra, and point to the important contribution to fundamental
physics by the instrumentation at the McMP facility.
4.2.2 Divestment or Closure of the McMP
The NSF/AST requires NSO to ramp down NSO support for the McMP to minimum operations
by the end of 2013 with divestment to follow as soon as practically possible. In order to get from
the current level of 2 FTEs to the envisioned shutdown with minimal interruption of
observations, operations at the McMP have been streamlined by block scheduling to minimize
set‐up time and by modifying the pointing and guiding system in order to provide more
automation for observing programs.
Discontinuing NSO operations can be accomplished by divesting the McMP to other groups or
by mothballing or removing the facility. There are no agreements that we are aware of that
require removal of the facility. This would be a matter of negotiation between NSF and the
Tohono O’odom Nation. The cost of long‐term mothballing of the facility will be estimated.
NSO has recently awarded a contract to assess the environmental impact of the divestiture of our
facilities at Kitt Peak.
The best, and least costly, path is to find a group or groups willing to assume responsibility for
the McMP. To this end, NSO conducted a workshop in early 2013 to identify parties interested in
taking over the telescope facility and to discuss the costs and logistics of the transition. Currently,
the NSO has a few (e.g., NASA‐funded) users that contribute to the cost of operating their
experiments at the McMP. To smooth the transition and give other groups time to obtain
funding, NSO proposes allowing users that can provide funding and their own support to
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24 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
continue using the facilities with a ramp‐down plan of NSO support through FY 2017.
Thereafter, it is expected that a consortium of users would assume full responsibility for the
operation of the McMP on Kitt Peak as a tenant observatory. This removes the McMP from the
NSO “books” and NSF funding, while providing interested parties more time to raise full
operational funding. We have a similar arrangement with the Evans Solar Facility at Sac Peak.
A number of issues will arise in negotiating with potentially new operating institutions. Some of
the costs of maintaining the McMP are contained in the Kitt Peak National Observatory (KPNO)
budget. These include a number of KPNO partial FTEs that provide maintenance and the McMP
footprint costs for overall mountain operations. NOAO’s long‐term plan for continuing mountain
operations is also a factor that any new operating institution must consider. In particular, the
NSF expects that the NOAO will not be operating telescopes on Kitt Peak (with the possible
exception of the Mayall 4‐meter) by the end of FY 2015. The NSO is in the process of negotiating
a ramp‐down of NOAO support of NSO Kitt Peak facilities contained in the shared resources
portion of the KPNO budget.
4.2.3 Impacts of Early Closure of the McMP
The McMP has been a model of Scientific Diversity. In addition to solar observations, it is used
for atmospheric and laboratory spectroscopy, planetary studies and observations of exoplanets
and stellar activity cycles. The NSO is currently involved with estimating the cost of a complete
removal of the McMP from Kitt Peak and is communicating with university partners who have
expressed an interest in operating the facility after NSO removes support. Unfortunately, an early
closure may preclude some of these groups from obtaining funds, or make it more difficult and
costly to operate if the McMP is forced to sit idle for an extended period.
As part of the ramp‐down, the FTS instrument was moved out of the McMP facility in early FY
2012 to the campus of a university. This resulted in the loss of NSOʹs ability to support ultra‐high
resolution spectroscopy for the laboratory, atmospheric and solar communities.
The research activities at the McMP have several unique applications to the future ATST facility.
Infrared spectropolarimetry tests of optics at 4667 nm have been performed at the McMP with
direct application to the ATST CryoNIRSP (cryogenic near‐IR spectropolarmeter) instruments.
Recent images at the McMP at 4667 nm have produced important design constraints for second‐
generation ATST IR imaging instruments. The low‐order adaptive optics system at the McMP
recently had its first solar application at 4667 nm wavelength, verifying that daytime wavefront
corrections made in the visible improved image quality on measurements across a wavelength
range of nearly a factor of ten. These capabilities are lost with closure of the facility.
4.2.4 Collaboration with the New Solar Telescope Cyra Development
The McMath‐Pierce is currently the only solar telescope that is equipped to observe the Sun at
wavelengths longer than 2.5 microns. During the development of the NJIT/BBSO New Solar
Telescope Cryogenic Infrared Spectrograph (Cyra), the McMP is playing an important role in the
testing of optical elements and the design of the Cyra observations.
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25 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
In early 2012, narrow‐band filters for isolating solar spectral lines from 3600‐4200 nm were
ordered for Cyra, and these were installed in the NSO Array Camera (NAC) at the McMP and
tested. In 2013, a polarimeter system consisting of a rotating quarter‐wave retarder and linear
polarizers was obtained by the Cyra program and tested at the McMP using the NAC. While the
McMP main spectrograph is at room temperature, resulting in a large background at these
wavelengths, the NAC was able to make the first spectropolarimetric maps of a sunspot at 4135
nm during observations in Fall 2013.
Observing programs to be run on the Cyra instrument are currently being tested on the McMP
using the NAC. While the Cyra observations will benefit from a greatly reduced thermal
background, exploratory observations at the McMP with the warm spectrograph will have
important scientific results. Several strange molecular transitions with negative effective Landé
g‐factors have already been observed, the curious linear polarization signals seen in an
unidentified atomic spectral line at 4136 nm have been recorded, and observations of the
polarimetric signals at CO 4666 nm were achieved. Initial observations of the infrared
chromospheric lines in this region are planned for 2014. The 3 – 4 micron region observed with
the NAC and the McMP have revealed spectral diagnostics arising from the photosphere,
chromosphere and corona with magnetic sensitivies that are five to ten times greater than
corresponding features in the visible. Thus, the McMP is demonstrating the tremendous
potential of the mid‐IR for solar magnetic field measure‐ments at the highest sensitivities.
With the exploratory NAC observations come experiments designed to enhance the signal to
noise of the observation procedure, and important tests of background subtraction and gain
correction techniques at this wavelength. These all will be applied to the Cyra observation
procedure at the NST, and should result in observations of the magnetic fields in the quiet Sun
with unprecedented magnetic sensitivity.
4.2.5 Current Programs
Synoptic observations from W. C. Livingston (NSO) using the McMath‐Pierce have revealed a
secular decrease in the mean sunspot magnetic field strength during solar cycles 23 and 24. If
this decline continues, it has enormous implications: a weak cycle 24 is one outcome, and an even
weaker, or non‐existent cycle 25 might also occur. No analogous observations have been made at
any other facility, and this data‐set alone shows the enormous value of the McMath‐Pierce and its
infrared capability. Extension to this data‐set using imaging spectropolarimetry at 1565 nm with
the new NAC system is currently underway. We have started an intercalibration program
between McMath‐Pierce and DST‐FIRS instrument to further understand these secular changes.
Much of the infrared spectrum is still barely explored, especially in flares, sunspots, and the
corona. The McMath‐Pierce Telescope and the NAC have begun to address these questions with
new observations of a powerful X1.8 flare and the magnetic structure of the sunspot
superpenumbra using the infrared He I line at 1083 nm, and new observations of the CO lines at
2330 nm and at 4667 nm. Full‐disk scans of the Mn I line at 1526 nm, which show sensitivity to
low magnetic fields with hyperfine structure, have been made for the first time at the McMath‐
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26 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Pierce. Further studies will be used to develop techniques and science questions that will
continue to refine the ATST IR capabilities.
As part of the ATST project, observations of telescopic scattered light are being made at the
McMP. After the ATST selected Haleakalā as the site for the ATST, it became clear that the
coronal observation of the ATST would be limited by telescopic rather than atmospheric
scattered light. The state‐of‐the‐art laboratory experiments in telescopic scattered light from dust
do not probe the small angle regime nor the wavelength regime where ATST coronal
observations are proposed. Direct measurements of these angles and wavelengths are possible
using the McMP telescope. Preliminary observations at 1565 nm are different from the model fits
using 10‐micron laboratory data, which have been used to predict ATST dust scatter. Further
observations in the 1‐12 micron wavelength region, particularly at 1075 and 3934 nm where the
ATST will measure solar coronal emission lines, will be done at the McMP, and the results will be
used to further refine the predicted ATST scattered light values as well as the cleaning program
for the ATST primary mirror.
4.3 NSO Integrated Synoptic Program
NISP (the NSO Integrated Synoptic Program) was formed in July 2011, and combines the Global
Oscillation Network Group (GONG) and the Solar Long‐Term Investigations of the Sun (SOLIS)
programs. These two programs have similar scientific goals and share a number of technical
approaches, so the combination of the two has resulted in improved system efficiency and
increased scientific synergy.
When ATST is completed, the combination of the ATST and the NISP will provide a complete
view of solar phenomena on a range of spatial scales from tens of kilometers to the full disk, and
on time scales from milliseconds to decades. In particular, NISP is a long‐term and consistent
source of synoptic solar that observes the Sun as a whole globe over solar‐cycle time scales.
While space missions, such as SOHO and SDO, also observe the entire solar disk, they cannot
match the long‐term coverage provided by NISP, which started in 1974 with the advent of the
Kitt Peak magnetograph, Sac Peak flare patrol, and spectroheliograms. In addition, space
missions are vulnerable to the effects of solar flares and CMEs, cannot be repaired, and are
extremely expensive. These qualities make NISP invaluable as a source of data for national space
weather needs. The recent National Academy report on Solar and Space Physics: A Science for a
Technological Society strongly supported synoptic solar physics as an essential component of the
science needed for space weather.
4.3.1 NISP Instrumentation
The NISP/GONG component is an international, community‐based program that studies the
internal structure and dynamics of the Sun by means of helioseismology—the measurement of
resonating acoustic waves that penetrate throughout the solar interior—using a six‐station,
world‐circling network to provide nearly continuous observations of the Sun’s five‐minute
oscillations. The instruments obtain 1K × 1K 2.5‐arcsec pixel velocity, intensity, and magnetic
flux images in the photospheric Ni I 676.7 nm line of the Sun every minute, with an
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27 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
approximately 90% duty cycle, enabling continuous measurement of local and global
helioseismic probes from just below the visible surface to nearly the center of the Sun. Near‐real‐
time continuous data, such as 10‐minute cadence, high‐sensitivity magnetograms, seismic images
of the far side of the Sun, and 20‐second cadence 2K × 2K H‐alpha intensity images are also
available. These real‐time data are used by the US Air Force Weather Agency (AFWA), and
NOAA’s Space Weather Prediction Center (SWPC) for space weather forecasts. AFWA provides
NSO with funding towards GONG operations.
NISP/SOLIS has three main instruments: a vector spectromagnetograph (VSM) capable of
observing full‐disk vector and line‐of‐sight magnetograms in the photosphere and chromosphere,
a full‐disk patrol (FDP) imager, and an integrated sunlight spectrometer (ISS) for observing the
high‐resolution spectra of the Sun as a star. The VSM produces 2K × 2K longitudinal and vector
magnetograms constructed from full Stokes polarization spectra at a resolution of 200,000 in the
Fe I 630.15/630.25 nm line pair, and longitudinal magnetograms in the Ca II 854.2 nm line core
and wings. This allows the VSM to provide simultaneous photospheric and chromospheric
magnetic field measurements, a powerful combination for understanding the structure of
magnetic fields in stellar atmospheres. The VSM also produces chromospheric intensity
(equivalent width) images in He I 1083.0 nm, which are used for identification of coronal holes.
The FDP can take observations with a temporal cadence as short as 10 seconds in several spectral
lines including Hα, Ca II K, He I 1083.0 nm, continuum (white light), and photospheric lines. The
ISS observations are taken in nine spectral bands centered at the CN band 388.4 nm, Ca II H
(396.8 nm), Ca II K (393.4 nm), C I 538.0 nm, Mn I 539.4 nm, Hα 656.3 nm, Ca II 854.2 nm, He II
1083.0 nm, and Na I 589.6 nm (D line) with a resolution of 300,000. The ISS can observe any other
spectral lines within its operating range.
Hardware for the guider in the VSM was installed in early June 2013, completing the SOLIS hardware
project. The software for the VSM guider is under development and will be completed by the end of
calendar year 2013. The VSM will operate as usual during this period.
With the move to Boulder and the divestment of the McMP, NSO will seek a superior site to locate
SOLIS. Under consideration are Big Bear Solar Observatory in California, Haleakalā on Maui, and
Mauna Loa on Hawai’i (or Big Island). The final choice will balance cost and performance.
4.3.2 NISP Data Products
The NISP provides a large number of data products to the community. In addition to the
products mentioned above, data processing pipelines produce global helioseismic frequencies,
localized subsurface velocity fields derived from helioseismic inversions, synoptic maps of the
solar magnetic field, potential field source surface extrapolations of the magnetic field in the
corona, vector magnetic field maps of active regions produced from inversions of the Stokes
profiles, and the total global magnetic flux. These data products are important for understanding
the Sun and its activity cycle and related space weather. They also can be used for understanding
the impact of stellar activity on habitable planets. In addition, the experience of NISP in
pipelining a large number of data products, and in performing inversions, can be applied to the
development of the ATST data processing and analysis system.
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28 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
NISP scientists use insights from their own research to monitor and improve the quality of NISP
data and to develop new data products. Most recent examples include error estimates for
synoptic magnetic maps, synoptic maps of vector fields, and sunspot field strengths derived from
separation of Zeeman components of spectral line profiles. Within the next few years, NISP is
expected to provide vector magnetic field observations in the chromosphere using the Ca II 854.2
nm line. This will provide a much fuller picture of the structure of the magnetic field in the
middle solar atmosphere, where the field direction changes from primarily vertical to horizontal
as it forms the magnetic canopy. This transition takes place in the solar atmosphere near the
location where the solar wind is accelerated. These future chromospheric vector magnetic field
observations would be extremely important not only for understanding the origins of space
weather for planets in our solar system, but also for testing the theories of the generation of
stellar winds and their consequences for the habitability of planets around other stars. A
combination of the ISS and VSM data would allow us to deconvolve the solar‐disk average
characteristics of the Sun in terms of activity across the disk. The latter would bring a new
understanding of stellar disk‐integrated parameters. It is also expected that progress will be
made on a new synoptic network with instrumentation capable of providing both vector
magnetic field and Doppler data in multiple wavelengths by 2020.
Research into the use of local helioseismology to detect active regions before they emerge is
continuing. In addition, helioseismic measurements of subsurface vorticity as a forecast of flare
activity are being developed. Both of these approaches hold out considerable promise of success,
but also have proven to be challenging. Global helioseismology has been tracking the evolution
of large‐scale flows, including the north‐south meridional flow and the zonal flow known as the
torsional oscillation. These flows are intimately connected with the dynamo mechanism that
produces the solar magnetic field and associated activity. For example, the timing of the
migration of the zonal flow has proven to be a good indicator of the future behavior of sunspot
activity. Current observations suggest that the next activity cycle, number 25, may be even
weaker than the current cycle.
4.3.3 NISP Status
4.3.3.1 NISP/GONG Component
The NISP/GONG component continues to operate nominally with the usual maintenance issues
concerning the turret and power supplies. A fire occurred at the Udaipur site in August 2010,
which delayed the deployment of the final H‐alpha instrument there. The data acquisition
system (DAS) is being upgraded and replaced with a PC‐based system similar to that used in the
SOLIS component; this is an example of the improved efficiency that NISP provides. In addition,
GONG has now stopped returning data on tapes, and is now obtaining data in near‐real time
from five of the six sites (Learmonth will be done by the end of CY 2013). This development will
save funds on tape supplies and maintenance, but at the added expense of Internet access fees.
The removal of the tapes has reduced the latency between data acquisition and reduction of the
helioseismology products. A long standing maintenance issue has been the degrading entrance
windows on the turrets. An alternative to the problematic 100 layer coating was recently
designed and the new entrance windows will be installed in FY14.
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29 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
4.3.3.1.1 NISP/GONG Operations Support
NISP has been receiving substantial support from the US Air Force Weather Agency since 2009, when
AFWA provided $650K to develop and install H‐alpha filters in the GONG shelters. AFWA
subsequently provided $800K of operational funds for two years, but has been forced to cut that
support by 50% in 2013 due to the Federal Sequestration Act. The immediate consequences of this cut
to NISP were the loss of three FTE technical support positions and the need to drastically lower site
operational costs at Big Bear and Mauna Loa. It is expected, however, that our relationship with
AFWA is good for the long term since In addition AFWA has informally stated that they expect
GONG to replace their aging Solar Optical Observing Network (SOON) on a long‐term basis. AFWA
however, would like to have long‐term commitment for NISP support from the NSF.
NISP is also providing data to the Space Weather Prediction Center in Boulder. SWPC is funded
by NOAA and uses GONG and SOLIS data as input to drive a predictive model of terrestrial geo‐
magnetic storms. Discussions have indicated that SWPC recognizes the value of the data and the
need for support, but a firm commitment is on hold until the SWPC director position is filled.
We note that NOAA SWPC declared GONG data essential during the recent Government
shutdown episode. While it is unlikely that SWPC will be able to directly supply funds, NOAA
should be able to supply the resources as an in‐kind contribution, such as assigning NOAA staff
to NSO or operating the Mauna Loa GONG site. Similarly, NISP data are used to drive models
hosted by NASA’s Community Coordinated Modeling Center (CCMC), and all of the NASA
solar space missions use NISP data for context and supporting observations. A proposal to
NASA’s recent opportunity for Heliophysics Infrastructure and Data Environment Enhance‐
ments has been submitted (July 2013).
Using helioseismology, NISP produces estimates of the magnetic field on the farside of the Sun
that is turned away from the Earth. The estimates provide a signal that new active regions have
emerged that will appear on the Earth‐facing side up to two weeks in advance. Research at the
US Air Force Research Laboratory (AFRL) has shown that the assimilation of farside data into the
construction of synoptic magnetic field maps greatly improves the quality of the maps as it
reduces the errors at the edge of the map that would otherwise contain older data from 28 days
earlier. In September 2012, the AFRL data assimilation system, known as ADAPT, was installed
at NSO/Tucson and will be used by NOAA/SWPC to drive the geomagnetic storm prediction
system discussed above.
4.3.4.2 NISP/SOLIS Component
The NISP/SOLIS component is nearing full operational status. The last instrument, the Full‐Disk
Patrol (FDP), was installed at Kitt Peak in July 2011. The data from the FDP are available on the
Web, but needs additional flat‐field development. The cameras in the VSM were installed in
December 2009, and have been performing well. The guider hardware for the VSM has been
installed, and is expected to be fully operational in early 2014. The temporary H‐alpha filter will
be replaced with the tunable filter that is currently under construction. This will allow NSO to
declare the SOLIS hardware phase as finished by mid FY14. The data processing system for
SOLIS is being revamped. The data are no longer being processed on Kitt Peak, but instead are
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30 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
now transferred down to Tucson and reduced in the NISP Data Center. This removes what has
been the most problematical SOLIS system, and exploits the pipeline expertise developed in the
GONG program. This is another example of the improved NISP efficiency.
4.3.4.3 NISP Data Center
There have been several developments in the NISP Data Center. Substantial progress has been
made in creating a standardized synoptic map pipeline to process both SOLIS and GONG data.
A multi‐wavelength, multi‐resolution synoptic map pipeline is now in place. The SOLIS
processing now occurs in Tucson (instead of Kitt Peak), in a centralized NISP infrastructure
isolated from SOLIS legacy hardware dependencies. The entire Level‐1 VSM code has been
revamped and rewritten. Significant improvements to 85421 and 6302v processing algorithms
have been made. A new, very fast vector inversion code based on the Instituto de Astrofísica de
Canarias (IAC) system that is also being used for the HMI instrument on SDO has been
implemented. The utilization of near‐real‐time NISP data products by space weather forecasters is increasing.
The hourly GONG magnetic field synoptic maps are now routinely used by NOAA/SWPC to
drive their forecasts of the solar wind and geomagnetic storms. The H‐alpha images from GONG
are used by the US AFWA for flare monitoring. AFWA also uses the high‐cadence GONG
magnetograms, and the AFRL receives a special ten‐minute GONG magnetic field data product
tailored for ingest by their ADAPT data assimilation system to predict the surface solar magnetic
field. Both NOAA and the AFRL use the maps of the far‐side magnetic field produced from
GONG helioseismic data.
4.3.4 NISP 2014 Goals
NISP goals in FY 2014 will be dominated by the transition to Boulder. For NISP/GONG
operations, the main issue will be the relocation of the two GONG engineering instruments to
Boulder. Since the network sites themselves are geographically independent of Tucson, their
operation and the resulting supply of space weather data should not be interrupted. Note that
the data reduction for the AFWA H‐alpha images is already located in the Cloud, and a prime
Data Center task is to transition the NOAA/SWPC magnetic field processing into the Cloud as
well. For NISP/SOLIS, the challenge will be to relocate the instrument suite with as little
downtime as possible. We are developing plans for temporarily relocating SOLIS to Tucson to
expedite upgrades and develop a modularized, automated observing system. A major decision
will be made as to the permanent location for NISP/SOLIS at either Big Bear, Tenerife, Haleakalā,
or Mauna Loa. The time frame for permanent relocation is expected in 2015. For the NISP Data
Center, the near‐term goals are to move all mission‐critical pipelines in support of space weather
to Cloud‐based computing platforms, continue to streamline and automate legacy GONG and
SOLIS reduction pipelines, develop the NSO Data Center plan for Boulder, and create a space‐
weather data oriented Website to cater to the growing user‐base of those products.
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31 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
4.4 Evans Solar Facility
The Evans Solar Facility provides a 40‐cm coronagraph as well as a 30‐cm coelostat. The Evans
Facility is the most thoroughly instrumented coronograph in the world. The Air Force group
(AFRL) at Sacramento Peak provides support for and is the primary user of the ESF 40‐cm
coronagraph. SOLIS and ISOON have replaced the spectroheliogram capability of the ESF with
full‐disk imaging. The AFRL also provides funding for a part‐time observer and a postdoctoral
fellow to support operations and data processing, as well as funds for minimal maintenance. The
High Altitude Observatory has installed an instrument for the ESF for measuring prominence
magnetic fields.
4.5 Access to NSO Data
4.5.1 Digital Library
In addition to its dedicated telescopes, the NSO operates a Digital Library that provides synoptic
datasets (daily solar images from SOLIS, GONG data, and a portion of the Sacramento Peak
spectroheliograms) over the Internet to the research community. Current NSO Digital Library
archives include the Kitt Peak Vacuum Telescope (KPVT) magnetograms and spectroheliograms;
the Fourier Transform Spectrometer transformed spectra, the Sacramento Peak Evans Solar
Facility spectroheliograms and coronal scans, and solar activity indices. In addition, NISP
archives comprise GONG and SOLIS instrument datasets. GONG data include full‐disk
magnetograms, Doppler velocity and intensity observations, local and global helioseismology
products, and near‐real‐time H‐alpha, far‐side, and magnetic‐field products.
The near‐real‐time products are automatically disseminated to various agencies, including
AFWA, AFRL, and NOAA/SWPC for space weather prediction applications. The SOLIS data
archive includes the VSM, ISS and FDP. In 2012, about 14 TB of combined NISP and Digital
Library data were exported to over 1,200 users. Additional data sets from ISOON, the DLSP, and
the remainder of the NSO/SP spectroheliograms (being digitized at NJIT) will be included in the
future. We will also be hosting some non‐NSO data sets such as the Mt. Wilson Ca K synoptic
maps and the AFRL Air Force Data Assimilative Photospheric flux Transport (ADAPT) magnetic
field forecasts. The Digital Libray will also host the data sets form the DTS Service Mode
observing runs.
Since the inception of the Digital Library in May 1998, more than 54 million science data files
have been distributed to about 149,000 unique computers. These figures exclude any NSO or
NOAO staff members. The holdings of the NSO Digital Library are currently stored on a set of
disk arrays and are searchable via a Web‐based interface to a relational database. The current
storage system currently has 125 TB of on‐line storage. The Digital Library is an important
component of the Virtual Solar Observatory (VSO).
4.5.2 Virtual Solar Observatory
In order to further leverage the substantial national investment in solar physics, NSO is
participating in the development of the Virtual Solar Observatory. The VSO comprises a
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32 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
collaborative distributed solar‐data archive and analysis system with access through the WWW.
The system has been accessed approximately a million times since Version 1.0 was released in
December 2004. The current version provides access to more than 80 major solar instruments and
200 data sets along with a shopping cart mechanism for users to store and retrieve their search
results. The interface has now expanded and in addition to the graphical user interface (GUI),
there is an interactive data language (IDL) and a Web service description language (WSDL)
interface (e.g., Python programmers). These two new interfaces currently make the bulk of the
volume in the VSO.
The overarching scientific goal of the VSO is to facilitate correlative solar physics studies using
disparate and distributed data sets. Necessary related objectives are to improve the state of data
archiving in the solar physics community; to develop systems, both technical and managerial; to
adaptively include existing data sets, thereby providing a simple and easy path for the addition
of new sets; and eventually to provide analysis tools to facilitate data mining and content‐based
data searches. None of this is possible without community support and participation. Thus, the
solar physics community is actively involved in the planning and management of the Virtual
Solar Observatory. None of the VSO funding comes from NSO; it is fully supported by NASA.
For further information, see http://vso.nso.edu/. Recently, the major effort in the VSO has been
the construction of remote mirror nodes for the data set produced by NASA’s SDO mission. This
effort is now complete, with one of these nodes is now located at NSO. SDO downloads via the
VSO are currently close to a 1TB/day, where the NSO provider is an important download node.
With the completion of the SDO mirror nodes, VSO is resuming the development of spatial
searches. Currently, almost all of the data accessible through the VSO is in the form of full‐disk
solar images. A spatial search capability will allow the user to locate data in a specific area on the
Sun delineated by heliographic coordinates. The returned data could be either observations of a
restricted area on the Sun, or full‐disk data covering the required Carrington longitudes. The
spatial search capability requires information on the location of the observational instruments,
since current NASA missions such as STEREO are not located near the Earth. In addition to the
spatial search capability, the VSO will soon provide access to another 6‐12 data sets that have
requested to be included.
In the time frame covered by NSO’s 2012‐2016 Long Range Plan, NSO will continue to be a
central component of the VSO.
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33 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Table 4. Telescope and Instrument Combinations FY 2014 Key: DST = Dunn Solar Telescope ESF = Evans Solar Facility GONG = Global Oscillation Network Group HT = Hilltop Telescope KPST = Kitt Peak SOLIS Tower McMP = McMath-Pierce Solar Telescope McMPE = McMath-Pierce East Auxiliary Telescope Instrument Telescope Comments/Description
NSO/Sacramento Peak – OPTICAL IMAGING & SPECTROSCOPY
High-Order Adaptive Optics DST 60 - 70-mode correction (two systems, Port 2 and Port 4)
Interferometric Bidimensional Spectrometer (IBIS) DST Spectroscopy/Polarimetry, 25-45 mÅ resolution, 550 nm-860 nm Diffraction-Limited Spectro-Polarimeter (DLSP) DST 6302 Å polarimetry, 0.09 arcsec and 0.25 arcsec/pixel
Universal Birefringent Filter (UBF) DST Tunable narrow-band filter, R < 40,000, 4200 - 7000 Å
Horizontal Spectrograph (HSG) DST R < 500,000, 300 nm - 1.0 m
Universal Spectrograph ESF Broad-spectrum, low-order spectrograph, flare studies
Littrow Spectrograph ESF R < 1,000,000, 300 nm - 2.5 m
Spectro-Polarimeter for Infrared & Optical Regions (SPINOR) DST HSG based Spectro-Polarimeter, 450-1700 nm
Rapid Oscillations in the Solar Atmosphere (ROSA) DST Imaging system, 350-660 nm
40-cm Coronagraph ESF 300 nm – 2.5 m
Prominence Magnetometer ESF Spectro-Polarimetry, 587.6, 656.3, 1083.0 nm
Coronal Photometer ESF Coronal lines: 5303 Å, 5694 Å, 6374 Å 6374 Å
NSO/Sacramento Peak –O/IR IMAGING & SPECTROSCOPY
Horizontal Spectrograph (HSG) DST High-resolution 1- 2.5 m spectroscopy/polarimetry, R < 300,000 Facility Infrared Spectropolarimeter (FIRS) DST Spectro-Polarimetry; 630.2, 1083.0, 1564.8 nm
Littrow Spectrograph ESF Corona and disk, 1 - 2.5 m spectroscopy/polarimetry
NSO/Kitt Peak – O/IR IMAGING & SPECTROSCOPY
SOLIS Vector Spectromagnetograph (VSM)
KPST
1083 nm: Stokes I, 2000 1.1 arcsec, 0.35-sec cadence 630.2 nm: I, Q, U, V, 2000 1.1 arcsec, 0.7-sec cadence 630.2 nm: I & V, 2000 1.1 arcsec, 0.35-sec cadence 854.2 nm: I & V, 2000 1.1 arcsec, 1.2-sec cadence
SOLIS Integrated Sunlight Spectrometer (ISS) KPST 380 – 1083 nm, R= 30,000 or 300,000
SOLIS Full-Disk Patrol (FDP) KPST High temporal cadence filterograms at 656.28 and 1083 nm
Vertical Spectrograph McMP 0.29 - 12 m, R < 106
NSO Array Camera (NAC) McMP 1 - 5 m, 1024 1024, direct imaging, and full Stokes polarimetry from 1- 2.2 m
CCD Cameras McMP 380 - 1083 nm, up to 2048 2048 pixels, high-speed IR Adaptive Optics McMP 2 – 12 m
Planetary Adaptive Optics McMP 0.4 - 0.7 m, planetary or stellar sources down to ~3rd magnitude at the stellar spectrograph
Stellar Spectrograph McMP 380 – 1083 nm, R < 105
Image Stabilizer McMP Solar, planetary or stellar use to 7th magnitude for use with the vertical or stellar spectrograph Integral Field Unit (IFU) McMP 6.25" 8" field, 0.25" per slice, producing a 200" long-slit. Optimized for 0.9 -5.0 µm on the vertical spectrograph
Wide-Field Imager McMPE Astrometry/Photometry, 6 arcmin field
NSO/GONG – GLOBAL, SIX-SITE, HELIOSEISMOLOGY NETWORKHelioseismometer & Magnetograph
H Intensity Images
California, Hawai῾i, Aus-tralia, India, Spain, Chile
2.8-cm aperture; imaging Fourier tachometer of 676.8 nm Ni I line; 2.5 arcsec pixels; 1-min. cadence.
Full Disk, 1 arcsec pixels; 20-sec. cadence
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5 INITIATIVES: THE ATST AND THE NEW SYNOPTIC NETWORK
The introduction of novel, post‐focus instrumentation and adaptive optics has greatly enhanced
the capabilities of the solar telescopes of NSO, thereby enabling whole new areas of scientific
inquiry, especially in high‐resolution and infrared observations of the Sun. These new results,
combined with improved modeling, have shown that advances in spatial, temporal, and spectral
resolution are required to accurately measure fine‐scale, rapidly changing solar phenomena and
to test the advances in our theoretical understanding. Increasing the number of photons collected
over the short evolutionary times of solar features is needed for making accurate polarimetric
observations. Meeting these challenges requires a new, large‐aperture solar telescope.
5.1 Advanced Technology Solar Telescope (ATST)
The 4m Advanced Technology Solar Telescope will be the most powerful solar telescope and the
world’s leading ground‐based resource for studying solar magnetism that controls the solar
wind, flares, coronal mass ejections, and variability in the Sun’s output. The strong scientific case
for the ATST was made in two previous decadal surveys (Astronomy and Astrophysics in the New
Millennium (2001) and The Sun to the Earth—and Beyond (2003)). The recent NSF sponsored
Community Workshop on the Future of Ground‐based Solar Physics (2011) reemphasized the “game
changing” science ATST will enable. The detailed science drivers for ATST are discussed in
numerous publications including the science requirements document (http://atst.nso.edu/library). The science drivers lead to a versatile ATST design that supports diffraction‐limited imaging,
spectroscopy and, in particular, magnetometry at visible and near‐ and far‐infrared wavelengths,
and infrared coronal observations near the limb of the Sun.
A primary scientific objective of the ATST is to precisely measure the three‐dimensional structure
of the magnetic field that drives the variability and activity of the solar atmosphere. The energy
released in solar flares and coronal mass ejections was previously stored in the magnetic field.
The magnetic field is structured on very small spatial scales and understanding the underlying
physics requires resolving the magnetic features at their fundamental scales of a few tens of
kilometers in the solar atmosphere. The large 4‐m aperture of the ATST, which represents a
transformational improvement over existing solar telescopes, opens up a new parameter space
and is an absolutely essential feature to resolve structures at 0.”025 (20 km on the Sun) at visible
wavelengths.
New technologies developed at existing NSO facilities, such as the high‐order adaptive optics
(HOAO) system, are incorporated into the ATST design to deliver a corrected beam to the initial
set of state‐of‐the‐art, facility‐class instrumentation located in the coudé lab facility. At near‐
infrared wavelengths, the HOAO will enable space quality observations of high Strehl for a vast
majority of the available clear time. Magnetically sensitive spectral lines in the infrared will be
used to reveal and study in detail the elusive internetwork magnetic fields that cover the entire
solar disk. The impact and significance of these fields are not yet understood. These fields may
contain more than 80‐90% of the solar magnetic energy that would interact with the solar
dynamo and heating of the upper solar atmosphere and irradiance variations. The ATST will
provide high‐precision polarimetric measurements of these fields, sometimes referred to as
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hidden or dark magnetic energy, by using combined visible and infrared diagnostics enabled by
the powerful and sophisticated ATST first‐generation instrumentation. The 4‐m aperture will for
the first time provide sufficient spatial resolution at near‐infrared wavelengths (60 km at 1.6
micron), where spectral lines are found that can provide the critical sensitive diagnostics needed
to precisely measure the properties of the weak internetwork fields. The science requirement for
polarimetric sensitivity (10‐5 relative to intensity) and accuracy (5 x 10‐4 relative to intensity) place
strong constraints on the polarization analysis and calibration units, making ATST a high‐
precision magnetometer.
A large photon collecting area is an equally strong driver toward large aperture as is angular
resolution. Observations of the chromosphere and, even more so, the faint corona are inherently
photon starved. The solar atmosphere is structured on small spatial scales and is highly
dynamic. Small structures evolve quickly, limiting to just a few seconds the time during which
the large number of photons required to achieve measurements of high sensitivity can be
collected. Measurements of the weak coronal magnetic fields are essential to understand the
physics of, for example, coronal mass ejections, and aid space weather prediction efforts.
Measurements of the coronal magnetic field are desperately needed to make progress but are also
extremely difficult. The coronal intensity is only 10‐5 to 10‐6 of the disk intensity. The polarimetric
signal ATST aims to detect is only 10‐3 to 10‐5 that of the coronal intensity. This means that
contrast ratios are of the order of 10‐8 to 10‐11 and, thus, are not too different from what planet
detection efforts are facing. The large collecting area and low scattered light properties of the
ATST are essential to achieve the chromospheric and coronal science requirements. The magnetic
sensitivity of the infrared lines used to measure coronal fields and the dark sky conditions in the
infrared are important motivations to utilize the ATST for exploring the infrared coronal
spectrum. The off‐axis design was motivated by the coronal science requirements as well as by
technical considerations.
A main driver for a large‐aperture solar telescope is the need to detect and spatially resolve the
fundamental astrophysical processes at their intrinsic scales throughout the solar atmosphere.
Modern numerical simulations have suggested that crucial physical processes occur on spatial
scales of tens of kilometers. Observed spectral and, in particular, Stokes profiles of small
magnetic structures are severely distorted by telescope diffraction, making the interpretation of
low‐resolution vector magnetograms of small‐scale magnetic structures difficult to impossible.
Resolving these scales is of utmost importance to be able to develop and test physical models and
thus understand how the physics of the small‐scale magnetic fields drives the fundamental global
phenomena. An example is the question of what causes the variations of the solar radiative
output, which impacts the terrestrial climate. The Sunʹs luminosity increases with solar activity.
Since the smallest magnetic elements contribute most to this flux excess, it is of particular
importance to study and understand the physical properties of these dynamic structures.
Unfortunately, even the most advanced and newest current solar telescopes, such as the 1.6‐m
New Solar Telescope (NST) or the 1.5‐m GREGOR, cannot resolve such scales because of their
limited aperture size (Figure 5.1‐1).
The European Association for Solar Telescopes (EAST) has recently and independently
developed science requirements for the European Solar Telescope (EST) to be located on the
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36 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Figure 5.1‐1. Complex line profiles from a quiet Sun MHD simulation. The panel shows a
simulation of convection (far left) and the resulting Stokes V profiles along the line shown on the
simulation (column labeled Sim). The other columns show the effect of observing the profiles with
various apertures (the 4m ATST, the 1m Swedish Solar Tower, and the 0.5m Hinode Solar Optical
Telescope.
Canary Islands. It is interesting to note that the EST requirement for aperture size is also 4m,
indicating that this is an aperture size that optimally enables addressing the science drivers.
Science operations, including data handling and dissemination, will be much more efficient
compared to the operations of current NSO or similar facilities. ATST operational concepts have
been developed and will be refined during the construction phase. These concepts build on the
lessons learned from recent spacecraft operations such as TRACE, Hinode and SDO. Efficient
operational modes such as Service Observations will make more efficient use of the available
observing time. The NSO Data Center at NSO Headquarters in Boulder will provide science‐
ready ATST data products to the solar physics community. An open data policy allows for
maximum science productivity.
5.1.1 ATST Science Working Group and Science Requirements
The Co‐Investigator institutions of the ATST project are the University of Hawaiʻi (Dr. J. Kuhn), the University of Chicago (Dr. R. Rosner), New Jersey Institute of Technology (Dr. P. Goode) and
the High Altitude Observatory (Dr. M. Knoelker). Monthly Co‐I meetings ensure that the Co‐
Investigators are kept apprised of project progress and that scientific and programmatic concerns
of the university and broader user community are considered. Several of the Co‐Investigator
institutions are actively involved in teaching a graduate education in solar physics course that
was initiated by the University of Colorado (Dr. M. Rast). The Kiepenheuer Institute in Freiburg,
Germany is contributing one of the first‐light instruments, the Visible Tunable Filter (VTF).
Additional collaborations are being pursued with the UK (science detector development) and
Spain (polarimetric analysis).
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The ATST Science Working Group (SWG) provides scientific oversight and advice concerning all
aspects of the project, including operations planning. The SWG works closely with the Project
Scientist in establishing and tracking science requirements for the telescope and its instruments.
The SWG actively participated in developing the ATST Science Requirements Document (SRD),
the formal specification document from which all designs flow. The SWG has guided and
reviews the Operations Concept Document (OCD), which lays out efficient operational modes for
the facility. The SWG is leading the definition of the Critical Science Plan (CSP). The CSP
includes high priority science observations that the community desires to accomplish during the
first 18 months of operations. These CSP observations will be performed in service mode.
Observations proposed by principal investigators and facilitated by the regular proposal
submission process will also be performed during this early operations phase. All data produced
will be made available to the community though the NSO Data Center at NSO Headquarters in
Boulder. In addition, an important goal for the early operations phase is to optimize instrument
and overall system performance and to refine and optimize service‐mode operational procedures.
The split between service‐mode and PI‐mode operations will also be established during this
phase based on input and feedback from the community and considering budgetary constraints.
The SWG has broad participation from the US and international community and includes
members from the fields of stellar and planetary physics, heliospheric physics, geophysics, the
space weather community, space sciences and other interdisciplinary fields. The group includes
members from the university community, national labs, NASA, Air Force, and international
partners, and demonstrates the strong collaborative spirit of the international solar community as
well as being an indicator for the broad societal impacts of solar astronomy.
The SWG meets at least once a year and issues formal findings and recommendations. In 2013, a
two‐day meeting was held just after the AAS/SPD meeting in July in Bozeman, Montana. The
meeting covered issues ranging from the instrument design review progression to operations and
Data Center design progress.
Since the ATST project design phase is ramping down and construction is underway, the SWG
will undergo a shift in focus and in composition for 2014. The SWG focus will shift to the
definition of the critical science plan (the science programs to be undertaken in the first year of
commissioning and operations) and supporting operations and Data Center design. The
composition of the SWG for 2014, including new members, is shown in Table 5.1‐1.
To support the ramp up of operations software and Data Center designs, the SWG will form two
sub‐working groups. The Operations sub‐working group will be chaired by Dr. Craig DeForest
(SWRI) and will consist of 4‐5 SWG members familiar with complex facility operations. The Data
Center sub‐working group will be chaired by Dr. Neal Hurlburt (Lockheed Martin Solar and
Astrophysics Laboratory) and will consist of SWG members versed in data center design and
operations.
The critical science plan (CSP) of the ATST will comprise approximately 20‐30 key science topics
that will be developed and supported by teams of community scientists, one of whom will be
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38 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
resident on the ATST SWG at any given time between now and first‐light operations. The topics
will be grouped into major themes such as “magnetoconvection”, “atmospheric heating and
dynamics”, “eruptive phenomena”, and “spectral surveys”. The CSP will be a living document
published in the ArXiv facility so that the entire solar physics community can track its progress
and offer to contribute in its development if they so choose. Topcis in each theme will be defined
by the Spring of 2014 with preliminary writing assignments completed by SWG members by the
next annual meeting in November of 2014.
Table 5.1-1. ATST Science Working Group
Nazaret Bello-Gonzales* Kiepenheuer Institute, Germany Wenda Cao New Jersey Institute of Technology Gianna Cauzzi Arcetri Observatory, Italy Steve Cranmer* Harvard Smithsonian Astrophysical Observatory Craig DeForest Southwest Research Institute Yuanyong Deng National Astronomical Observatory, China Lyndsay Fletcher University of Glasgow, United Kingdom Neal Hurlburt Lockheed Martin, Solar & Astrophysics Laboratory Philip G. Judge High Altitude Observatory Yukio Katsukawa* National Astronomical Observatory of Japan Piet Martens* Montana State University Scott McIntosh High Altitude Observatory Clare Parnell University of St. Andrews, Scotland Jiong Qiu Montana State University Mark Rast (Ch.) University of Colorado Luis Bellot Rubio Instituto de Astrofisica de Andalucia, Spain Eamon Scullion* Queen's University, Belfast Hector Socas-Navarro Instituto de Astrofisica, Spain Stein Vidar Haugen* University of Oslo, Norway
*New member (2014)
5.1.2 ATST Project Engineering and Design Progress
The ATST is an all‐reflecting, 4‐m, off‐axis Gregorian telescope housed in a co‐rotating dome.
The ATST delivers a maximum 300‐arcsec‐diameter circular field of view. Energy outside of this
field is rejected from the system by a heat stop located at prime focus, allowing manageable
thermal loading on the optical elements that follow. The telescope also includes a sophisticated
wavefront control system, including active optics (aO) for figure control of the primary, active
alignment of the critical optical elements, such as primary and secondary mirrors, and an
integrated high‐order adaptive optics system designed to provide diffraction‐limited images to
the focal‐plane instruments at the coudé observing stations. The basic telescope parameters and design for the ATST and its subsystems have been described
in detail in a number of recent publications to which we refer the reader for design details and
perfor‐mance analysis (see http://atst.nso.edu/library/pubs). Additional information can be found
on the ATST Web site, http://atst.nso.edu. The most important capabilities of the ATST are
summarized in Table 5.1‐2.
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Table 5.1-2. ATST Capabilities Telescope Property Specification or Reason for Property
Aperture 4 meters Diffraction-Limited Resolution λ = 430 nm 0.022 arcsec λ = 1 µ 0.05 arcsec λ = 4 µ 0.2 arcsec λ = 12 µ 0.60 arcsec Gregorian Off-Axis Unobstructed Aperture No Spider Diffraction Clean Point-Spread Function High Strehl Alt-Az Mount High-Order Conventional Adaptive Optics MCAO-Ready Optical Design Internal Seeing Control Thermal Control of Optics and Structure Dust Control for Low Scattered Light Coronal Observations Polarimetric Sensitivity >10-5 Polarimetric Accuracy 5 x 10-4 Wavelength Coverage 300 nm to 28 micron Facility-Class, First-Light Instruments
5.1.2.1 Construction Phase Status and Milestones
The project followed the Project Execution Plan established and reviewed at the NSF‐conducted
Final Design Review. Commencement of site construction on Haleakalā, however, was tied to
the “all permits in place” milestone. After the Record of Decision (ROD) was signed by the NSF
Director, the project submitted an application for a Conservation District Use Permit (CDUP), as
required by Hawaiian statute. The Hawaiʻi Board of Land and Natural Resources (BLNR) voted
and approved the CDUP on December 2, 2010. A contested case was immediately filed. The
contested challenge was re‐solved in November 2012, followed by a judgment in the project’s
favor with regard to the existing legal challenges. Full access to the site was granted on
November 29, 2012 and a ceremonial groundbreaking occurred on November 30, 2012.
Construction began on December 1, 2012.
Construction contracts for the major sub‐systems of the telescope and instrumentation systems
(e.g., M1 blank and polishing, enclosure, telescope mount assembly (TMA), M1 assembly, instru‐
ments, support facilities final design), have been issued and are proceeding according to a revised
baseline schedule (see Section 5.1.3). Major subsystems milestones are shown in Table 5.1‐3.
5.1.2.2 Current Design Activities
The current ATST design is shown in Figure 5.1‐2. The design includes the coudé instrument
area and feed arrangement. Preliminary instrument design efforts and other activities have
continued with the Co‐PI teams and partners. The following efforts are underway:
High Altitude Observatory (Visible Spectro‐Polarimeter).
University of Hawaiʻi (Diffraction‐Limited Near‐IR Spectro‐Polari‐meter Design; Cryo IR
Spectro‐Polarimeter.
NSO/ATST (Red‐ and Blue‐Visible Broadband Imager).
Kiepenheuer Institut für Sonnen‐physik (Visible Tunable Filter).
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40 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Table 5.1-3. ATST Major Systems Milestones
Support Facilities 2014-Jun 2014-Jun 2016-May 2016-Jun 2017-May
Support & operations (S&O) building foundations complete. Lower telescope pier complete. Support & operations building Beneficial Occupancy Date. Coating and cleaning facilities available on site. System interconnects for S&O/mount installed; IT infrastructure complete.
Optical Systems 2015-Sep 2015-Dec 2015-Apr 2015-Jun 2015-Jun 2015-Nov 2016-May
Primary mirror (M1) polishing complete. Delivery of M1 to site. M1 cell assembly acceptance testing complete. Delivery of M1 cell assembly to site. Top end optical assembly (TEOA) acceptance testing complete. Delivery of TEOA to site. Delivery of feed/transfer optics to site. Telescope Mount Assembly
(TMA) 2014-Oct 2015-Apr 2016-Apr 2017-Feb 2017-Aug
TMA fabrication complete. TMA available for site assembly. Coudé structure installation complete. TMA coudé acceptance testing complete. TMA mount installation complete.
Enclosure 2014-Sep 2014-Oct 2016-May
Enclosure ready for site assembly and testing. Enclosure AZ track installation, assembly and testing complete. Enclosure site fabrication, assembly and testing complete. Facility Thermal Systems
(FTS) 2015-May 2016-Apr 2017-Apr 2017-May 2017-Aug
Facility plant equipment inspection & acceptance on site. Facility control system site assembly begins. Facility management systems fabrication, site assembly & testing complete. Facility control system site assembly and testing complete. F ilit th l b t f b i ti bl d t ti l t Wavefront Correction (WFC) 2014-Apr
2015-Sep 2016-Nov 2017-Jun 2017-Dec 2018-Oct
High-order AO real-time hardware delivered. Deformable mirror (DM) acceptance testing complete. Context viewer control assembly, integration & testing complete. Low-order wavefront system assembly, integration and testing complete. WFC lab installation begins. WFC coudé installation complete.
Software 2014-Jul 2016-Feb 2016-Mar 2016-Jun 2016-Jul 2017-Nov
Data Storage System testing complete. Observatory Control System site acceptance testing complete. Data Handling System & data processing pipeline testing. Instrument Control System software delivered. Camera Software delivered. Global Interlock System installation and testing complete.
5.1.2.3 Schedule and Milestone Summary
For the schedule development, the engineer responsible for each Work Breakdown Structure
(WBS) element has developed detailed plans, including schedules and budgets, for the
construction phase. The project manager and the systems engineering team have integrated
these details into the overall project schedule (the Integrated Project Schedule).
The top‐level ATST construction schedule is shown in Figures 5.1‐3 and 5.1‐4. Current planning
targets calendar year 2019 for obtaining the first scientific data with an ATST instrument. At the
end of the commissioning phase each instrument will be tested for its compliance with key
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41 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
science performance specifications (e.g. spatial, spectral resolution, polarimetric sensitivity).
Training of operations staff will occur during the extended Integration, Test and Commissioning
(IT&C) phase. A short science verification period performed by the instrument partner and
operations teams will demonstrate the scientific validity of delivered data products. With the
conclusion of instrument science verification the facility will be handed over to operations.
The NSO is engaging in the planning of science operations, including telescope operations on Maui
and science operations and data‐center management at NSO headquarters at CU in Boulder.
NSO is already applying significant resources to the effort and will begin the ramp up to final
operations staffing in 2015. Table 5.1‐3 shows the staffing plan for ATST operations ramp up.
5.1.3 Funding
In FY09, funding from the American Recovery and Reinvestment Act of 2009 (ARRA) was made
available to the project at the level of $146M. Funding from the MREFC was made available to
the project at the level of $151,928,000. Figure 3.5‐1 shows the funding currently planned by NSF.
The first MREFC increment of $7M was awarded on February 12, 2010 (FY)(funds) with
subsequent award amounts of $13M on June 15, 2010, $5M in August 2011, $10M in 2012, and
$25M in 2013. These values have been significantly lower than the anticipated funding profile
(set at FDR),
Figure 5.1‐2. Current ATST facility.
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42 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Figure 5.1‐3. Top‐level construction schedule.
Figure 5.1‐4. Summary schedule illustrating key critical path construction and major (off‐site development) milestones.
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43 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Figure 5.1‐5. ATST funding by fiscal year.
principally due to the site access delays; the changes have created contracting challenges to the
project with some schedule impact. Most significantly, the overall multi‐year delay in site access
has had a profound impact on both the project schedule and the project budget. During 2012, the
project performed an internal re‐baseline of the project execution plan, considering the
unanticipated delays and unanticipated costs incurred by the project (in the permitting and
associated legal process). At the lowest granularity of the project work packages, every item was
re‐evaluated for cost (updating all basis‐of‐estimates on labor/material resources needed to
complete that area), schedule (updating the completion based on the modified integrated project
schedule, adjusting for the site access delays), and risk (updating a factored risk assessment
based on the cost, schedule and technical performance risk remaining). In October 2012, the NSF
convened an external panel‐of‐experts to review the project’s revised baseline. This process
concluded in March 2013, with the panel endorsing the project’s baseline development. The
baseline proposal was subsequently further reviewed and audited internally within the NSF and
then submitted to the National Science Board. The NSB authorized the NSF Director to approve
the revised baseline, including both the updated milestone schedule as well as a revised funding
profile and total cost of $344.1M. Figure 5.1‐5 summarizes the re‐baseline funding and spend
profiles by fiscal year.
5.2 A Multi‐Purpose Global Network
Synoptic data is vital both for the success of the ATST and for society in general. Both the aging
of GONG and the single‐site nature of SOLIS has led the solar physics research community to call
for a new improved synoptic network. While NSO has previously proposed for a network of
three VSM instruments similar to the one currently on SOLIS, it is now thought that a better
solution would comprise a new multi‐purpose network. Such a network would open new realms
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44 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
of scientific research, and provide input data that are vital for space weather operational
forecasts. Since the NSF/AST Division Portfolio Review recommends a substantial reduction in
NISP support, the funds for developing and operating a new network will need to have major
support from the space weather community, including agencies such as AFWA, NASA and
NOAA.
There are a number of new scientific research directions in solar physics that motivate the desire
for a new ground‐based network. For example, there is a growing need for multi‐wavelength
measurements to provide observations of wave propagation and the vector magnetic field as a
function of height in the solar atmosphere. For helioseismology, we now know that inclined
magnetic fields in the solar atmosphere convert the acoustic waves into various types of MHD
modes and change the apparent phase of the waves, which produces incorrect inferences of the
sub‐surface structure below active regions. For magnetic field measurements, it is essential to
know the direction and strength of the field above the photosphere for accurate coronal field
extrapolations, and to reliably remove the azimuthal ambiguity. Our understanding of the
generation, transport, and evolution of the solar magnetic fields would make significant progress
with the availability of continuous long‐term multi‐wavelength observations. Simultaneous
helioseismic and magnetic observations will also bring a better understanding of propagation of
acoustic waves in the presence of magnetic fields, thus bringing us closer to forecasting the
subphotospheric properties of magnetic fields. In addition, irradiance measurements such as
those provided by the Precision Solar Photometric Telescope (PSPT), which are important for
climate research, would be improved with additional spectral bands and more continuous
coverage.
It is important to note that existing and future space missions often propose to combine
helioseismic observations made from different vantage points to better map layers inside the Sun
such as the tachocline. While we have long benefited from continuous Earth line‐of‐sight
helioseismic observations from space that could be combined with observations made from a
different perspective, the best way to secure in the long run such observations is through a
ground‐based network similar to GONG. The ESA/NASA Solar Orbiter mission (launch 2017)
will provide helioseismic observations made from a variety of perspectives including from out of
the ecliptic. These observations will be made at particular mission orbits that are of interest for
the study of the meridional flows near the poles and will occur well into the last phases of the
mission (late next decade). Combining such data with observations made from the Earth line‐of‐
sight will bring new insights about fundamental ingredients of the dynamo problem. Similarly,
the combination of magnetic field observations from different perspectives allow disentangling
complex projection effects that occur when observing crucial locations of the Sun such as the
solar poles. SOLIS‐like synoptic vector observations and Solar Orbiter similar measurements can
be combined to clarify the distribution and strength of the magnetic fields at the solar poles. We
thus remain convinced that these opportunities will surely enhance the value of a ground‐based
synoptic network such as the one proposed here by NSO.
In addition to the research role of a network, space weather operational forecasts rest on the
foundation of synoptic solar observations. Agencies such as AFWA and NOAA/SWPC need
reliable and continuous sources of solar data, and are already using NISP facilities as a source of
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45 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
surface magnetic fields, H‐alpha intensity, and helioseismic far‐side maps. A new network that
provides multi‐wavelength observations would increase the quality of information available for
space weather and is an efficient and cost‐effective solution to a multi‐agency requirement.
There is considerable international community interest in establishing a new network, as
demonstrated by a workshop that was held in Boulder in April 2013 to discuss and gather input
on science requirements, capabilities and instrumentation. About 60 scientists and engineers
either attended the meeting or expressed interest, representing space weather agencies, solar
physics research institutes, observatories, government agencies, and international organizations.
Most of the presentations, along with the participant list, can be found at
https://www2.hao.ucar.edu/docs/2013‐synoptic‐network. An article reporting on the workshop has
been published in Space Weather (Hill, Thompson, and Roth SpWea 11, 2013). The International
Astronomical Union (IAU) has recognized the importance of synoptic observations of the Sun by
creating a special Working Group that is chaired by a scientist from NSO (A. Pevtsov).
The instrumentation in a new network should not be a single device to provide all observations,
but should comprise individual specialized instruments on a common pointing platform. This
approach has several advantages:
Fewer compromises for scientific requirements within a single instrument;
More flexibility in funding and schedules;
Ability to have different instrument suites at different sites to exploit specific
observing conditions (e.g., coronal, radio observations);
Relaxation of stringent scientific requirements for space weather forecast data;
Lower initial costs – need pointing platform, infrastructure and one instrument.
The NSO, with HAO and the Kiepenheuer Institut für Sonnenphysik in Germany, is developing a
white paper on the idea, and KIS has obtained funding through the SOLARNET program to carry
out an evaluation of instrumental concepts. A possible configuration is shown in Figure 5.2‐1.
NSO, along with partner institutions, will develop a full proposal for a new network in the next
year or two. It will likely be proposed that the NSF lead the development through its recently
announced Mid‐Scale Instrumentation Program (MSIP). Additional agency partners are likely to
be AFWA, NOAA/SWPC, and NASA. In addition, the Atmospheric and Geospace Sciences
(AGS) Division of the Geosciences Directorate in the NSF supports space weather research, which
necessarily uses solar synoptic data as inputs for models.
NSO is participating in the European SPRING (Solar Physics Research Integrated Network
Group) effort, which is currently seeking to fill a position at KIS to evaluate instrument concepts
for the network. An approximate timeline of the network effort is:
2013: Work with KIS and HAO to develop concept.
2013 – 2014: Advocacy for agency, international, and research partnerships.
2014: Submit baseline infrastructure and initial instrument proposal for the
NSF MSIP opportunity.
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46 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
2015 – 2018: Assuming success, begin development of infrastructure and first‐light
instrument hardware.
2015 – 2018: Continuing advocacy with AFWA, NOAA, NASA, NSF/AGS, etc.
2019: Initial deployment.
2020 – 2024: Operations, and additional instrumentation development.
Figure 5.2‐1. A possible instrumental configuration for a new synoptic solar observing network.
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47 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
6 EDUCATION AND PUBLIC OUTREACH AND BROADENING
PARTICIPATION With the decrease in NSO base funding in FY 2013 NSO had to reduce its Education and Public
Outreach (EPO) efforts in FY 2013. We recently lost our EPO officer because of lack of sufficient
funds to support his position. We, however, remain committed to undergraduate, graduate, and
postdoctoral training, areas in which NSO has been most effective. We will support other
outreach areas as funding and staff time permit. NSO is also committed to increasing the diversity of the solar work force. We focus our efforts on
expanding participation by underrepresented groups in our student and teacher research
programs as well as staff recruitment. To this end, we participate in the Fisk‐Vanderbilt Masters‐to‐
PhD Bridge Program, the Akamai Workforce Initiative (AWI) on Maui, two Partnerships in
Astronomy & Astrophysics Research and Education (PAARE) programs, and with New Mexico
State University graduate programs. In addition, we are working closely with the University of
Colorado, Boulder (CU) in the program they recently implemented to enhance the number and
training of solar graduate students.
6.1 Goals and Metrics
The primary NSO EPO objectives and goals in priority order are:
To help train the next generation of scientists and engineers through support for under‐graduate and graduate students, postdoctoral fellows, and close collaboration with
universities and the ATST consortium.
Continue our successful REU program.
Each REU student provides a program assessment, gives a talk on their work and
writes a final report (which can be viewed at http://eo.nso.edu/).
o Metrics –
(1) Number of excellent students persuaded toward solar research.
(2) Number of students helped toward a science/engineering/computer career.
(3) Increased diversity in the REU program.
Strengthen our Summer Research Assistantships (SRA) for graduates program.
Our involvement in the Akamai Workforce Initiative Program has increased the
number of mentors by including engineers. The metrics are the same as above.
We have made more of our indirect earnings and carryover funds available for
student and postdoctoral support.
Increase the number of thesis students and postdoctoral fellows working at NSO.
The move of the NSO directorate site to the CU campus will strengthen this area
by giving access to more top notch graduate students and by providing an
attractive locale for postdoctoral fellows. NSO continues to be involved in the
training of postdocs and graduate students. We currently have five postdoctoral
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48 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
research associates: Sanjay Gosain, Lewis Fox, Brian Harker, Fraser Watson, and
Dirk Schmidt. Watson and Schmidt joined the NSO staff in FY 2013. After
spending five years as a postdoc with the NSO adaptive optics program, Jose
Marino was promoted to Assistant Scientist in July 2013 and continues to focus on
AO and MCAO, including ATST wavefront correction. Students who have
defended their PhD thesis in 2013 with NSO advisors include Thomas Schad (U.
Arizona) with Matt Penn, and Michael Kirk (New Mexico State U.) with K.S.
Balasubramaniam (NSO/AFRL) and Irene González Hernández. Greg Taylor
(New Mexico State U.) is currently working on his thesis with Thomas Rimmele on
adaptive optics. Sarah Jaeggli received her PhD in 2011 from the University of
Hawaiʻi (Haosheng Lin, thesis advisor); she was an REU student with Matt Penn
in 2003, worked as a visiting grad student at NSO/SP with Han Uitenbroek for part
of her dissertation research which included commissioning of the Facility Infrared
Spectro‐polarimeter (FIRS) on the DST. She is now a postdoc at Montana State U.
and continues to collaborate on NSO instrumentation projects. Teresa Monsue
(Fisk‐Vanderbilt Masters‐to‐PhD Bridge Program) completed her master’s thesis
and started on her PhD this fall using GONG data; Frank Hill and Keivan Stassun
(Vanderbilt U.) are her advisors.
o Metrics –
(1) Number of students who successfully complete their PhD based on NSO data.
(2) Number of successful postdoctoral fellows pursuing careers in solar science.
(3) Increased diversity in these programs.
Continue collaboration with the Workforce Initiative Program on Maui for
workforce development.
This effort is going very well. The Akamai Workforce Initiative is a program
started by the Center for Adaptive Optics and provides students and graduates in
Hawai‘i with technical training, then places them in internships. We have
sponsored four workshops on Maui for Akamai program graduates—the most
recent in November 2012 and in November 2013. Since 2010, nine Akamai
graduates have participated in NSO programs and one was hired on the ATST
project staff (James Linden, 2011). Five of the students have worked on ATST
projects, including one Native Hawaiian. In summer 2013, there were two
Akamai students, one in Tucson (male working on digitizing solar images) and
one at Sac Peak (female working on implementing the NSO lab
spectropolarimeter). We expect to recruit up to four Akamai interns in summer
2014.
o Metrics –
(1) Akamai trained personnel available for the ATST Maui work force.
(2) Increased diversity available for NSO hires.
To develop K‐12 teacher training and student training programs to advance knowledge
of science and technology.
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49 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Strengthen our Research Experience for Teachers (RET) program.
The NSO generally has up to three RETs working with staff each summer. Pia
Denzmore, a science teacher at Debakey High School for the Health Professions,
participated in the summer 2013 program. Debakey has a student population of
over 70% under‐represented minorities. During the past few years, we have had
teachers from the Navajo and Tohono O’odham Nations participate in the RET
program.
Make RET lesson plans available on the WWW.
Metrics –
(1) Use of experience gained in the classroom by RET participants.
(2) Student awareness of science careers.
To increase public understanding of the Sun, both as a star and as the driver of conditions on the Earth, as well as understanding of the related disciplines of optical
engineering, electronics and computer sciences, as applied through the ATST and other
NSO projects.
Increase the relevance and content of our WWW outreach.
NSO Web pages were recently redone to include more outreach. The outreach
effort for the June 2012 solar eclipse and transit of Venus were highly successful.
This area needs more work, but is resource limited.
Develop outreach materials for both classroom and public distribution.
NSO is working with NOAO EPO and UH Maui College and local middle and
high school teachers to develop a program for Maui. We have asked NOAO EPO
(supported with NSO funding) to lead this effort.
Complete our Solar System Model and the handout materials that accompany it.
The New Mexico Museum of Space History in Alamogordo is working with NSO
to continue support of the model and has expressed interest in the NSO Visitor
Center after NSO has departed Sac Peak.
To increase nationally the strength and breadth of the university community pursuing
solar physics.
Work closely with our ATST university partners and other groups to recruit and
help diversify the community of scientists doing solar research.
This has started in the form of a joint program (Collaborative Graduate Education
Program) involving the University of Colorado, New Jersey Institute of
Technology, University of Hawaiʻi (CU/NJIT/UH) and NSO. The first phase is to
establish remote teaching at all three university sites, then expand once the
logistics of the program are well understood. The NSO’s role will include
scientists participation in teaching; planning and participating in summer
workshops; increased presence in the Akamai program; and collaboration with
NOAO and UH Maui College to provide training and materials to K‐12 teachers.
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50 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Establish close ties with additional universities to provide NSO thesis students.
Currently, ties include New Mexico State University (NMSU), University of
Arizona (UofA), and the University of Hawaiʻi (UH) for thesis students. We will
form an alliance with CU for both faculty and graduate students.
6.2 Recruiting a New Generation of Scientists
The future of solar physics hinges on the successful recruitment of a talented new generation of
scientists by the universities and national research organizations. NSO has programs for both
undergraduate and graduate students. The undergraduate program is supported primarily
through a Research Experiences for Undergraduates (REU) grant from NSF. This grant also
allows for a proposal to support elementary, middle and high school teachers, the Research
Experiences for Teachers (RET) program. NSO has proposed for and participated in these
programs since their inception at NSF.
We typically host several REUs each year, with almost all going on to graduate schools. Not
surprisingly, most of our REUs end up with careers in Astronomy (since it is this interest that led
them to apply), but a substantial number pursue careers in solar physics, which is often difficult
since most universities do not have a solar graduate program. NSO’s collaboration with CU and
other universities will increase the opportunities to attend graduate school in solar physics. NSO provides research and instrument development opportunities for students at both of our
sites in Sunspot, New Mexico and Tucson, Arizona. As we ramp up staffing for ATST
operations, these programs will be extended to Maui and Boulder. The NSO summer research assistantship (SRA) program provides opportunities for graduate
students and additional opportunities for undergraduates to work at NSO. This program has
been extremely effective in attracting graduate students into the field of solar physics, with over
50% of the graduates advancing to postdoctoral fellowships in solar research and over 80%
remaining in astronomy. Many of the current NSO staff and solar science staff at other
institutions have participated in NSO’s SRA program. Some of the biggest benefits to locating NSO on the CU campus are to provide NSO with access
to top quality graduate students and to increase the strength of solar research at CU and the
teaching of solar research techniques at universities. Thereʹs a commitment by the University to
the teaching of solar physics, including involvement of other universities in teaching of solar
courses through remote learning. This program started recently with CU professors giving a
course in solar physics with participation from students at the University of Hawaiʻi, New Jersey
Institute of Technology, New Mexico State University and CU. This program will be extended to
other universities in the future. The program will develop a cadre of graduate students with
interest in solar physics, and with NSO contributing to their strength in solar research and
instrumentation through studentships and by supporting summer workshops that bring together
students from the various participating universities. The exciting research opportunities ATST
will provide and the increasing need to understand space weather should provide graduates of
the program opportunities to obtain teaching and research positions at other universities.
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51 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
*Includes participants in the 10‐week IRES and Akamai programs.
Through NISP, NSO has sponsored students participating in the International Research
Experience for (Graduate) Students (IRES) program. This program is funded by the NSF Office of
International Science and Engineering (OISE) and is open to US graduate students in any
discipline of astronomy or astrophysics who are US citizens or permanent residents, age 21 years
or older, and have a passport. The main goal of the program is to expose potential researchers to
an international setting at an early stage in their career. The program takes place in Bangalore,
India, under the auspices of the Indian Institute of Astrophysics (IIA), a premier national center
devoted to research in astronomy, astrophysics and related physics.
6.3 Increasing Diversity
To recruit more underrepresented minority students, we have expanded our recruitment efforts
to include colleges from the Historically Black College List generated by the NSF and a list of
American Indian Science and Engineering Society affiliates. NSO also has partnered with two
universities that participate in the Partnerships in Astronomy & Astrophysics Research and
Education program. As described by the NSF synopsis, “the objective of PAARE is to enhance
diversity in astronomy and astrophysics research and education by stimulating the development
of formal, long‐term, collaborative research and education partnerships between minority‐
serving colleges and universities and the NSF Astronomical Sciences Division (AST)‐supported
facilities, projects or faculty members at research institutions including private observatories.” The NSO has been successful with the inclusion of women in its REU program as more than half
of the research undergraduates in recent years have been female (see Table 7.3‐1 for the gender
and underrepresented minority breakdown of REU statistics for 2006–2013).
Table 7.3-1. NSO REU Participant Statistics (2006-2013) Year 2013 2012 2011 2010 2009 2008 2007 2006 % Participants
Male 3 2 2 2 3 4 2 1 38.8
Female 2 4 4 5 3 2 4 6 61.2
Minority* 0 0 0 2 0 1 0 0 6.1
*Includes only students from underrepresented minorities (Hispanic and African‐American).
Table 7.2-1. Number of Participants in NSO Educational Outreach Programs (2005–2013) Year Graduate (SRA) Undergrad (SRA) Undergrad (REU) Teachers (RET) Postdoctoral Fellows
2013 8* 1* 5 1 5 2012 8* 2 6 2 6 2011 8* 2* 6 3 6 2010 6* 7 5 2009 6* 6 2 6 2008 7* 1 6 0 6 2007 9* 6 4 7 2006 4 7 4 5 2005 9 8 4 5
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52 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
In accordance with the AURA action plan to respond constructively to the NSF goal of
broadening the participation of underrepresented groups, the NSO has appointed a Diversity
Advocate (DA) and adopted a set of near‐term and long‐term goals in this vital area. AURA has
established a Work‐force and Diversity Committee (WDC) that includes each AURA Center’s
Diversity Advocate as a permanent member. The AURA Web site provides an overview of the
meaning of “broadening participation” and its action plan (http://www.aura‐
astronomy.org/diversity.asp?diversity=actionplan). The NSO goals are guided by input received
from our oversight committees that also take into account our resource constraints in effectively
addressing this area of national concern. Despite limited resources, the NSO has and will
continue to make important contributions to broadening participation in the STEM workforce.
Our near‐term and long‐term goals are as follows:
6.3.1 Near‐Term Goals:
Expand recruitment efforts of underrepresented groups through broader advertising
venues for NSO job opportunities.
Participate in STEM‐related society meetings, either national or regional, serving under‐
represented communities such as the National Society of Black Physicists (NSBP),
National Society of Hispanic Physicists (NSHP), Society for the Advancement of
Chicanos an Native Americans in Science (SACNAS) and American Indian Science and
Engineering Society (AISES).
Add a scientific staff member from an underrepresented group to the NSO Scientific
Personnel Committee.
Continue PAARE student participation in NSO programs as funded by the Fisk‐
Vanderbilt and NMSU PAARE proposals, as well as graduate student participation in
the NSO through the Fisk‐Vanderbilt Masters‐to‐PhD Bridge program. Respond to
interest expressed by additional institutions to propose for a PAARE program with the
NSO. Expand this beyond the scientific staff to include our engineering and technical
staff as mentors.
Identify more mentors among the engineering and technical staff, in addition to the
scientific staff.
Expand recruitment of Akamai Program graduates.
6.3.2 Long(er)‐Term Goals:
Increase the number of underrepresented students in the NSO REU program, ideally,
with a supplement to our REU funding.
Expand the NSO RET program effort by targeting teachers at underrepresented
minority‐serving institutions, including obtaining funding for more RET internships.
Increase the number of underrepresented minorities on the scientific and/or engineering
and technical staff.
Obtain student‐internship funding for engineering and computing at the NSO.
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53 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
We are pleased with the progress already being made in these areas. NSO continues to work
towards a more diverse staff. Given our small numbers and low turnover, opportunities arise
only occasionally. When they do arise, we have expanded our recruitment platforms to
encourage more applications for underrepresented groups.
Mark Giampapa, the first NSO Diversity Advocate, has passed that responsibility to John
Leibacher, who currently is also vice chair of the AURA Workforce Diversity
Committee. The NSO DA represents the Observatory on the AURA WDC and at
underrepresented minority conferences and job fairs.
NSO has added a female tenure‐track scientist, Serena Criscuoli, to its staff.
Walter Allen, male African‐American, was hired in a postdoctoral fellow position. After
completing his postdoctoral fellowship, he went on to teaching at Pima Community
College in Tucson and is now at Mesa Community College.
Matthew Richardson, male African‐American, participated in the joint Fisk‐Vanderbuilt‐
NSO Masters‐to‐PhD Bridge Program and did his masterʹs thesis with Frank Hill and
Keivan Stassun (Vanderbilt U.) using GONG data. Matthew is now in the PhD
program.
Teresa Monsue, an African‐American female, is participating in the joint Fisk/Vanderbilt‐
NSO Masters‐to‐PhD Bridge Program; she recently completed her masterʹs thesis and is
now working on her PhD with co‐advisors Frank Hill and Keivan Stassun.
NSO is a partner on the Fisk University five‐year AST/PAARE proposal, ʺGraduate
Opportunities at Fisk in Astronomy and Astrophysics Research (GO‐FAAR)ʺ submitted
in August 2013.
Alexandra Tritschler was hired to a scientist‐track position to begin developing the ATST
operations model. Previously, she was hired as an NSO postdoctoral fellow.
Crystal Hart, an African‐American female, joined the NSO observing staff at the DST.
Crystal has a background in engineering from San Diego State University.
Participation in the Akamai Workforce Initiative Program has resulted in the hiring of
several staff who were either regionally underrepresented (local Hawaiian) and/or from
ethnic minorities (Native Hawaiian).
Andrew Whitehorse, a Native American, was promoted from general helper to plumber
at Sac Peak.
Irene González Hernández was the NISP Interior Program Scientist; she has moved to
the Interior Data Scientist position, and Kiran Jain is now the NISP Interior Program
Scientist.
ATST has hired several female lead engineers, including Heather Marshall, enclosure
engineer; LeEllen Phelps, thermal systems engineer; Pat Eliason, support structure
engineer (who has since returned to NISP), and Kerry Gonzales, opto‐mechanical
engineer.
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54 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
6.4 Public Outreach
6.4.1 Visitor Centers
The NSO Astronomy and Visitor Center at Sacramento Peak is host to over 15,000 visitors per
year. A wide range of interactive education displays at the Visitor Center provides hands‐on
experience with astronomical and terrestrial phenomena, interactive demonstrations on the
properties of light and how telescopes work, recent science results from both ground‐based and
space‐based solar and astrophysical experiments, and access to interactive Web‐based pages. The Kitt Peak Visitor Center also attracts more than 40,000 public visitors annually. Exhibits
adjacent to the gift shop include a large model of the McMath‐Pierce Solar Telescope, a live feed
for solar images, and a hands‐on display about spectroscopy and its solar science applications.
Daily tours of the McMP are available. The McMP facility also includes an educational exhibit
referred to as the “Sunnel.” The tunnel that leads from the entrance to the main observing room
features exhibits or displays that take the visitor from the center of the Sun to its outer
atmosphere along the length of the “Sunnel.” Because the Sunspot and Kitt Peak Visitor Centers are located in the Southwest, a large
proportion of visitors are Hispanic and Native American. NSO provides tours in both Spanish and
English. Sunspot has the largest solar system model in the Western US, the third largest in the US, and the
sixth largest in the world.
6.4.2 Internet Resources and Public Web Pages
As the public becomes more Internet‐savvy, organizations need to respond by continually
updating their presence on the Web. The NSO Web site provides information to the public on
solar physics and astronomy in general. Near‐real‐time solar images are available from NSO instruments on the following Web pages
http://www.nso.edu/current_images.html and http://nsosp.nso.edu/current_images. The Virtual Solar Observatory (VSO) is a cornerstone to ensuring that NSO data are accessible to
all scientists internationally. Currently, data from NISP/GONG and NISP/SOLIS are routinely
archive and available through the VSO portals.
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55 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
7 FY 2014 PROGRAM IMPLEMENTATION
The NSO FY 2014 Program Plan is designed to meet the expected level funding between FY 2013
and FY 2014. This has required some reductions in staffing and a delay in beginning some of the
planned ramp up toward ATST operations. Some of the impacts of level funding are being
addressed with revenues, indirect earnings and carry forward funds.
7.1 NSO Organization
During the ATST construction phase, the challenges to NSO have shifted. In addition to
transitioning personnel to ATST construction tasks, we have other personnel charging some of
their time to ATST and some to the base‐funded program. We are also ramping up a group on
NSO base funding to plan for ATST operations. Preventing the loss of essential personnel as we
pursue a new NSO directorate site location will be a challenge that the results of the Portfolio
Review have made more severe, especially with regard to the expertise to operate the NISP
components, SOLIS and GONG. The NSO will continue to pursue opportunities to increase diversity. Of special interest in this
regard are our work with the Akamai program and the University of Hawaiʻi on Maui, and our
participation in proposals with universities hosting large constituents of underrepresented
minorities (PAARE and the Fisk‐Vanderbilt Bridge‐to‐PhD programs). We will continue to
pursue EPO opportunities as funding permits. During this period, NSO needs to continue its strong support of the solar community while
using current assets to develop ATST instruments to test ATST operational concepts, and to
train personnel on the multi‐instrument, high‐data output expected with ATST. The new NSO
organizational structure is shown in Figure 7.1‐1.
7.1.1 Director’s Office
The NSO Director’s office consists of the Director, a Deputy Director, and an Executive
Administrative Manager; financial and budget support is also provided by the NSO/SP‐ATST
Facilities and Business Manager. A major change occurring this year is the stepping down of the
previous NSO Director, Stephen Keil, and the hiring of a new NSO Director. The NSO Director,
Valentín Martínez Pillet, is responsible for the overall NSO operations. The current NSO Deputy
Director, Mark Giampapa, serves as the interface with the NOAO for shared facilities, chairs the
Scientific Personnel Committee, and supervises senior scientific personnel in Tucson. His
funding is half in the Tucson base budget and half in the Director’s office FY 2014 budget. In
addition, the NSO Director obtains support from AURA Central Administrative Services (CAS)
for accounting, payroll, and human resources (HR), and from NOAO for graphics, IT support in
Tucson, and some educational outreach.
7.1.2 NSO/Sacramento Peak
NSO/SP operates the Dunn Solar Telescope on Sacramento Peak, provides facility support to the
ATST lab in the Hilltop Facility and provides occasional maintenance support for the Evans Solar
Facility in support of the Air Force group at Sac Peak. NSO/SP is undertaking several ATST work
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56 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Figure 7.1‐1. NSO Organizational Chart
packages during ATST construction. In addition to telescope support, the staff at SP supports an
office building, library, computing, instrument development, and housing facilities for visitors
and the resident scientific and technical staff. The ATST Director/PI, Thomas Rimmele, and the
ATST Project Scientist, Thomas Berger, currently reside at Sac Peak. The ATST wavefront sensor
project also resides at Sac Peak. Han Uitenbroek is the DST Program Scientist reporting to the
NSO Director, who also serves as Sac Peak site director. Han leads and oversees telescope
operations and instrument projects. Craig Gullixson is the DST Project and Support Manager.
Rex Hunter continues with the business management functions for NSO. Geoffrey Roberts is the
head of administrative support, and Bruce Smaga leads the facility crew. With the reduction in
technical staff, we have limited projects at the DST in order to concentrate on science operations with
the newly completed suite of diffraction‐limited instruments and support for testing of ATST
instrument technologies.
7.1.3 NSO Tucson and NSO Synoptic Program
NSO operates the McMath‐Pierce Solar Telescope on Kitt Peak, offices in Tucson, and conducts
projects at the Tucson facilities. The Deputy Director oversees Tucson programs and operations
with support from Priscilla Piano as Administrative Manager. McMath‐Pierce operations and
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57 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
projects are led by Telescope Scientist Matthew Penn, who reports to the Deputy Director. NISP
combines the SOLIS and GONG programs under Frank Hill as Associate Director. Both the
SOLIS Program Scientist, Alexei Pevtsov, and GONG Program Scientist, Kiran Jain, report to Hill.
Kim Streander manages projects and operational personnel in Tucson and also serves as Program
Manager for the NSO Integrated Synoptic Program (NISP). Sean McManus manages the NISP
Data Center.
7.1.4 NSO ATST
NSO/ATST is now funded through both the NSF MREFC program and through funds from the
American Recovery and Reinvestment Act (ARRA). Thomas Rimmele is the ATST Director/PI
and reports to the NSO Director. Project Manager Joseph McMullin and Project Scientist Tom
Berger report to the Project Director. The ATST project staff reside in Tucson, at Sacramento
Peak, in Boulder, and Hawaiʻi. There are plans to continue moving a few project personnel to
Boulder in FY 2014. Having staff at multiple locations allows the ATST team to interact with
NSO operations and projects. Lead engineers have responsibility for the various ATST work
packages. While some NSO personnel have transferred full time to ATST construction, others
work part time for the project. As NSO prepares for operations in the ATST era, the management structure will evolve as
needed to provide the most efficient and cost effective structure. NSO has begun
implementation of the reorganization that is needed to support ATST operations. ATST
commissioning will lead to the ramp down of current operations and divestment of current
facilities. In the ATST era, the NSO organizational structure will evolve to effectively support
ATST, the Synoptic Program, an instrument program, and a data processing and distribution
center.
7.2 Planning for the Future Organization of NSO
NSO plans call for consolidation of its Tucson and Sunspot staffs into an efficient organization to
operate the ATST, conduct synoptic programs, operate a data reduction and distribution center,
carry out forefront research by its staff and community, and to more effectively recruit new
students into solar astronomy. NSO’s new site will be on the east campus of the University of
Colorado, and NSO will share a building with the Laboratory for Atmospheric and Space Physics
(LASP). As operations at the two NSO sites are ramped down, establishing a single directorate
site at CU‐Boulder with a remote operational site on Maui for the ATST will be the best
configuration, allowing NSO to combine its science and engineering staff into a cohesive
organization. During FY 2014, AURA and NSO will work with NSF to establish a new cooperative agreement
that includes the planned move to Boulder and NSO will continue to develop and implement
plans for divestment of current facilities. The NSO Cooperative Agreement Proposal provides an
estimate of the cost of relocations to CU and the operating site for the ATST on Maui.
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58 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
7.3 FY 2014 Spending Plan
The NSO spending plan that follows is based on receiving the President’s FY 2014 budget request
of $8M for NSO.
7.3.1 Total Budget
Table 7.3‐1 summarizes the funding that NSO expects to receive as new NSF funding, as well as
anticipated non‐grant revenues for support of operations in FY 2014. The NSO program in FY
2014 was developed based on receiving $8,000K of NSF funding for the NSO base program. This
represents level funding from FY 2013 as well as a reduction in Air Force support for NISP.
These cuts were absorbed by reducing the NSO staff by several positions and moving some staff
to part‐ time. NSO expects $42M of MREFC funds in FY 2014 for the ATST project. The ATST
spending plan is presented in Section 5.1.3. NSO receives additional operational support from
the Air Force Research Laboratory (AFRL) through an MOU between the Air Force and NSF, in
exchange for supporting several AFRL staff at NSO/Sac Peak. NSO also receives funding from
the Air Force Weather Agency (AFWA) for GONG operations. NSO earns revenue from
cafeteria, Visitor Center, and housing operations on Sacramento Peak that are used to support the
respective functions.
Table 7.3-1. NSO FY 2014 Funding
(Dollars in Thousands)
NSF Astronomy Division Funding $8,000
AFRL Support for Sac Peak Operations 400
AFWA Support for GONG Operations 385
NSF REU/RET Program 107
Revenue (Housing, Kitchen, Visitor Center) 176
Programmed Indirects/Reserves 579
ATST Fellowship Support 105
Total NSO Funding 9,752
In addition to the funds shown in Table 7.3‐1, NSO receives funding through a variety of grants
and contracts with both NSO and non‐NSO principal investigators. These funds are used to hire
research fellows for specific programs, support visiting PIs and students, and to enhance
capabilities needed for these programs. The enhanced capabilities are then normally made
available to the user community. Table 7.3‐2 shows NSO’s currently active grants and contracts.
The funding shown in Table 7.3‐1 is allocated to the various programs NSO conducts to fulfill its
mission. Table 7.3‐3 shows the program areas in which funds will be expended, and those are
broken down further into the work packages within each funding area (telescope operations,
instrumentation, administration, EPO, etc.). The table also shows how we apply the revenue and
some of our indirect cost earnings to cover expenses not supported by the NSF FY 2014 funding.
NATIONAL SOLAR OBSERVATORY
59 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Table 7.3-2. NSO Grants and Contracts
Proposal Title Source Term PI Program FY 2014a Grant/Contract
Term Total a
NSF International Research Experiences for (Graduate) Students
NSF/IRES 2010-2013 Hill/Jain GONG 50,000b 150,000b
Development of MCAO for the 1.6 m BBSO Telescope
NSF/MRI sub-award via NJIT
2010-2013 Rimmele MCAO 93,280b 458,688b
Development of High-Order AO for the 1.6 m BBSO Telescope
NSF/ATI sub-award via NJIT
2010-2013 Rimmele HOAO 125,000b 125,000b
ISOON-Based Investigations of Solar Eruptions
AFRL 2011-2013 Radick/Keil AFRL/NSO Research
38,383 76,765
The Solar Mass Ejection Imager (SMEI) Space Experiment
AFRL 2012-2013 Radick/Keil SMEI 28,278 87,206
Using Helioseismology Measurements to Predict Active Region Flaring Probability
NASA sub-award via CU-Boulder
2010-2014 Komm NISP/GONG 72,860b
278,260b
Fast Processing of Spherical Seismic Holography
NASA sub-award via North-West Research Assoc.
2011-2013 González Hernández/Hill
NISP/GONG 77,300 121,403
Development of the Virtual Solar Observatory (VSO)
NASA 2011-2014 Hill VSO 103,386c 317,788c
An Investigation of the Physical Properties of Erupting Solar Prominences (Postdoc Support)
AFOSR 2011-2014 Radick/Altrock ESF 157,678 500,193
An Investigation of the Physical Properties of Erupting Solar Prominences Phase II
AFOSR 2014 Radick/Altrock ESF 29,232 29,232
New Aspects of Acceleration and Transport of Solar Energetic Particles (SEPs) from the Sun to the Earth
AFRL 2011-2014 Radick/Keil ESF 15,618 36,640
Incorporation of Solar Far-side Active Region Data within the Air Force ADAPT Model
AFOSR & AFRL 2011-2014 González Hernández
NISP GONG/SOLIS
55,316 159,979
Multi-wavelength Analysis of Solar Oscillations
NASA 2011-2014 Jain NISP/GONG 155,075 449,276
Helicity Transport from the Solar Interior to the Corona and its Role in Flares and Coronal Mass Ejections (CMEs)
NSF/AGS 2011-2014 Komm NISP/GONG 110,048 318,655
The influence of Subsurface (and Surface) Dynamics on the Activity Cycle
NASA 2011-2014 Komm NISP/GONG 136,505b 396,636b
Scientific Research Support Using Data from the Interface Region Imaging Spectrograph (IRIS)
NASA sub-award via Lockheed Martin Space Systems Co.
2011-2014 Uitenbroek IRIS Mission 93,884b 193,862b
Observing Support at the McMath-Pierce Solar Telescope
NASA 2011-2014 Penn/Giampapa McMP Observing
65,583 88,870
Implementation of Real-Time High-Resolution EUV Solar Spectral Irradiance
Air Force sub-award via North-West Research
2013-2014 González Hernández
NISP GONG/SOLIS
19,172
19,172
GONG Data for Nearly Continuous Observations of the Sun over Long Period
Air Force Weather Agency (AFWA)
2014 Hill NISP/GONG 374,760 374,760
TOTAL 1,801,358 4,182,385
aAmounts do not include NSF fee. bNSF fee not assessed. cDoes not include sub-awards to Stanford U., Harvard SAO, and Montana State.
Funding that NSO provides AURA for business support has been prorated to each program
area by the number of personnel and office space supported. Note that office space at Sac Peak is
supported under facilities at Sac Peak, and the AURA support for Sac Peak is primarily for HR,
accounting, and contracting.
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60 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Table 7.3-3. NSO Spending Plan
(Dollars in Thousands)
Directorʹs
Office Sunspot
Tucson Programs TOTAL
Expenses McMP NISP
Director, Staff, Committee Support 495 495
Directorate Site Development 74 0 74
Scientific Staff 741 247 1,329 2,317
Scientific Support/Computing 323 7 1,144 1,474
Telescope Support/Maint./Develop. 607 3 631 1,241
Telescope Operations 270 125 465 860
Facilities 677 0 0 677
Administrative Support 229 0 279 508
Education & Public Outreach1 94 113 20 36 263
AURA Business Support2 42 346 59 560 1,007
ATST Operations Development 407 65 0 473
ATST Fellow 105 0 0 105
AURA Management Fee 260 0 0 0 260
Program Total 964 3,818 526 4,444 9,752
Revenue
Programmed Indirects/Reserves (166) (329) (84) (579)
Housing Revenue (104) (104)
Meal Revenue (17) (17)
NSF REU/RET Funding (51) (20) (36) (107)
Air Force Support (400) (385) (785)
ATST Fellowship Support (105) (105)
Visitor Center Revenue (55) (55)
NSF/AST Funds 798 2,758 422 4023 8,000
1These funds are transferred to NOAO to support mutual EPO programs.2These funds are transferred to AURA for HR, procurement and accounting, contracting, and facilities services in
Tucson. 3AURA provides funds for cost sharing of an ATST Fellowship.
Figure 7.3‐1 lays out how NSO funding is divided among the various work packages, showing
that the science staff spends about 2/3 of its time supporting observatory operations, projects and
visitors (labeled Scientific Staff Support). Facilities, telescope operations, instrument development
and maintenance, and sciencesupport/computing are all part of NSO direct support for users of
NSO facilities.
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61 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Figure 7.3‐1. Distribution of NSO budget by tasks including revenue (total $9,752K)
7.3.2 Work Package Break Out
Tables 7.3‐4 to 7.3‐10 show the spending plan for the major functional areas in more detail,
breaking out payroll and non‐payroll by work packages.
7.3.2.1 Director’s Office
Table 7.3‐4 presents the Director’s office budget. Staff included in the Director’s office budget are
the Director, 0.5 of the Deputy Director’s salary, and an Executive Administrative Manager. As
noted earlier, the other half of the Deputy Director’s salary is included in the Tucson budget. Non‐
payroll expenses include travel, supplies and materials, and other miscellaneous expenses incurred
by the Director. Committees include the semi‐annual meetings of the NSO Users’ Committee and support for other
committee meetings as needed to support management of the observatory.
AURA central services includes support for the Director and Executive Administrative Manager
office space, HR, accounting and procurement in Tucson.
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62 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Table 7.3-4. Director’s Office
(Dollars in Thousands)
FTEs Payroll Non‐Payroll Total
Staff 2.3 462 33 495 Committees 9 9
Directorate Site Development 0.2 35 30 65
AURA Central Admin. Services 29 13 42
AURA Management Fee 260 260
Reserve 0 0
Outreach Support 65 28 94
Total Director’s Office 2.5 591 373 965
The AURA management fee line item is based on the NSO base budget. It covers management
support provided by AURA, including the Solar Observatory Council (SOC), which provides
management oversight and program advocacy. The outreach support goes to the NOAO Education and Public Outreach (EPO) division for
support received from EPO staff for various outreach programs.
7.3.2.2 Tucson/McMP Program
Tables 7.3‐5 and 7.3‐6 show the budget breakdown for Tucson and support for the McMath‐Pierce
Solar Telescope (McMP) facility and for the NSO Integrated Synoptic Program (NISP). It contains
$71K of indirect earnings.
The Tucson/McMP staff provide support for operations on Kitt Peak and for instrumentation and
maintenance of the McMath‐Pierce Solar Telescope. The NSO Deputy Director has 25% of his time
for research and 25% for management of programs in Tucson, where he acts on behalf of the
Director. The other 50% is in the Director Office where he works on documentation, diversity, and
other issues as they arise.
Table 7.3-5. NSO/Tucson/McMP (Dollars in Thousands)
FTEs Payroll Non‐Payroll TotalScientific Staff 1.5 234 13 247Science Support/Computing 7 7
Telescope Support/Maintenance/Develop. 3 3
Telescope Operations 1.00 82 43 125
Administration 0 0 0
AURA/NOAO Support 41 18 59
ATST Operations Planning 0.50 65 0 65
Outreach (REU/RET) 20 0 20
Total Tucson/McMP 3 442 84 526
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63 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
The 1.5 FTEs of scientific staff provide support of programs at the McMP, including the NSO Array
Camera (NAC) IR program and support for the California State University at Northridge integral
field unit (IFU). The salary figure includes a postdoctoral position and 50% of the Deputy
Director’s salary. The science staff also support related student programs and outreach.
Telescope operations consist of support for visiting and staff astronomers at the telescope, support
for installing upgrades and general telescope maintenance.
AURA/NOAO support consists of office and laboratory space in Tucson, HR, accounting, vehicles
support, shops, and janitorial services. Not listed because it is part of the NOAO/KPNO budget is
general maintenance support on the summit of Kitt Peak, road upkeep, cafeteria services, etc.
These costs are in the KPNO budget per the memorandum of agreement of 2000, when NSO
separated from NOAO.
Outreach funding is primarily for REU and RET participants that are supervised by the
NSO/Tucson scientific staff.
7.3.2.3 NSO Integrated Synoptic Program (NISP)
The NSO Integrated Synoptic Program combines staff from SOLIS and GONG under the direction
of Frank Hill as Associate Director.
Table 7.3-6. NSO Integrated Synoptic Program (Dollars in Thousands)
FTEs Payroll Non‐Payroll Total
Scientific Staff 10.10 1,275 54 1,329Scientce Support/Computing 10.50 1,038 107 1,144
Telescope Support/Maint./Develop. 5.14 472 159 631
Telescope Operations 1.50 93 371 465
Administration 2.00 219 60 279
Education & Public Outreach 0 29 7 36
AURA/NOAO Support 0 392 168 560
Total NISP 29.24 3,518 926 4,444
NISP is broken down into an Atmospheric section and an Interior section, each led by a program
scientist reporting to the NISP Associate Director. The Telescope Support/Maintenance/Develop‐
ment staff are supervised by a Program Manager and support both SOLIS and GONG
instruments and upgrades as required. The science staff support the various data products
produced by NISP and respond to the communityʹs need for new products.
Both SOLIS and GONG data are reduced daily and added to the NSO Digital Library, where they
can be downloaded by the solar community.
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64 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
AURA/NOAO support consists of office and laboratory space in Tucson, HR, accounting, vehicles
support, shops, and janitorial services. Table 7.3‐6 also includes the support received from the Air
Force Weather Agency..
7.3.2.4 Sacramento Peak
Table 7.3‐7 breaks out the Sacramento Peak operations budget. NSO/SP scientific staff support
the Dunn Solar Telescope and participate in development of ATST operations. The DST Program
Scientist oversees telescope operations and projects and supervises the NSO/SP Technical and
Telescope Operations Manager, IT support, and the DST chief observer. The scientists also
support the TAC process and observatory operations (library, outreach, instrument program,
modeling, and users). The ATST fellowship supports an ATST postdoctoral position that is cost‐
shared with AURA.
Table 7.3-7. NSO Sacramento Peak (Dollars in Thousands)
FTEs Payroll Non‐Payroll Total
Scientific Staff 4.8 700 41 741
Science Support/Computing 3.00 237 85 323
Telescope Support/Maint./Develop. 7.3 572 35 607
Telescope Operations 3.15 244 26 270
Facilities 6 303 374 677
ATST Operations Planning 2.5 371 37 407
ATST Fellow 1 100 5 105
Administration 3.2 209 20 229
AURA Support 0 277 69 346
Outreach (REU/RET), Visitor Center 1 83 30 113
Total NSO/SP 31.15 3096 722 3,818
The Telescope Support/Maintenance/Development staff support DST maintenance and opera‐
tions and upgrades to the DST control system and focal‐plane instrumentation so users can take
full advantage of diffraction‐limited imaging. The DST is also serving as a test bed for ATST by
exploring ways to operate several instruments simultaneously. We would also like to use the DST
for prototyping various ATST control software and operational concepts.
Telescope staff operate the DST, provide user support, help with instrumentation installation and
interfaces, and perform maintenance tasks on the telescope. The telescope is allocated and
operated on all but two days out of the year, weather permitting.
The Sac Peak administrative staff oversee general site maintenance and daily site operations,
logistical visitor support, purchasing, shipping, receiving, and budgeting. The facilities budget
includes costs for buildings (offices, shops, civil engineering facilities, and administrative
facilities), grounds, maintenance, utilities, housing (funding for housing support comes from
NATIONAL SOLAR OBSERVATORY
65 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
rental revenue), water and sewage treatment, site snow removal and road maintenance. NOAO
support includes HR, accounting, contracting, and some legal support.
Outreach includes REU and RET support, public outreach programs, and operation of the
Sunspot Astronomy and Visitor Center. Table 7.3‐8 contains the $400K contribution from the US Air Force as well as the revenue earned from
housing, meal services, Visitor Center sales and $329K of indirect earnings and carry forward. The
US AF funding is added to NSO’s general operations funding to offset the support provided to the
Air Force Research Laboratory program at Sac Peak. During FY 2011, one AF staff scientist moved
to Albuquerque and the AF group added a new scientist and a postdoctoral fellow. Table 7.3‐8
provides an estimate of how AF funds are used to support the AFRL program. This varies from
year to year, based on program needs and facility usage.
Table 7.3-8. Air Force FY 2014 Funding (Dollars in Thousands)
Payroll Non‐Payroll Total
Scientific Support/Computing 50 45 95
Telescope Operations 75 35 110
Library Services 15 10 25
Facilities 74 76 150
Administrative Services 15 5 20
Total Air Force Funding $229 $171 $400
7.4 Infrastructure Plan and Strategic Needs
Although NSO plans to divest its current facilities, with the commissioning date and scientific
operation of the Advanced Technology Solar Telescope about six years away, NSO must continue
to serve the US solar community with its current facilities and maintain them in a manner that
keeps US solar astronomers at the forefront of solar physics. Additionally, we believe that the
facilities at Sac Peak and Kitt Peak will have a life beyond the NSO and our plan is to find parties
to which we can transfer these facilities. We have an obligation as a steward of government owned
facilities to maintain them at an appropriate level that will allow a suitable transfer to a qualified
operating institution. Continued investment in the maintenance of Sac Peak and the DST is not only important for
supporting high‐resolution solar physics, but also for development of ATST instruments and
operations. The plan for maintaining Sac Peak is designed to address infrastructure needs that will
ensure the viability of current NSO assets to support the solar user community for the next several
years. We also need to maintain and enhance our synoptic programs. With the Portfolio Review
mandate for NSO to find outside funding for the majority of NISP operations, its important that
the NISP instruments and data products are maintained and improved to attract funding sources
such as the NOAA Space Weather Predictions Center (SWPC) and the Air Force Weather Agency.
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66 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Infrastructure funds are used to support forefront solar research by replacing failing and outdated
systems at our telescopes and data handling facilities and to ensure continued safety of operations
at NSO’s observatory sites.
Because of continued near level support (often below level, sometimes above, but never sufficient
to account for inflation), NSO has limited its small amount of allocated base infrastructure
spending to critical items for maintaining safety and telescope operations. It has generated
requests for additional funding for larger ticket items and for those maintenance items not covered
in exiting budgets. The supplemental funding received from the American Reinvestment and
Recovery Act (ARRA) has permitted NSO to catch up in several areas. We have integrated these
into our overall plan.
7.4.1 FY 2014 Unfunded Infrastructure Improvement Requests
The major funding reduction in FY 2013 limited NSO to conducting only essential routine
maintenance. To insure the NSO facilities are in good condition to enhance divestment
opportunities, we request additional funding for the list of items in Table 7.4‐1. Completion of
these items would ensure that NSO continues with robust operations until ATST is online, and that
NSO facilities will be attractive to potential organizations willing to take over when NSO ceases Sac
Peak and Tucson operations.
Table 7.4-1 Unfunded Infrastructure Improvements (Dollars in Thousands)
Item Cost Notes
NSO/Sac Peak DST Turret Repair 75 Replace obsolete controls and hardware Computer Numerical Controlled (CNC) Lathe 50 Instrument development for SP and ATST DST Data Acquisition System 80 Continue upgrade to handle larger, faster CCDs Main Lab Boiler Lines and Radiators 50 Replace obsolete heating system, reduce cost
Apartment Building Boiler Lines and Water Lines 50 Replace obsolete heating and water lines, reduce cost Vehicle Replacement 25 Replace older vehicle Dump Truck/Snow Plow 65 Replace old truck Redwood Building Painting 35 Contract to paint redwood buildings Total NSO/SP 430 NSO/Tucson GONG Air Conditioner Replacements 25 Replace obsolete units with energy efficient model SOLIS Structure Modification 50 Required for remote observations at new, permanent location Total NSO/T 75
7.4.2.1 NSO/SP
DST Basic Infrastructure Improvements
Other basic infrastructure investments needed at the DST to upgrade/replace aging equipment,
provide safety improvements, and ensure continued smooth DST operations include:
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67 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
DST Turret Repair and Controls Upgrade. Replace 1960’s hardware with digital hardware.
Estimated Cost: $75K.
CNC Lathe. Needed for on‐site ATST machine shop work. Estimated Cost: $50K.
Modernizing the DST Data Acquisition System (DAS), i.e., data storage, network, acquisition
system (to handle the increased data loads from high‐speed large‐format cameras). Estimated
Cost: $80K.
NSO/SP Facilities
Historically, the budget for NSO/SP has included approximately $40K in funds above our normal
maintenance program for use on larger “projects.” Typically, we saved or carried over some of
these funds to accomplish these projects that were beyond our normal budget. With the
continuing rise in cost of building supplies, propane, and electricity, and our flat budgets, our
discretionary funds have been absorbed into the daily maintenance activities. The size of these
projects make them very difficult or impossible for us to accomplish without supplemental
funding. Each of these items has been evaluated with the development of the ATST and the
expected closure or divestiture of Sac Peak in mind, and represents improvements needed in the
short term.
Main Lab Boiler Line and Radiator Replacement. Request $50K: The Main Lab houses the
offices of three‐quarters of our staff and computing facilities. The facility is over 40 years
old and is heated with a hot water system with radiators in individual offices. The boiler
was replaced about 15 years ago but remains serviceable. The hot water lines connecting
the boiler to the individual radiators and the radiators themselves have never been
replaced. We are experiencing multiple failures of these lines each winter and expect that
pattern to worsen. A catastrophic failure during the winter months could make the
facility uninhabitable for an extended period of time. This project would replace all of
the lines and the radiators. Replacement of the radiators with more modern units should
increase the efficiency and improve the quality of heat in the building.
Apartment Building Boiler Line and Water Line Replacement. Request $50K: The apartment
building is our primary source of housing for official visitor and users of the telescopes.
As with the Main Lab, the facility is over 40 years old and has had little maintenance to
the hot water heating and drinking water lines during that time. Failures are becoming
frequent and maintenance costs are rising. This project would replace all the hot water
heater lines, radiators and drinking water lines. This will greatly improve the quality of
heat in the building and the drinking water.
Vehicle Replacement. Request $25K: One of our current staff vehicles has well over 100K
miles and is beginning to experience more maintenance problems. These vehicles are
heavily used for transportation of our staff to Tucson, El Paso (airport) and other
locations. Frequently, they are driven in very remote parts of the country and at odd
hours and conditions where breakdowns could be dangerous. Also, with the funding of
the ATST and the participation of many of our current employees, our travel to Tucson
and other locations has increased dramatically, requiring that all of our staff vehicles be
available for use.
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68 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
Dump Truck/Snow Plow Replacement. Request $65K: Current dump truck is about 20 years
old. As with the loader, it is heavily used for snow removal and is experiencing more
problems. Maintenance costs and dependability have negatively impacted our facilities
maintenance staff and will continue to grow as it ages. As our main road plow, a
catastrophic breakdown during the winter would have a severe impact on our ability to
complete snow removal.
Redwood Building Painting. Request $35K: Redwoods including the apartment building
and the community center have not been repainted for approximately 20 years. Paint is
beginning to peel and subject the wood exterior to the severe elements at Sac Peak. The
wood exteriors will deteriorate fairly quickly in this environment causing more costly
repairs in the future.
7.4.2.2 NSO/Tucson
NISP
New Air Conditioning Units for GONG Network. The current units are old and ineffecient.
Current electric usage can be reduced by ~30% with higher effeciency systems.
Estimated Cost: $25K.
Modify Existing SOLIS Structure at Tucson Site to Test and House Instrument Suite Prior to
Move to Permanent Location. The existing structure needs to be fitted with a movable section
on the south side to be lowered out of the line‐of‐sight for observations. The modified
structure will demonstrate the ability to take remote observations. The structure will be
dismantled and relocated to a permanent site at later date. Estimated Cost: $50K.
NATIONAL SOLAR OBSERVATORY
APPENDICES
APPENDIX A. NSO 2020 – 2025 VISION
APPENDIX B. OBSERVING & USER STATISTICS
APPENDIX C. ORGANIZATIONAL PARTNERSHIPS
APPENDIX D. PUBLICATIONS
APPENDIX E. MILESTONES FOR FY 2014
APPENDIX F. STATUS OF 2013 MILESTONES
APPENDIX G. FY 2014 STAFFING SUMMARY
APPENDIX H. SCIENTIFIC STAFF RESEARCH & SERVICE
APPENDIX I. ACRONYM GLOSSARY
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70 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
APPENDIX A. NATIONAL SOLAR OBSERVATORY 2020–2025 VISION1
NSO will support and lead community research into the nature of the Sun by providing critical ground‐
based optical capabilities. The Sun is the archetypal astrophysical body, and we can exploit its proximity
to explore fundamental processes not directly observable elsewhere in the Universe. Perhaps more
importantly, the Sun is the source of the highly variable heliosphere in which the Earth and humanity
reside. NSO’s unique facilities will include the worldʹs largest solar telescope and a network of full‐Sun
imaging magnetometers to continuously observe the Sunʹs structure and evolution. A resident scientific
staff will support the development and exploitation of these facilities, support a diverse community of users, and point the way to mid‐century frontiers.
The NSO 2020 ‒ 2025 vision provides critical capabilities for solar research that address both
fundamental science issues and vital societal imperatives enunciated in several decadal surveys
‒ New Worlds, New Horizons in Astronomy and Astrophysics, and The Sun to the Earth and Beyond
(and its successor Solar and Space Physics Decadal Survey to be released in Spring 2012) ‒ as well
as the recent NSF sponsored Workshop on the Future of Ground‐based Solar Physic. The NSO
science vision is focused on the basic question1 of how the Sun creates and evolves its magnetic
field: to understand the fundamental physics and its manifestations in other astrophysical
settings, and how this violent activity impacts the solar system and Earth while also helping to
shield humanity from dangerous galactic cosmic particles. The NSO vision of societal benefits
and impacts centers on research leading to a predictive capability for variations of the Sunʹs
radiative and eruptive outputs and planetary effects2. The NSO vision is founded upon
community‐based research objectives and requirements, and enables effective responses to new
discoveries, synergistic research with planned and future space missions, and testing the results
of advanced numerical models of solar phenomena.
To achieve this vision for the solar research community, NSO is replacing its 50+ year old
facilities with major new observational capabilities. The range of observational capabilities that
will be available in 2020 ‒ 2025 includes world‐leading high‐resolution observations of the
vector magnetic field, thermal and dynamic structure of the solar surface and atmosphere, and
measurements of structure and dynamics of the solar interior, both for short‐term and solar‐
cycle‐long time periods. These capabilities will be provided by the high‐resolution Advanced
Technology Solar Telescope (ATST) and moderate‐resolution, nearly continuous (ʺsynopticʺ)
observations of the full solar disk through the NSO Integrated Synoptic Program (NISP).
NSO in 2020 and beyond will enable the community to:
1. Clearly resolve fundamental magnetic structure and processes in space and time, and
achieve high photon flux for accurate, precise measurements of physical parameters
throughout the solar atmosphere4;
1See NSO 2012‐2016 Long Range Plan for science goals (http://www.nso.edu/reports) 2NWNH, p. 64 3 NWHH, pp. 29, 37,38, 60,61, 115 4 NWHH, p. 64
NATIONAL SOLAR OBSERVATORY
71 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
2. Study the drivers and manifestations of the long‐term, quasi‐cyclic, inhomogeneous and
intermittent solar magnetic fields and flows;
3. Resolve outstanding uncertainties in the abundance of atomic species;
4. Understand space weather and climate as they affect Earth, the solar system, and space
assets today5, and as a pathfinder for the study of exo‐planet habitability;
5. Prepare the next diverse generation of solar researchers; and,
6. Carry out coordinated investigations with solar space‐based missions using NSO’s robust
and adaptable capabilities.
To achieve this, the NSO will in priority order:
1. Operate and enhance the ATST, currently under development; and
2. Operate and enhance the multi‐site NISP
To continue NSO’s engagement in education and outreach NSO will6:
1. Conduct a vigorous training program for undergraduate, graduate, thesis students, and
postdoctoral fellows;
2. Provide research experience and science training for middle school and high school
teachers;
3. Conduct public outreach through its visitor center, tours, classroom talks and displays;
and,
4. Increase its efforts to establishing a more diverse NSO staff and bringing
underrepresented minorities into science and engineering in general.
Failure to build ATST or a serious delay in its construction would create a significant gap in US
solar astronomy. We would lose the capability to probe the physics of solar magnetic fields on
spatial and temporal scales that are critical (according to both theory and observation) for
understanding the energy balance of the Sun (and stars) and solar activity that impacts Earth.
While space missions provide a complementary part of the required capability, a permanent
space‐borne 4m class telescope with the necessary functionality and flexibility is not affordable.
5 NWNH, p. 29: Serving the Nation 6 NWNH, Chapter 4
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72 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
APPENDIX B: OBSERVING AND USER STATISTICS
(OCTOBER 1, 2012 ‐ SEPTEMBER 30, 2013)
In the 12 months ended 30 September 2013, 64 observing programs, which included 11 thesis
programs, were carried out at NSO. Associated with these programs were 67 scientists, students
and technical staff from 27 US and foreign institutions.
*IncludesobservingprogramsconductedbyAURAstaffscientists.
**Note: Total number of institutions represented by users do not includeDepartmentsordivisionwithinaninstitutionasseparateentities(e.g.,U.S.Air Force and NASA are each counted as one institution even thoughdifferentsites/bases/centersareseparatelylistedinthedatabase.
12 Months Ended September 2013 Nbr % Total
Programs (US, involving 2 non-thesis grad students) 50 78%
Programs (non-US, involving 1 non-thesis grad student) 3 5%
Thesis (US, involving 10 grad students) 8 13%Thesis (non-US, involving 5 grad students) 3 5%
Total Number of Unique Science Projects* 64 100%
NSO Observing Programs by Type(US and Foreign)
AURA StaffUS Non-US Total % Total
PhDs 33 18 51 76% 17
Graduate Students 6 8 14 21% 0
Undergraduate Students 0 0 0 0% 0Other 2 0 2 3% 14
Total Users 41 26 67 100% 31
Users of NSO Facilities by CategoryVisitors
US Non-US Total % Total
Academic 12 7 19 70%
Non-Academic 4 4 8 30%
Total Academic & Non-Academic 16 11 27 100%
Institutions Represented by Visiting Users**
Belgium 2 Italy 7
Germany 7 Mexico 1
Ireland, UK 9 United States 72
Number of Users by Nationality
Institutions Represented by Users Foreign Institutions (11)
Armagh Observatory, University of Sheffield INAF - Arcetri Astrophysical Observatory INAF, Instituto di Fisica dello Spazio Interplanetario Katholieke Universiteit Leuven Leibniz Institute for Astrophysics Potsdam (AIP) Max-Planck-Institut für Aeronomie Queen's University Belfast Universidad de Monterrey, Mexico University of Köln, Germany University of Naples, Osservatorio Astron. di Capodimonte University of Rome "Tor Vergata" US Institutions (16)
Alfred University California State University, Northridge Edinboro University High Altitude Observatory, NCAR, Boulder Lockheed-Martin Solar & Astrophysics Laboratory Montana State University NASA/Ames Research Center NASA/Goddard Space Flight Center (NASA/GSFC) New Jersey Institute of Technology New Mexico State University Salpointe Catholic High School University of Arizona University of Florida University of Colorado, CASA University of Hawaii, IFA University of Texas-Austin, McDonald Observatory US Air Force/Philips Lab (USAF/PL/GSS)
NATIONAL SOLAR OBSERVATORY
73 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
FY 2013 USER STATISTICS – TELESCOPE USAGE & PERFORMANCE DATA
In the fiscal year ended 30 September 2013, 40.5% of the total available telescope hours at
NSO/Sacramento Peak and NSO/Kitt Peak went to the observing programs of visiting principal
investigators; 18.7% were devoted to those of NSO scientists. Scheduled maintenance (including
instrument tests, engineering, and equipment changes) accounted for 3.5% of total allotted telescope
hours.
Total ʺdowntimeʺ (hours lost to weather and equipment problems) for NSO telescopes was 37.3%. A
significant portion of these lost observing hours were due to bad weather (33.0%), with 4.3% lost to
equipment problems.
aIncludessynopticprogramsforwhichalldataaremadeavailableimmediatelytothepublicandscientificcommunityatlarge.bFormerlytheKittPeakVacuumTelescope(KPVT).cDuringFY12,theFTSwasmovedoutoftheMcMath‐PierceFacilityandtoauniversitycampus.*Totalsincludebothdayandnighthours.(Allothersaredayonly.)
% DISTRIBUTION OF TELESCOPE HOURSALL NSO TELESCOPES
Maintenance 3.53%
Visitorsa
40.53%
Staff 18.65%
Weather32.95%
Equipment4.34%
% Hrs. Lost To:Hours
Scheduled Visitorsa Staff Weather Equipment Scheduled Maintenance
Dunn Solar Telescope/SP 3,774.0 19.6% 27.9% 34.0% 2.4% 16.1%McMath-Pierce* 5,316.0 30.1% 40.5% 24.7% 4.7% 0.0%KP SOLIS Towera,b 6,024.0 64.5% 0.0% 29.5% 6.0% 0.0%FTS Labc* 0.0 0.0% 0.0% 0.0% 0.0% 0.0%Evans Solar Facility 2,064.0 35.6% 0.0% 62.5% 1.9% 0.0%Hilltop Dome 0.0 0.0% 0.0% 0.0% 0.0% 0.0%
All Telescopes 17,178.0 40.5% 18.7% 32.9% 4.3% 3.5%
NSO TELESCOPESPercent Distribution of Telescope Hours
(Scheduled vs. Downtime)01 October 2012 - 30 September 2013
Telescope% Hours Used By: % Hours Lost To:
NATIONAL SOLAR OBSERVATORY
74 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
FY 2013 USER STATISTICS – ARCHIVES & DATA BASES
(October 1, 2012 ‐ September 30, 2013)
All statistics exclude the use of NSO archives and data bases from within the NSO Local Area
Network in Tucson and at Sac Peak, and from AURA/NOAO as a whole.
0.0
1,000.0
2,000.0
3,000.0
4,000.0
5,000.0
6,000.0
7,000.0
GB
ytes
U.S. Science (.gov, .edu, .mil)Other U.S. (.com, .net, misc.)ForeignUnresolved
DATA (Gbytes) DOWNLOADED FROM NSO FTP & WWW SITES 01 October 2012 - 30 September 2013
Domain GbytesU.S. Science (.gov, .edu, .mil ) 6,556.3Other U.S. (.com, .net, misc. ) 662.4Foreign 3,152.8Unresolved 1.4 TOTAL 10,372.8
Site Product Type Gbytes %
T NISP/GONG Helioseismology 3,599.92 35.488%T NISP/GONG (Magnetograms, spectra, time series, frequencies) 3,431.63 33.829%T NISP/GONG H-alpha 2,273.57 22.413%T NISP/SOLIS (VSM, ISS, FDP) 635.94 6.269%
SP & T Other 103.57 1.021%T FTS (Spectral atlases, general archive) 66.00 0.651%
SP Staff Pages 17.42 0.172%SP Press Releases 6.58 0.065%T KPVT (magnetograms, synoptic maps, helium images) 3.98 0.039%T Evans/SP Spectroheliograms (Hα, Calcium K images) 2.90 0.029%
SP General Information 1.72 0.017%SP DST Service Mode Support 0.75 0.007%
SP SMEI Experiment & Data Pages 0.03 0.000%SP Icon & Background Images 0.03 0.000%
TOTAL 10,144.04 100.000%
PRODUCT DISTRIBUTION BY DOWNLOADED GBYTES 01 October 2012 - 30 September 2013
NATIONAL SOLAR OBSERVATORY
75 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
APPENDIX C: ORGANIZATIONAL PARTNERSHIPS
C1. Community Partnerships and NSO Leadership Role
Through its operation of the majority of US ground‐based solar facilities and its ongoing synoptic
programs, NSO is clearly important to the solar community. In turn, NSO must work closely with
the solar community and provide leadership to strengthen solar research, renew solar facilities and
to develop the next generation of solar instrumentation. Recent examples of NSO meeting this
responsibility include the addition of rapid magnetograms and Hα images to GONG; development
of solar adaptive optics and multi‐conjugate adaptive optics for both NSO and university telescopes;
development of infrared observing capabilities in collaboration with the University of Hawaiʻi, California State University‐Northridge, and NASA; leading the development of SPINOR in
collaboration with HAO, and participating in IBIS with Arcetri Observatory, and ROSA with Queens
University Belfast. Table C.1 lists several ongoing joint projects and development efforts. NSO will continue to work closely with the ATST Science Working Group and the community to
develop a sound operations plan for exploiting the full potential of the ATST.
NSO sponsored several community workshops and forged an alliance of 22 institutions to develop a
proposal for the design of the ATST and its instrumentation. NSO worked closely with this group
in leading the successful completion of the design and transition to construction of the telescope.
Beginning in 2009, the ATST project began a series of workshops on ATST science operations to
provide guidance for developing a sound plan for exploiting the full potential of the ATST.
Table C.1. Joint Development Efforts Telescope/Instrument/Project Collaborators
Advanced Technology Solar Telescope (ATST) HAO, U. Hawaiʻi, U. Chicago, NJIT, Montana State U., Princeton U., Harvard/Smithsonian CfA, UC-San Diego, UCLA, U. Colorado, NASA/GSFC, NASA/MSFC, Caltech, Michigan State U., U. Rochester, Stanford U., Lockheed-Martin, Southwest Research Institute, NorthWest Research Associates, Cal State Northridge
Adaptive Optics, Multi-Conjugate AO NJIT, Kiepenheuer Institute, AFRL Diffraction-Limited Spectro-Polarimeter ((DLSP) HAO Spectropolarimeter for Infrared and Optical Regions (SPINOR) HAO Rapid Oscillations in the Solar Atmosphere (ROSA) Instrument
Queen’s University, Belfast
Narrowband Filters and Polarimeters Arcetri Observatory, Kiepenheuer Institute Synoptic Solar Measurements USAF/AFRL, NASA IR Spectrograph and Cameras U. Hawaiʻi, Cal State Northridge, NJIT Advanced Image Slicer & Integral Field Unit Cal State Northridge Virtual Solar Observatory NASA, Stanford, Montana State, Harvard-SAO H-alpha Imaging System (GONG) Air Force Weather Agency (AFWA)/AFRL
NATIONAL SOLAR OBSERVATORY
76 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
C2. Operational Partnerships
NSO’s strategic planning embraces the interdisciplinary nature and dual objectives of solar physics in
that it is both basic science and applied research. Likewise, NSO’s relationships to its users reflect the
diversity and richness of the communities they represent—solar and stellar astronomy, space plasma
physics, solar‐terrestrial relationships, space weather prediction, terrestrial atmospheric chemistry,
and more. Table C.2 is a summary of the current partnerships that provide operational support. NSO’s long‐standing relationship with the US Air Force space science group will continue into the
ATST era. The Air Force Research Laboratory (AFRL) and its Office of Scientific Research (AFOSR)
have indicated a desire to keep their basic solar research program colocated with NSO. They are
contributing to the ATST project through their mirror coating chamber and are looking for ways to
support ATST detector development. Currently, NSO is vigorously pursuing other partnerships. It
has had discussions with many organizations and has received letters of intent from several
institutions to support ATST construction. These include organizations in Germany; the United
Kingdom; a consortium of the Netherlands, Sweden, and Norway; and the US Air Force. Other
potential partnerships include Italy, Japan, Spain, and Canada. Scientists from Italy, Japan, and Spain
are currently involved on the ATST Science Working Group. NSO has formed a close working
relationship with the University of Hawai‘i for ATST operations and expects other partners to have some involvement in operations as well.
NISP is actively seeking operational partnerships with members of the space environment
community, including international partnerships for site operations and data processing. The Air
Force has provided NISP/GONG with funds to add an Hα capability in anticipation of helping to
fund GONG operations.
Table C.2. Current NSO Partnerships
Partner Program
Air Force Research Laboratory - Solar activity research at NSO/SP; telescope operations; adaptive optics; instrument development; 5 scientists, including 1 postdoc, stationed at NSO/SP; daily coronal emission line measurements; provides operational funding for SP: $400K-Base and various amounts for instrument development.
- NSO/Tucson Farside ADAPT Project support (0.25 FTE).
Air Force Weather Agency Funded the addition of an H-alpha capability for GONG. Providing ~740K/year for GONG/Synoptic Program operations.
NASA - Funding for SOLIS Science Goals: Postdoctoral Research Associates (1.25 FTE); Instrument/Observing Specialist (0.5 FTE).
- McMath-Pierce: Support for Operation of the FTS (1.0 FTE); Upper Atmospheric Research; Solar-Stellar Research; Planetary Research.
- DST: Support for a Research Fellow for Hinode mission support (coordinated observations, science planning, mission operations, data analysis) (via Lockheed- Martin sub-award).
- GONG: 3.0 FTE Scientific Support; SDO/HMI Pipeline Development Support (0.7 FTE). - Virtual Solar Observatory Development Support (0.75 FTE). - Development of VSM advanced flux estimate map for next general model of the corona and solar wind (via SAIC sub-award).
- SHINE research support for 3 scientists at 0.17 FTE each. - SDO/GONG White-light flare study support via UC-Berkeley SSL sub-award (0.11 FTE) - Active Region Flaring Predictions using Helioseismology research support via CU-
Boulder sub-award (0.33 FTE).
NATIONAL SOLAR OBSERVATORY
77 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
APPENDIX D: PUBLICATIONS (OCTOBER 2012 THROUGH
SEPTEMBER 2013)
Author—NSO Staff Author—REU
Author—RET Author—Grad Student
Author —Non‐REU Undergrad
Refereed Publications 1. Alissandrakis, C., and Patsourakos, S., “Hot coronal loops associated with umbral brighten‐
ingsʺ, A&A 556: A79, 08/2013.
2. Altrock, R. C., “Forecasting the Maxima of Solar Cycle 24 with Coronal Fe XIV Emissionʺ,
SoPh Online First, 01/2013.
3. Amari, T., Aly, J.‐J., Canou, A., and Mikic, Z., “Reconstruction of the solar coronal magnetic
field in spherical geometryʺ, A&A 553: A43, 05/2013.
4. Antia, H. M., Chitre, S., and Gough, D., “On the magnetic field required for driving the
observed angular‐velocity variations in the solar convection zoneʺ, MNRAS 428: 470, 01/2013.
5. Ayres, T. R., Lyons, J., Ludwig, H‐G., Caffau, E., and Wedemeyer‐Böhm, S., “Is the Sun
Lighter than the Earth? Isotopic CO in the Photosphere, Viewed through the Lens of Three‐
dimensional Spectrum Synthesisʺ, ApJ 765(1): 46, 03/2013.
6. Baldner, C. S., Basu, S., Bogart, R. S., Burtseva, O., González Hernández, I., Haber, D. A.,
Hill, F., Howe, R., Jain, K., Komm, R. W., et al., “Latest Results Found with Ring‐Diagram
Analysisʺ, SoPh 287: 57, 10/2013.
7. Banerji, M., McMahon, R. G., Hewett, P. C., Alaghband‐Zadeh, S., Gonzalez‐Solares, E.,
Venemans, B. P., and Hawthorn, M. J., “Heavily reddened quasars at z ~ 2 in the UKIDSS
Large Area Survey: a transitional phase in AGN evolutionʺ, MNRAS 427: 2275, 12/2012.
8. Berger, T. E., Liu, W., and Low, B. C., “SDO/AIA Detection of Solar Prominence Formation
within a Coronal Cavityʺ, ApJL 758(2): L37, 10/2012.
9. Bertello, L., Pevtsov, A. A., and Pietarila, A., “Signature of Differential Rotation in Sun‐as‐a‐Star CaII K Measurementsʺ, ApJ 761(1): 11, 12/2012.
10. Bi, Y., Jiang, Y., Li, H., Hong, J., and Zheng, R., “Eruption of a Solar Filament Consisting of
Two Threadsʺ, ApJ 758(1): 42, 10/2012.
11. Birch, A. C., Braun, D. C., Leka, K. D., Barnes, G., and Javornik, B., “Helioseismology of Pre‐
emerging Active Regions. II. Average Emergence Propertiesʺ, ApJ 762: 131, 01/2012, 2013.
12. Bisoi, S. Kumar, Janardhan, P., Chakrabarty, D., Ananthakrishnan, S., and Divekar, A.,
“Changes in Quasi‐periodic Variations of Solar Photospheric Fields: Precursor to the Deep
Solar Minimum in Cycle 23?ʺ, SoPh Online First, 07/2013.
13. Broiles, T. W., Desai, M. I., Lee, C. O., and MacNeice, P. J., “Radial evolution of the three‐
dimensional structure in CIRs between Earth and Ulyssesʺ, JGRA 118: 4776‐4792, 08/2013.
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78 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
14. Burtseva, O., and Petrie, G. J. D., “Magnetic Flux Changes and Cancellation Associated with
X‐Class and M‐Class Flaresʺ, SoPh 283(2): 429, 04/2013.
15. Cameron, R. H., Dasi‐Espuig, M., Jiang, J., Işik, E., Schmitt, D., and Schüssler, M., “Limits to
solar cycle predictability: Cross‐equatorial flux plumesʺ, A&A 557: A141, 09/2013.
16. Cegla, H., Shelyag, S., Watson, C., and Mathioudakis, M., “Stellar Surface Magneto‐
convection as a Source of Astrophysical Noise. I. Multi‐component Parameterization of
Absorption Line Profilesʺ, ApJ 763(2): 95, 02/2013.
17. Choudhary, D. P., Gosain, S., Gopalswamy, N., Manoharan, P. K., Chandra, R., Uddin, W.,
Srivastava, A. K., Yashiro, S., Joshi, N. C., Kayshap, P., et al., “Flux emergence, flux
imbalance, magnetic free energy and solar flaresʺ, AdSpR 52: 1561, 10/2013.
18. Chowdhury, P., Choudhary, D. P., and Gosain, S., “A Study of the Hemispheric Asymmetry
of Sunspot Area during Solar Cycles 23 and 24ʺ, ApJ 768(2): 188, 05/2013.
19. Civiš, S., Ferus, M., Chernov, V., and Zanozina, E., “Infrared transitions and oscillator
strengths of Ca and Mgʺ, A&A 554: A24, 06/2013.
20. Cranmer, S. R., van Ballegooijen, A. A., and Woolsey, L. N., “Connecting the Sunʹs High‐
resolution Magnetic Carpet to the Turbulent Heliosphereʺ, ApJ 767(2): 125, 04/2013.
21. Criscuoli, S., “Comparison of Physical Properties of Quiet and Active Regions through the
Analysis of MHD Simulations of the Solar Photosphere ʺ, ApJ 778(1): 27, 11/2013.
22. Criscuoli, S., Del Moro, D., Giannattasio, F., Viticchié, B., Giorgi, F., Ermolli, I., Zuccarello, F.,
and Berrilli, F., “High cadence spectropolarimetry of moving magnetic features observed
around a poreʺ, A&A 546: 26, 10/2012.
23. Criscuoli, S., Ermolli, I., Uitenbroek, H., and Giorgi, F., “Effects of Unresolved Magnetic
Field on Fe I 617.3 and 630.2 nm Line Shapesʺ, ApJ 763(2): 144, 02/2013.
24. de la Cruz Rodríguez, J., Rouppe van der Voort, L., Socas‐Navarro, H., and van Noort, M.,
“Physical properties of a sunspot chromosphere with umbral flashesʺ, A&A 556: A115,
08/2013.
25. de Toma, G., Chapman, G., Cookson, A., and Preminger, D., “Temporal Stability of Sunspot
Umbral Intensities: 1986‐2012ʺ, ApJL 771(2): L22, 07/2013.
26. DeForest, C. E., Howard, T. A., and Tappin, S. J., “The Thomson Surface. II. Polarizationʺ,
ApJ 765: 44, 03/2013.
27. Deland, M., and Marchenko, S., “The solar chromospheric Ca and Mg indices from Aura
OMIʺ, JGRD 118: 3415, 04/2013.
28. Deng, N., Tritschler, A., Jing, J., Chen, X., Liu, C., Reardon, K. P., Denker, C., Xu, Y., and
Wang, H., “High‐cadence and High‐resolution Hα Imaging Spectroscopy of a Circular Flareʹs
Remote Ribbon with IBISʺ, ApJ 769(2): 112, 06/2013.
29. Eckart, A., Mužić, K., Yazici, S., Sabha, N., Shahzamanian, B., Witzel, G., Moser, L., Garcia‐
Marin, M., Valencia‐S, M., Jalali, B., et al., “Near‐infrared proper motions and spectroscopy of
infrared excess sources at the Galactic centerʺ, A&A 551: A18, 03/2013.
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79 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
30. Eff‐Darwich, A., and Korzennik, S. G., “The Dynamics of the Solar Radiative Zoneʺ, SoPh
287(1‐2): 43, 10/2013.
31. Fischer, C. E., Keller, C. U., Snik, F., Fletcher, L., and Socas‐Navarro, H., “Unusual Stokes V
profiles during flaring activity of a delta sunspotʺ, A&A 547: 34, 11/2012.
32. Francile, C., Costa, A., Luoni, M., and Elaskar, S., “Hα Moreton waves observed on December
06, 2006. A 2D case studyʺ, A&A 552: A3, 04/2013.
33. Giersch, O., “GONG Inter‐site Hα Flare Comparisonʺ, JPhCS 440(1): 2006, 06/2013.
34. González Hernández, I., Díaz Alfaro, M., Jain, K., Tobiska, W. K., Braun, D. C., Hill, F., and
Pérez Hernández, F., “A Full‐Sun Magnetic Index from Helioseismology Inferencesʺ, SoPh
Online First, 07/2013.
35. Gosain, S., and Foullon, C., “Dual Trigger of Transverse Oscillations in a Prominence by
EUV Fast and Slow Coronal Waves: SDO/AIA and STEREO/EUVI Observationsʺ, ApJ 761(2):
103, 12/2012.
36. Gosain, S., and Pevtsov, A. A., “Resolving Azimuth Ambiguity Using Vertical Nature of
Solar Quiet‐Sun Magnetic Fieldsʺ, SoPh 283(1): 195, 03/2013.
37. Gosain, S., Pevtsov, A. A., Rudenko, G. V., and Anfinogentov, S. A., “First Synoptic Maps of
Photospheric Vector Magnetic Field from SOLIS/VSM: Non‐radial Magnetic Fields and
Hemispheric Pattern of Helicityʺ, ApJ 772(1): 52, 07/2013.
38. Gosain, S., Schmieder, B., Artzner, G., Bogachev, S., and Török, T., “A Multi‐spacecraft View
of a Giant Filament Eruption during 2009 September 26/27ʺ, ApJ 761(1): 25, 12/2012.
39. Gough, D., “Commentary on a putative magnetic field variation in the solar convection
zoneʺ, MNRAS 435(4): 3148, 11/2013.
40. Greco, V., and Cavallini, F., “Optical design of a near‐infrared imaging spectropolarimeter for
the ATSTʺ, OptEng 52: 063001, 06/2013.
41. Harker, B. J., “Parameter‐free Automatic Solar Active Region Detection by Hermite Function
Decompositionʺ, ApJSS 203: 7, 11/2012.
42. Hesman, B. E., Bjoraker, G. L., Sada, P. V., Achterberg, R. K., Jennings, D. E., Romani, P. N.,
Lunsford, A. W., Fletcher, L., Boyle, R. J., Simon‐Miller, A. A., et al., “Elusive Ethylene
Detected in Saturnʹs Northern Storm Regionʺ, ApJ 760: 24, 11/2012.
43. Hinkle, K. H., Wallace, L., Ram, R. S., Bernath, P. F., Sneden, C., and Lucatello, S., “The
Magnesium Isotopologues of MgH in the A 2^Π‐X 2^Σ+ Systemʺ, ApJS 207(2): 26, 08/2013.
44. Howard, T. A., Tappin, S. J., Odstrčil, D., and DeForest, C. E., “The Thomson Surface. III.
Tracking Features in 3Dʺ, ApJ 765: 45, 03/2013.
45. Howe, R., Christensen‐Dalsgaard, J., Hill, F., Komm, R. W., Larson, T. P., Rempel, M., Schou,
J., and Thompson, M. J., “The High‐latitude Branch of the Solar Torsional Oscillation in the
Rising Phase of Cycle 24ʺ, ApJL 767: L20, 04/2013.
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80 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
46. Howe, R., Jain, K., Bogart, R. S., Haber, D. A., and Baldner, C. S., “Two‐Dimensional
Helioseismic Power, Phase, and Coherence Spectra of SDO Photospheric and Chromospheric
Observablesʺ, SoPh 281(2): 533, 12/2012.
47. Iorio, L., “Constraining the Angular Momentum of the Sun with Planetary Orbital Motions
and General Relativityʺ, SoPh 281: 815, 12/2012.
48. Javaraiah, J., “A Comparison of Solar Cycle Variations in the Equatorial Rotation Rates of the
Sunʹs Subsurface, Surface, Corona, and Sunspot Groupsʺ, SoPh 287(1‐2): 197‐214, 10/2013.
49. Jess, D. B., De Moortel, I., Mathioudakis, M., Christian, D. J., Reardon, K. P., Keys, P. H., and
Keenan, F. P., “The Source of 3 Minute Magnetoacoustic Oscillations in Coronal Fansʺ, ApJ
757: 160, 10/2012.
50. Jiang, Y., Hong, J., Yang, J., Bi, Y., Zheng, R., Yang, B., Li, H., and Yang, D., “Partial Slingshot
Reconnection between Two Filamentsʺ, ApJ 764: 68, 02/2013.
51. Jin, C. L., Harvey, J. W., and Pietarila, A., “Synoptic Mapping of Chromospheric Magnetic
Fluxʺ, ApJ 765(2): 79, 03/2013.
52. Johnstone, B. M., Petrie, G. J. D., and Sudol, J. J., “Abrupt Longitudinal Magnetic Field
Changes and Ultraviolet Emissions Accompanying Solar Flaresʺ, ApJ 760(1): 29, 11/2012.
53. Joshi, N. C., Uddin, W., Srivastava, A. K., and et al., “A multiwavelength study of eruptive
events on January 23, 2012 associated with a major solar energetic particle eventʺ, AdSpR
52(1): 1, 07/2013.
54. Karachik, N. V., and Pevtsov, A. A., “Properties of Magnetic Neutral Line Gradients and
Formation of Filamentsʺ, SoPh Online First, 08/2013.
55. Keys, P. H., Mathioudakis, M., Jess, D. B., Shelyag, S., Christian, D. J., and Keenan, F. P.,
“Tracking magnetic bright point motions through the solar atmosphereʺ, MNRAS 428(4):
3220, 02/2013.
56. Kholikov, S., ʺA Search for Helioseismic Signature of Emerging Active Regionsʺ, SoPh 287(1‐
2): 229, 10/2013.
57. Kholikov, S., and Hill, F., “Meridional Flow Measurements from Global Oscillation Network
Groupʺ, SoPh Online First, 09/2013.
58. Kirk, M. S., Balasubramaniam, K. S., Jackiewicz, J., McNamara, B. J., and McAteer, R. T. J.,
“An Automated Algorithm to Distinguish and Characterize Solar Flares and Associated
Sequential Chromospheric Brighteningsʺ, SoPh 283(1): 97, 03/2013.
59. Kleint, L., and Sainz Dalda, A., “Unusual Filaments inside the Umbraʺ, ApJ 770(1): 74,
06/2013.
60. Ko, Y‐K., Tylka, A. J., Ng, C. K., Wang, Y‐M., and Dietrich, W. F., “Source Regions of the
Interplanetary Magnetic Field and Variability in Heavy‐ion Elemental Composition in
Gradual Solar Energetic Particle Eventsʺ, ApJ 776(2): 92, 10/2013.
61. Komm, R. W., Gosain, S., and Pevtsov, A. A., “Active Regions with Superpenumbral Whirls
and Their Subsurface Kinetic Helicityʺ, SoPh Online First, 01/2013.
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81 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
62. Korngut, P. M., Renbarger, T., Arai, T., Battle, J., Bock, J., Brown, S. W., Cooray, A., Hristov,
V., Keating, B., Kim, M. G., et al., “The Cosmic Infrared Background Experiment (CIBER):
The Narrow‐Band Spectrometerʺ, ApJS 207: 34, 08/2013.
63. Korzennik, S. G., and Eff‐Darwich, A., “Mode Frequencies from 17, 15 and 2 Years of GONG,
MDI, and HMI Dataʺ, JPhCS 440(1): 2015‐, 06/2013.
64. Korzennik, S. G., Rabello‐Soares, M. C., Schou, J., and Larson, T., “Accurate characterization
of high‐degree modes using MDI dataʺ, JPhCS 440(1): 012016, 06/2013.
65. Kramar, M., Inhester, B., Lin, H., and Davila, J., “Vector Tomography for the Coronal
Magnetic Field. II. Hanle Effect Measurementsʺ, ApJ 775(1): 25, 09/2013.
66. Kretzschmar, M., Dominique, M., and Dammasch, I., “Sun‐as‐a‐Star Observation of Flares in
Lyman α by the PROBA2/LYRA Radiometerʺ, SoPh 286: 221, 08/2013.
67. Kuridze, D., Mathioudakis, M., Kowalski, A. F., Keys, P. H., Jess, D. B., Balasubramaniam, K.
S., and Keenan, F. P., “A Failed Filament Eruption Inside a Coronal Mass Ejection in Active
Region 11121ʺ, A&A 552: A55, 04/2013.
68. Lam, H. ‐ L., Boteler, D. H., Burlton, B., and Evans, J., “Anik‐E1 and E2 satellite failures of
January 1994 revisitedʺ, SpWea 10: 10003, 10/2012.
69. Lawler, J. E., Guzman, A., Wood, M. P., Sneden, C., and Cowan, J. J., “Improved Log(gf)
Values for Lines of Ti I and Abundance Determinations in the Photospheres of the Sun and
Metal‐Poor Star HD 84937 (Accurate Transition Probabilities for Ti I)ʺ, ApJS 205(2): 11,
04/2013.
70. Lee, C. O., Arge, C. N., Odstrčil, D., Millward, G., Pizzo, V., Quinn, J. M., and Henney, C. J.,
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71. Leka, K. D., Barnes, G., Birch, A. C., González Hernández, I., Dunn, T., Javornik, B., and
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73. Liewer, P. C., González Hernández, I., Hall, J. R., Thompson, W. T., and Misrak, A.,
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77. Martínez Oliveros, J., Lindsey, C., Hudson, H. S., and Buitrago Casas, J., “Transient Artifacts
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80. Morton, R. J., Verth, G., Jess, D. B., Kuridze, D., Ruderman, M. S., Mathioudakis, M., and
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81. Nagovitsyn, Y. A., Pevtsov, A. A., and Livingston, W. C., “On a Possible Explanation of the
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82. Nelson, C. J., Doyle, J. G., Erdélyi, R., Huang, Z., Madjarska, M. S., Mathioudakis, M.,
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83. Nikitin, A., Brown, L., Sung, K., Rey, M., Tyuterev, V., Smith, M.A.H., and Mantz, A.,
“Preliminary modeling of CH3D from 4000 to 4550 cm‐1ʺ, JQSRT 114: 1, 01/2013.
84. Norquist, D. C., “Forecast performance assessment of a kinematic and a magnetohydro‐
dynamic solar wind modelʺ, SpWea 11: 17‐33, 01/2013.
85. Nuevo, F. A., Huang, Z., Frazin, R., Manchester, W. B., Jin, M., and Vásquez, A. M.,
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86. Pereira, T. M. D., Asplund, M., Collet, R., Thaler, I., Trampedach, R., and Leenaarts, J., “How
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87. Petrie, G. J. D., “Evolution of Active and Polar Photospheric Magnetic Fields During the Rise
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88. Petrie, G. J. D., “Solar Magnetic Activity Cycles, Coronal Potential Field Models and
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89. Petrie, G. J. D., and Haislmaier, K. J., “Low‐latitude Coronal Holes, Decaying Active
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90. Pevtsov, A. A., Bertello, L., and Uitenbroek, H., “On Possible Variations of Basal Ca II K Chromospheric Line Profiles with the Solar Cycleʺ, ApJ 767(1): 56, 04/2013.
91. Pevtsov, A. A., Bertello, L., Tlatov, A. G., Kilcik, A., Nagovitsyn, Y. A., and Cliver, E. W.,
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92. Pietarila, A., and Harvey, J. W., “Ca II 854.2 nm Bisectors and Circumfacular Regionsʺ, ApJ
764(2): 153, 02/2013.
93. Pietarila, A., and Pietarila‐Graham, J., “Instrumental and Observational Artifacts in Quiet
Sun Magnetic Flux Cancellation Functionsʺ, SoPh 282(2): 389, 02/2013.
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94. Pietarila, A., Bertello, L., Harvey, J. W., and Pevtsov, A. A., “Comparison of Ground‐Based
and Space‐Based Longitudinal Magnetogramsʺ, SoPh 282(1): 91, 01/2013.
95. Potter, A. E., Killen, R. M., Reardon, K. P., and Bida, T. A., “Observation of neutral sodium
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96. Qiu, J., Cheng, J. X., Hurford, G. J., Xu, Y., and Wang, H., “Solar flare hard X‐ray spikes
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97. Richards, M. T., Agafonov, M. I., and Sharova, O. I., “New Evidence of Magnetic Interactions
between Stars from Three‐dimensional Doppler Tomography of Algol Binaries: β PER and RS
VULʺ, ApJ 760(1): 8, 11/2012.
98. Richards, M. T., Hill, F., and Stassun, K. G., “No Evidence Supporting Flare‐Driven High‐
Frequency Global Oscillationsʺ, SoPh 281(1): 21, 11/2012.
99. Riley, P., Linker, J. A., and Mikić, Z., “On the application of ensemble modeling techniques to
improve ambient solar wind modelsʺ, JGRA 118: 600, 02/2013.
100. Romano, P., Berrilli, F., Criscuoli, S., Del Moro, D., Ermolli, I., Giorgi, F., Viticchié, B., and
Zuccarello, F., “A Comparative Analysis of Photospheric Bright Points in an Active Region
and in the Quiet Sunʺ, SoPh 280: 407, 10/2012.
101. Romano, P., Frasca, D., Guglielmino, S. L., Ermolli, I., Tritschler, A., Reardon, K. P., and
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771(1): L3, 07/2013.
102. Scargle, J. D., Keil, S. L., and Worden, S. P., “Solar Cycle Variability and Surface Differential
Rotation from Ca II K‐line Time Series Dataʺ, ApJ 771(1): 33, 07/2013.
103. Schad, T. A., Penn, M. J., and Lin, H., “He I Vector Magnetometry of Field‐aligned
Superpenumbral Fibrilsʺ, ApJ 768(2): 111, 05/2013.
104. Schmieder, B., Kucera, T. A., Knizhnik, K., Luna, M., Lopez‐Ariste, A., and Toot, D.,
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108, 11/2013.
105. Shayesteh, A., Ram, R. S., and Bernath, P. F., ʺFourier transform emission spectra of the A2Π
→ X2Σ+ and B2Σ+ → X2Σ+ band systems of CaHʺ, JMoSp 288: 46, 06/2013.
106. Shi, X. J., and Xie, J. L., “The Rotation Profile of Solar Magnetic Fields between ±60°
Latitudesʺ, ApJL 773(1): L6, 08/2013.
107. Simoniello, R., Jain, K., Tripathy, S. C., Turck‐Chièze, S., Baldner, C. S., Finsterle, W., Hill, F.,
and Roth, M., “The Quasi‐biennial Periodicity as a Window on the Solar Magnetic Dynamo
Configurationʺ, ApJ 765(2): 100, 03/2013.
108. Simoniello, R., Jain, K., Tripathy, S. C., Turck‐Chièze, S., Finsterle, W., and Roth, M.,
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12/2012.
109. Sobotka, M., Švanda, M., Jurčák, J., Heinzel, P., and Del Moro, D., “Atmosphere above a large
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110. Sornig, M., Sonnabend, G., Stupar, D., Kroetz, P., Nakagawa, H., and Mueller‐Wodarg, I.,
“Venusʹ upper atmospheric dynamical structure from ground‐based observations shortly
before and after Venusʹ inferior conjunction 2009ʺ, Icar 225: 828‐839, 07/2013.
111. Sriramachandran, P., and Shanmugavel, R., “Identification of Zirconium Oxide molecular
lines in the sunspot umbral spectraʺ, NewA 17: 640‐645, 10/2012.
112. Stenflo, J. O., “Solar magnetic fields as revealed by Stokes polarimetryʺ, A&ARv 21: 66,
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113. Tadesse, T., Wiegelmann, T., Inhester, B., and Pevtsov, A. A., “Coronal Magnetic Field
Structure and Evolution for Flaring AR 11117 and Its Surroundingsʺ, SoPh 281(1): 53, 11/2012.
114. Tadesse, T., Wiegelmann, T., Inhester, B., MacNeice, P., Pevtsov, A. A., and Sun, X., “Full‐
disk nonlinear force‐free field extrapolation of SDO/HMI and SOLIS/VSM magnetogramsʺ,
A&A 550: A14, 02/2013.
115. Tadesse, T., Wiegelmann, T., MacNeice, P., and Olson, K., “Modeling coronal magnetic field
using spherical geometry: cases with several active regionsʺ, ApSS 347: 21‐27, 09/2013.
116. Tadesse, T., Wiegelmann, T., MacNeice, P., Inhester, B., Olson, K., and Pevtsov, A. A., “A
Comparison Between Nonlinear Force‐Free Field and Potential Field Models Using Full‐Disk
SDO/HMI Magnetogramʺ, SoPh Online First, 09/2013.
117. Tappin, S. J., and Altrock, R. C., “The Extended Solar Cycle Tracked High into the Coronaʺ,
SoPh 282(1): 249, 01/2013.
118. Tlatov, A. G., and Pevtsov, A. A., “Bimodal Distribution of Magnetic Fields and Areas of
Sunspotsʺ, SoPh Online First, 08/2013.
119. Tripathy, S. C., Jain, K., and Hill, F., “Acoustic Mode Frequencies of the Sun during the
Minimum Phase between Solar Cycles 23 and 24ʺ, SoPh 282(1): 1, 01/2013.
120. Tripathy, S. C., Jain, K., Howe, R., Bogart, R. S., and Hill, F., “Helioseismic analysis of active
regions using HMI and AIA dataʺ, AN 333: 1013, 12/2012.
121. Vieytes, M., and Fontenla, J. M., “Improving the Ni I Atomic Model for Solar and Stellar
Atmospheric Modelsʺ, ApJ 769: 103, 06/2013.
122. Wang, H., and Liu, C., “Circular Ribbon Flares and Homologous Jetsʺ, ApJ 760: 101, 12/2012.
123. Wiedenbeck, M., Mason, G., Cohen, C.M.S., Nitta, N., Gómez‐Herrero, R., and Haggerty, D.,
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Heliographic Longitudeʺ, ApJ 762(1): 54, 01/2012, 2013.
124. Wood, M. P., Lawler, J. E., Sneden, C., and Cowan, J. J., “Improved Ti II Log(gf) Values and
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ApJS 208: 27, 10/2013.
125. Wright, J. T., Roy, A., Mahadevan, S., Wang, S. X., Ford, E. B., and et al., “MARVELS‐1: A
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126. Xie, H., St. Cyr, O. C., Gopalswamy, N., Odstrčil, D., and Cremades, H., “Understanding
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127. Yan, X. L., Pan, G. M., Liu, J. H., Qu, Z. Q., Xue, Z. K., Deng, L. H., Ma, L., and Kong, D. F.,
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128. Yeates, A. R., “Coronal Magnetic Field Evolution from 1996 to 2012: Continuous Non‐
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129. Zhilyaev, B. E., Verlyuk, I. A., Andreev, M. V., and et al., “Observations of high‐frequency
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Conference Proceedings and Other Publications
1. Arge, C. N., Henney, C. J., González Hernández, I., Toussaint, W. A., Koller, J., and Godinez,
H. C., “Modeling the corona and solar wind using ADAPT maps that include far‐side
observationsʺ, SOLAR WIND 13: Proceedings of the Thirteenth International Solar Wind
Conference, AIP Conf Proc 1539: 11, 06/2013.
2. Aschwanden, M. J., “Coronal Seismology with ATSTʺ, The Second ATST‐EAST Meeting:
Magnetic Fields from the Photosphere to the Corona, ASP Conf Ser 463: 133, 12/2012.
3. Ayres, T. R., Lyons, J., Ludwig, H‐G., Caffau, E., and Wedemeyer‐Böhm, S., “Solar carbon
monoxide: poster child for 3D effectsʺ, MmSAI 24: 85, 00/2013.
4. Barden, S. C., “The Simple Hyperspectral Imaging Polarimeter Conceptʺ, The Second ATST‐
EAST Workshop in Solar Physics: Magnetic Fields from the Photosphere to the Corona, ASP Conf
Ser 463: 453, 12/2012.
5. Beck, C. A. R., and Rezaei, R., “Chromospheric Multi‐Wavelength Observations near the
Solar Limb: Techniques and Prospectsʺ, The Second ATST‐EAST Meeting: Magnetic Fields from
the Photosphere to the Corona, ASP Conf Ser 463: 257, 12/2012.
6. Berger, T. E., “The Prominence/Coronal Cavity System: a unified view of magnetic structures
in the Solar coronaʺ, The Second ATST‐EAST Workshop in Solar Physics: Magnetic Fields from the
Photosphere to the Corona, ASP Conf Ser 463: 147, 12/2012.
7. Bisoi, S. Kumar, and Janardhan, P., “Asymmetry in the periodicities of solar photospheric
fields: A probe to the unusual solar minimum prior to cycle 24ʺ, Solar and Astrophysical
Dynamos and Magnetic Activity, IAUS 294: 85, 07/2013.
8. Bisoi, S. Kumar, and Janardhan, P., “Peculiar behavior of solar polar fields during solar cycles
21‐23: Correlation with meridional flow speedʺ, Solar and Astrophysical Dynamos and Magnetic
Activity, IAUS 294: 81, 07/2013.
9. Bućík, R., Mall, U., Korth, A., Mason, G., and Gómez‐Herrero, R., “3He‐rich SEP events
observed by STEREO‐Aʺ, SOLAR WIND 13: Proceedings of the Thirteenth International Solar
Wind Conference, AIP Conf Proc 1539: 139, 06/2013.
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86 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
10. Burtseva, O., Tripathy, S. C., Bogart, R. S., Jain, K., Howe, R., Hill, F., and Rabello‐Soares, M.
C., “Temporal Variations of High‐Degree Solar p‐Modes using Ring‐Diagram Analysisʺ,
JPhCS 440: 012027, 06/2013.
11. Cadavid, A. C., Lawrence, J. K., Christian, D. J., Jess, D. B., and Mathioudakis, M., “Turbulent
Fluctuations in G‐band and K‐line Intensities Observed with the Rapid Oscillations in the
Solar Atmosphere (ROSA) Instrumentʺ, The Second ATST‐EAST Meeting: Magnetic Fields from
the Photosphere to the Corona, ASP Conf Ser 463: 75, 12/2012.
12. Cauzzi, G., and Reardon, K. P., “The IBIS Mosaicʺ, Science with Large Solar Telescopes,
Proceedings of IAU Special Session 6: E5.11, 12/2012.
13. Choudhary, D. P., and Deng, N., “Photospheric and Chromospheric Measurements of a
High‐Speed Flow near the Light Bridge of a δ ‐Spotʺ, The Second ATST‐EAST Workshop in
Solar Physics: Magnetic Fields from the Photosphere to the Corona, ASP Conf Ser 463: 43, 12/2012.
14. Criscuoli, S., Ermolli, I., Uitenbroek, H., and Giorgi, F., “On the sensitivity of FeI 617.3 and
630.2 nm line shapes to unresolved magnetic fieldsʺ, MmSAI 84: 335, 00/2013.
15. Cristaldi, A., Guglielmino, S. L., Zuccarello, F., Ermolli, I., Falco, M., and Criscuoli, S.,
“Small‐scale brightenings observed in active regions with SST and Hinodeʺ, MmSAI 84: 339,
00/2013.
16. Del Moro, D., Berrilli, F., Stangalini, M., Giannattasio, F., Piazzesi, R., Giovannelli, L.,
Viticchié, B., Vantaggiato, M., Sobotka, M., Jurčák, J., et al., “IBIS: High‐Resolution Multi‐
Height Observations and Magnetic Field Retrievalʺ, The Second ATST‐EAST Meeting:
Magnetic Fields from the Photosphere to the Corona, ASP Conf Ser 463: 33, 12/2012.
17. Deng, N., Tritschler, A., Jing, J., Chen, X., Reardon, K. P., Liu, C., Xu, Y., and Wang, H., “H‐
alpha Imaging Spectroscopy of a C‐class flare with IBISʺ, Science with Large Solar Telescopes,
Proceedings of IAU Special Session 6, IAUS: E3.07, 12/2012.
18. Elmore, D. F., “ATST Telescope Calibration: Summary of Studies and their Conclusionsʺ,
The Second ATST‐EAST Meeting: Magnetic Fields from the Photosphere to the Corona, ASP Conf
Ser 463: 307, 12/2012.
19. Falco, M., Zuccarello, F., Criscuoli, S., Cristaldi, A., Guglielmino, S. L., and Ermolli, I.,
“Sunspot evolution observed with SSTʺ, MmSAI 84: 345, 00/2013.
20. González Hernández, I., Komm, R. W., van Driel‐Gesztelyi, L., Baker, D., Harra, L., and
Howe, R., “ Subsurface flows associated with non‐Joy oriented active regions: a case studyʺ,
JPhCS 440: 012050, 06/2013.
21. González Hernández, I., Lindsey, C., Braun, D. C., Bogart, R. S., Scherrer, P. H., and Hill, F.,
“Far‐side helioseismic maps: the next generationʺ, JPhCS 440: 012029, 06/2013.
22. Gosain, S., Sankarasubramanian, K., Venkatakrishnan, P., and Raja Bayanna, A., “A New
Technique for Solar Imaging Spectro‐polarimetry using Shack‐Hartmann and Fabry‐Pérotʺ,
The Second ATST‐EAST Meeting: Magnetic Fields from the Photosphere to the Corona, ASP Conf
Ser 463: 301, 12/2012.
23. Howe, R., Broomhall, A‐M., Chaplin, W. J., Elsworth, Y., and Jain, K., “Low‐degree multi‐
NATIONAL SOLAR OBSERVATORY
87 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
spectral p‐mode fittingʺ, JPhCS 440: 012011, 06/2013.
24. Jain, K., Tripathy, S. C., Basu, S., Bogart, R. S., González Hernández, I., Hill, F., and Howe,
R., “Multi‐spectral study of acoustic mode parameters and sub‐surface flowsʺ, JPhCS 440:
012012, 06/2013.
25. Jain, K., Tripathy, S. C., Hill, F., and Larson, T., “Solar oscillations in cycle 24 ascendingʺ, JPhCS 440: 012023, 06/2013.
26. Johnson, L. C., Upton, R., Rimmele, T. R., Hubbard, R. P., and Barden, S. C., “Active Optical Control of Quasi‐Static Aberrations for ATSTʺ, The Second ATST‐EAST Meeting: Magnetic
Fields from the Photosphere to the Corona, ASP Conf Ser 463: 315, 12/2012.
27. Kirk, M. S., Balasubramaniam, K. S., Jackiewicz, J., McAteer, R. T. J., and McNamara, B. J.,
“Sequential Chomospheric Brightening: An Automated Approach to Extracting Physics from
Ephemeral Brighteningʺ, The Second ATST‐EAST Meeting: Magnetic Fields from the Photosphere
to the Corona, ASP Conf Ser 463: 267, 12/2012.
28. Komm, R. W., González Hernández, I., Harra, L., Baker, D., and van Driel‐Gesztelyi, L.,
“Are subsurface flows and coronal holes related?ʺ, JPhCS 440: 012022, 06/2013.
29. Marino, J., and Rimmele, T. R., “Expected Performance of Adaptive Optics in Large
Aperture Solar Telescopesʺ, The Second ATST‐EAST Meeting: Magnetic Fields from the
Photosphere to the Corona, ASP Conf Ser 463: 329, 12/2012.
30. Martin, S. F., Panasenco, O., Berger, M. A., Engvold, O., Lin, Y., Pevtsov, A. A., and
Srivastava, N., “The Build‐Up to Eruptive Solar Events Viewed as the Development of Chiral
Systemsʺ, The Second ATST‐EAST Meeting: Magnetic Fields from the Photosphere to the Corona,
ASP Conf Ser 463: 157, 12/2012.
31. Nelson, C. J., Doyle, J. G., Erdélyi, R., Madjarska, M. S., and Mumford, S. J., “Ellerman bombs:
small‐scale brightenings in the photosphereʺ, MmSAI 84: 436, 00/2013.
32. Norton, A. A., Jones, E. H., Liu, Y., Hayashi, K., Hoeksema, J.T., and Schou, J., “How much
more can sunspots tell us about the solar dynamo?ʺ, Solar and Astrophysical Dynamos and
Magnetic Activity, IAUS 294, 07/2013.
33. Orozco Suárez, D., Bellot Rubio, L. R., and Katsukawa, Y., “Requirements for the Analysis of
Quiet‐Sun Internetwork Magnetic Elements with EST and ATSTʺ, The Second ATST‐EAST
Meeting: Magnetic Fields from the Photosphere to the Corona, ASP Conf Ser 463: 57, 12/2012.
34. Pietarila, A., “Magnetometry with Large Solar Telescopes: Beyond the Photospheric
Boundariesʺ, The Second ATST‐EAST Meeting: Magnetic Fields from the Photosphere to the
Corona, ASP Conf Ser 463: 3, 12/2012.
35. Rimmele, T. R., Tritschler, A., Wöger, F., Collados, M., and et al., “The 2nd ATST‐EAST
Workshop in Solar Physics: Magnetic Fields from the Photosphere to the Coronaʺ, The Second
ATST‐EAST Workshop in Solar Physics: Magnetic Fields from the Photosphere to the Corona, ASP
Conf Ser 463, 12/2012.
36. Rimmele, T. R., Keil, S. L., McMullin, J. P., Goode, P. R., Knoelker, M., Kuhn, J. R., Rosner,
R., and ATST Team, “Construction of the Advanced Technology Solar Telescope ‐ A ona,
NATIONAL SOLAR OBSERVATORY
88 NSO FY 2013 Annual Progress Report & FY 2014 Program Plan
ASP Conf Ser 463: 25, 12/2012.
37. Schad, T. A., Penn, M. J., Lin, H., and Tritschler, A., “He I Spectropolarimetry with FIRS:
Towards Vector Magnetometry of Chromospheric Fibrils Plus New Diagnostics of Coronal
Rainʺ, The Second ATST‐EAST Meeting: Magnetic Fields from the Photosphere to the Corona, ASP
Conf Ser 463, 12/2012.
38. Stein, R.F., and Nordlund, A., “Flux Emergence and Pore Formation: What ATST can Seeʺ,
The Second ATST‐EAST Workshop in Solar Physics: Magnetic Fields from the Photosphere to the
Corona, ASP Conf Ser 463: 83, 12/2012.
39. Strassmeier, K. G., Carroll, T. A., Ilyin, I., and Järvinen, S., “Observational methods for stellar
magnetism: from detection to cartographyʺ, Solar and Astrophysical Dynamos and Magnetic
Activity, IAUS 294, 07/2013.
40. Taylor, G. E., Rimmele, T. R., Marino, J., Tritschler, A., and McAteer, R. T. J., “Solar Limb
Adaptive Optics: A Test of Wavefront Sensors and Algorithmsʺ, The Second ATST‐EAST
Meeting: Magnetic Fields from the Photosphere to the Corona, ASP Conf Ser 463: 321, 12/2012.
41. Tripathy, S. C., Jain, K., Simoniello, R., Hill, F., and Turck‐Chièze, S., “Solar cycle and quasi‐
biennial variations in helioseismic frequenciesʺ, Solar and Astrophysical Dynamos and Magnetic
Activity, IAUS 294, 07/2013.
42. Tritschler, A., Uitenbroek, H., and Rempel, M., “The Sunspot Penumbra in the Photosphere:
Results from Forward Synthesized Spectroscopyʺ, The Second ATST‐EAST Meeting: Magnetic
Fields from the Photosphere to the Corona, ASP Conf Ser 463: 89, 12/2012.
43. Uitenbroek, H., “Eyes on the Sun: Solar Instrumentationʺ, 370 Years of Astronomy in Utrecht,
ASP Conf Ser 470: 83, 01/2013.
44. Uitenbroek, H., and Criscuoli, S., “A novel method to estimate temperature gradients in
stellar photospheresʺ, MmSAI 84: 369, 00/2013.
45. Uitenbroek, H., and Tritschler, A., “Observing strategies for future solar facilities: the ATST test caseʺ, Science with Large Solar Telescopes, Proceedings of IAU Special Session 6: E4.01, 12/2012.
46. Uitenbroek, H., Dumont, N., and Tritschler, A., “The Influence of Molecular Lines on the
Measurement of Photospheric Velocitiesʺ, The Second ATST‐EAST Meeting: Magnetic Fields
from the Photosphere to the Corona, ASP Conf Ser 463: 99, 12/2012.
47. Warner, M., McMullin, J. P., Rimmele, T. R., and Berger, T. E., “The Advanced Technology Solar Telescope project: a construction updateʺ, Solar Physics and Space Weather
Instrumentation V, Proc SPIE 8862: 88620D, 09/2013.
48. Wöger, F., McBride, W. R., Ferayorni, A., Gregory, B. S., Hegwer, S. L., Tritschler, A., and Uitenbroek, H., “The Visible Broadband Imager: The Sun at High Spatial and Temporal
Resolutionʺ, The Second ATST‐EAST Meeting: Magnetic Fields from the Photosphere to the Corona,
ASP Conf Ser 463: 431, 12/2012.
49. Zhang, M., “Helicity transport from solar convection zone to interplanetary spaceʺ, Solar and
Astrophysical Dynamos and Magnetic Activity, IAUS 294: 505, 07/2013.
50. Zolotova, N. V., and Ponyavin, D. I., “Model of poleward magnetic field streams from
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sunspot butterfliesʺ, Solar and Astrophysical Dynamos and Magnetic Activity, IAUS 294: 87,
07/2013.
51. Zuccarello, F., Berrilli, F., Criscuoli, S., Del Moro, D., Ermolli, I., Giannattasio, F., Giorgi, F.,
Romano, P., and Viticchié, B., “Spectro‐polarimetric Observations of Moving Magnetic
Features around a Poreʺ, The Second ATST‐EAST Meeting: Magnetic Fields from the Photosphere
to the Corona, ASP Conf Ser 463: 51, 12/2012.
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APPENDIX E: MILESTONES FY 2014 This section describes the major project milestones for 2014.
E1. Advanced Technology Solar Telescope
Utility Building Beneficial Occupancy Date
Lower Enclosure Ready for Enclosure Installation
S&O Building Steel Erection Starts
ATST Telescope Pier complete
TMA Factory Acceptance Testing; ship to Hawaii
Enclosure Factory Acceptance Testing; ship to Hawaii
M1 Final Blank Acceptance; begin polishing
M10 DMS Factory Acceptance Testing complete
First engineering relocation to Hawaii
VBI Red Fabrication Complete
Engineering/Facility Camera Procurement and Testing
Mini‐DHS procurement and delivery to Instrument Development Teams
System Reviews
o High Level Software Systems FDR
o Cryo‐NIRSP CDR
o DL‐NIRSP CDR
o VTF PDR
o PA&C FDR
o WFC FDR
E2. Solar Adaptive Optics
Develop Solar Limb AO system that can lock on prominence structure. Graduate Student
Thesis Project.
Install optical test bench at Sac Peak optics lab. System tests
Perform on‐sky tests with Limb‐AO at DST.
Conclude integration and testing of MCAO at GREGOR and BBSO.
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E3. Diffraction‐Limited Spectro‐Polarimeter On‐Line Data Reduction
Current demand for this instrument is low because of its location on a separate optical
port, preventing it to be combined with other instruments, and duplication of its
capabilities in space (Hinode).
Maintain instrument and make available as user instrument on demand.
E4. NISP/SOLIS
Complete assembly and install visible, tunable filter for FDP.
Develop technique for flat fielding FDP data.
Complete full implementation of VSM guider.
Continue to provide VSM, ISS and FDP data online to the solar community and make
comparisons with data products from other instruments. Complete transition to VFISV
inversion for VSM 6302 vector data.
Support joint observing programs such as the IRIS mission, sounding rocket launches, and
queue observing mode at the DST.
Investigate usability of chromospheric synoptic maps as a source field for coronal
field/interplanetary field extrapolation and solar wind studies.
Complete cross‐calibration of ISS and Sac Peak K‐monitor data, successfully merge ISS and
K‐line monitor, and implement ISS K‐line data as the prime source to continue NSO historic
K‐line dataset.
Develop new data products for all three SOLIS instruments. Incorporate active region fields
from vector observations to traditional (line‐of‐sight) synoptic maps.
Develop and install new VSM 8542 modulator to obtain chromospheric vector magnetic
field observations.
Install new optical components in VSM calibration assembly to enable full polarimetric
calibration in the chromospheric lines.
Develop cost estimates and plan for future relocation of SOLIS instrumentation.
Develop plan for transition of NISP staff and resources into restructured NSO organization,
i.e. pooled data center and engineering groups.
E5. NISP/GONG
Install new data acquisition systems at remote network sites.
Assemble and test spare boards (motor amplifier, command, resolver, signal conditioner
and tachometer compensation) to expand long‐term maintenance inventory.
Operate the Learmonth site with expanded network bandwidth to accommodate near‐real‐
time data transfer.
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Replace existing turret entrance windows with units having superior coating properties.
Develop full automation of GONG network P‐angle registration software (COPIPE), to
include improved drift scan processing and quality assurance monitoring.
Improve near‐real‐time full disk calibrations to approach quality requirements for global
and local helioseismology products.
Add quality control parameters, daily and synoptic flow maps to Ring pipeline code.
Add error estimations to level‐3 synoptic products (both GONG and SOLIS).
Investigate the usability of GONG white light data for determination of classic proxies such
as sunspot number and sunspot area.
E6. Virtual Solar Observatory (VSO)
Add 6‐12 new data providers and data sets.
Develop spatial search capability.
Develop comprehensive reporting across all data providers.
E7. NSO Array Camera (NAC)
Sunspot and quiet Sun spectro‐polarimetric observations at 4132nm in preparation for
BBSO/Cyra and ATST.
Spectropolarimetric observations of 1565nm in sunspots.
E8. Spectropolarimeter for Infrared and Optical Regions (SPINOR)
Maintain instrument and keep available as user instrument.
Replace failed computer hardware.
Keep instrument available to perform telescope polarization matrix measurements.
Make instrument available in multi‐instrument configuration.
Provide software for data reduction by user.
E9. Facility IR Spectropolarimeter (FIRS)
Maintain instrument and keep available as user instrument.
Upgrade AD framegrabber boards for higher throughput. These framegrabber boards
should provide for higher frame rates and more flexibility on how the infrared camera can
be used.
Provide software for data reduction by user.
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E10. Dunn Solar Telescope Control and Critical Hardware (Systems Upgrade)
Continue efforts to proactively upgrade telescope and other critical hardware systems to
the extent possible given financial and personnel constraints.
E11. Rapid Oscillations in the Solar Atmosphere (ROSA) Imaging System.
Maintain instrument and keep available as user instrument.
Work on streamlining data collection to DST SAN, or other storage media.
E12. Interferometric Bidimensional Spectrometer (IBIS) Camera Upgrade
Maintain instrument and keep available as user instrument.
Provide software for data reduction by user.
E13. Service‐Mode Operations at the Dunn Solar Telescope
Evaluate cycle 1 & 2 service‐mode campaigns.
Conduct at least one, perhaps two, further experiments in 2014.
Use gathered information to set up new specifications and fine‐tune already existing
specifications for ATST operations planning.
E14. Establish NSO Headquarters
Finalize the third floor of the Space Sciences building at the CU east campus. Negotiate the
Lease for the HQ in Boulder with CU.
Initiate plans for fast‐track design and renovation of the third floor space with the goal of
completing renovations by March 2015.
Establish a complete relocation plan of NSO to the new Boulder/Maui sites and make it
available to the staff via the Observatory’s intranet.
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Pier mat slab concrete finishing work, Sept 2013.
APPENDIX F: STATUS OF FY 2013 MILESTONES This section describes the progress of current projects relative to the milestones established in the
FY 2013 Program Plan. (FY 2013 milestones appear in italics below.)
F1.AdvancedTechnologySolarTelescope
Initiate and manage site work on Haleakalā
The initiation is complete and the management is ongoing.
Site: Preparation, grading, trenching, utility corridor, environmental mitigations, foundations
for utility building, lower enclosure.
Complete. The early off‐site work was completed in
December 2012 – January 2013 (removal of the Reber
circle foundations, removal of overhead powerlines,
installation of the improved power corridor for HO);
environmental mitigations have been underway
(census of burrows, predator control including
trapping and removing known predators, monitoring
and removal of invasive species, assessment and
documentation of historic properties associated with
State Road 378, documentation of historic features
within the Park Road Corridor and start of construction on the ungulate fencing around the
boundary of petrel burrows) – along with the early site preparation. As of the end of FY 2013,
the ATST Utility Building is completing its steel erection and cladding and is scheduled for its
Beneficial Occupancy Date in December 2013. The Support and Operations Building
foundations for the telescope facility have been formed and the telescope pier walls were
poured in November 2013.
Conduct a ground‐breaking ceremony
Complete. A modest ceremony was held on November 30, 2012.
Manage vendor construction contracts for the major sub‐assemblies (M1 blank, enclosure, telescope
mount assembly, M1 assembly, etc.).
TMA Final Design Review (Dec 2012)
Complete.
Delivery of Telescope Control System (Mar 2013)
Complete.
Enclosure Fabrication, Factory Acceptance (2013)
Not yet complete (see photo). The Factory acceptance is
scheduled for December 2013.
FAA Tower Modification Completed (Jul 2012)
Complete.
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Final M1 Blank Ceramization Complete (Aug 2013)
Complete.
PA&C Preliminary Design Review (Feb 2013)
Incomplete; the procurement of the polarization optics was found to challenge both
budget and manufacturing capabilities. A redesign in collaboration with the instrument
partners is underway. In addition, there were some staffing issues within the instrument
team (staff transfer, new hire, relocation to Boulder) which are being resolved. This
milestone has been pushed into 2014 (with no impact on the project end date).
Instrument Control System Release (Jun 2013)
Incomplete. A systems review of the top level requirements and their flow down to the
control software resulted in significant clarifications on the interaction between the high
level software control systems. The re‐work is underway (working closely with the VBI
instrument team) to both meet the specifications and to ensure integration with
instrument needs.
Coudé Lab Procurements
Ongoing.
FTS Component Fabrication and Shipment to HI (2013)
Partially complete. The critical path items (Air Handling Units) have been fabricated and
shipped. Remaining components are on schedule.
ViSP Contract Award (Nov 2012)
Complete.
VTF Preliminary Design Review (July 2013)
Delayed into FY 2014 (with no impact on the project schedule).
F2.SolarAdaptiveOptics
Hire MCAO Research Assistant.
Complete. Dr. Dirk Schmidt has been hired as Postdoctoral Research Associate. Dr. Schmidt is
collaborating closely with the BBSO and Kiepenheuer Institute MCAO efforts and spends
significant time at those observatories to lead MCAO development and testing.
Install Kiepenheuer Institute MCAO software at Big Bear Solar Observatory (BBSO).
Complete. The Kiepenheuer Adaptive Optics System (KAOS) software has been installed at
BBSO during FY12 and has been successfully tested at the 1.6m telescope.
Test and modify MCAO software as needed for BBSO hardware.
Complete. The KAOS system has been successfully interfaced to the BBSO 357 actuator
XINETICS DM systems. The loop was closed on‐sky with the conventional AO308 system at
the 1.6m NST at BBSO.
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On‐sky MCAO testing at GREGOR telescope on Tenerife.
Delayed. Due to delays with the final commissioning of the 1.5m GREGOR telescope the
MCAO integration and testing phase of the GREGOR MCAO has been post‐poned until Nov.‐
Dec. 2013. Preparation for this campaign is in progress.
F3. Diffraction‐Limited Spectro‐Polarimeter On‐Line Data Reduction
Maintain the instrument as a well‐supported user instrument, as well maintaining it as quickly
available instrument to profit from excellent seeing conditions in DST queue observing mode.
If community interest is significant provide reduced data of sets with excellent seeing.
The DLSP is the prime instrument for telescope polarization calibration measurements on the Dunn
Solar Telescope Port 2. Maintain the procedures to perform these measurements and compare with
measurements on Port 4 with SPINOR.
Measurements to compare telescope polarization calibration parameters between the DLSP
and SPINOR have been obtained. There is no driver nor resources to work on the on‐line data
reduction for the DLSP.
F4. NISP/SOLIS
Continue to observe daily (synoptic and user‐requested data) and supply research‐grade data to the
community.
Complete. SOLIS takes daily synoptic observations and runs special observations for user‐
submitted observing proposals. Additional data were taken in support specific missions
(SUNSRISE flight, sounding rockets launches, co‐observing with IRIS etc).
Extend improvements of ISS data reduction to include additional spectral ranges requested by outside
users.
On‐going, partially complete. Due to higher priority tasks, work on these ISS improvements
was delayed. The improvements were made for K and H lines, and new code for H‐alpha was
recently implemented to the pipeline. Ca I 854.2nm was identified as the next priority for this
task. Improvements for remaining wavelength bands will be made later based on priorities
within SOLIS project.
Implement extinction monitor to improve ISS data.
Tests conducted with the extinction monitor and with taking data with different exposures
indicated that while using existing monitor to control exposure time complicates the
observations, it does not result in significant improvement to the quality of data. This talk was
given a low priority and put on hold until other aspects of the data reduction are improved to
justify this additional change.
Develop new data products for synoptic maps. Incorporate active region fields from vector
observations to traditional (line‐of‐sight) synoptic maps. Investigate a usability of vector field area
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scans of solar polar regions for pole‐filing in synoptic maps. Add error estimates to magnetic synoptic
maps.
Complete and on‐going. Three new data products were developed: synoptic vector magnetic
field maps, synoptic error maps, and maps of field strength derived from SOLIS VSM line
profiles by directly measuring the Zeeman splitting. All three data products are awaiting the
final implementation in the SOLIS production pipeline. Sample data products produced in
the process of their development are provided to the community (e.g., vector field synoptic
maps are provided to ARFL ADAPT developers and also are available on‐line). Additional
data product – geometry corrected full spectra in 6302v – is produced on a weekly basis due to
current disk limitations. These new spectral cubes provide one‐to‐one correspondence with fill
disk SOLIS magnetograms (i.e., for each pixel of inverted magnetograms, there are
corresponding spectra). Due to change in priorities, area scans of polar regions were taken in
Ca I 854.2 nm (to monitor polar field reversals), instead of vector ‐ Fe I 630.2 nm. Incorporation
of active region fields from vector to traditional (LOS) synoptic maps will be explored next.
Continue to provide VSM vector data online to the solar community and make comparisons with data
products from other instruments while evaluating alternative inversion techniques.
Nearly complete. Transition to VFISV inversion is nearly completed. The code is fully adopted
to SOLIS/VSM 630.2v data and is in the process of being implemented to the pipeline. The
final switch to new inversion depends on other improvements to the data (e.g., fringe
removal, stage 2 clean‐up etc); these improvements are now completed and tested.
Conduct comparative studies of SOLIS/VSM measurements of chromospheric fields with other
instruments (e.g., SPINOR).
Complete. Comparative studies have been performed between IBIS at the DST and
SOLIS/VSM. Results are excellent. Additional comparisons between the DST SPINOR and
SOLIS/VSM were not conducted due to weather and DST scheduling conflicts.
Improve systematic (automatic or semi‐automatic) approach for monitoring the quality of SOLIS
data.
Complete and on‐going. Several approaches were implemented, e.g., cloud transparency code
to monitor quality of VSM data, ISS line position warning system etc. Additional approaches
are under investigation.
Unify the production of SOLIS and GONG synoptic maps via a common pipeline code by early
FY13.
Complete. New synoptic maps are now publically available.
Develop technique for properly flat fielding FDP data. Develop necessary web interface for accessing
FDP data, and conduct comparative studies of SOLIS/FDP images with data products from other
instruments (e.g., ISOON).
Currently, on‐hold. Several approaches to flatfielding were investigated. Currently, this task
was put on hold awaiting a completion of the final tunable filter for FDP.
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Continue collecting data sets to work on isolating changes in the vector photospheric field parameters
before and after flare events as observed in the fast‐scan observations.
Complete. Additional observations (area scans) of flare events were acquired. Case studies of
changes in magnetic field associated with flares were conducted.
Integrate VSM vector photospheric and space borne coronal data (STEREO, SDO/AIA, Hinode) to
calculate and compare energy budgets for coronal fields and CMEs.
Complete, on‐going. An exploratory work on computing the magnetic energy of coronal fields
was conducted in collaboration with domestic and international partners. The results are
presented in conference presentations and peer‐reviewed papers. The adaptation of code to
perform NLFFF extrapolation and computation of magnetic energy is under investigation at
NISP/Atmospheric Section. Depending on the results of this early investigation, the decision
on NSO implementation will be made later.
Improve approach for producing helicity maps based on VSM vector magnetograms.
Complete, on‐going. Current helicity density will be computed as part of vector synoptic
maps production. In addition, a new improved azimuth dis‐ambiguation was implemented to
the pipeline, which is necessary step for routine computation of helicity maps.
Investigate usability of chromospheric synoptic maps as a source field for coronal field/interplanetary
field extrapolation and solar wind studies.
On‐going. Due to higher priority talks, the progress on this task is incremental. A low‐level
research effort continues to investigate this question.
Re‐design VSM calibration assembly to enable full polarimetric calibration in the chromospheric
lines.
Complete. Design is complete and vendors have been contacted for bids on optical
components.
Install VSM guider.
Complete. VSM guider was installed during the first week of June, 2013. Software and
hardware interface testing is in progress. Guider functions will be implemented in phases to
reduce risk to delicate optical components. Full guider implementation is expected within first
half of FY14.
Estimate impact on observing program to implement a new modulator for obtaining chromospheric
vector data.
Complete, on‐going. Tests were conducted toevaluate the impact of replacing 6302l modulator
by new 8542v modulator. The results are very encouraging. Additional tests have been
conducted.
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F5. NISP/GONG
Complete new data acquisition system and deploy at remote network sites.
System design and fabrication complete. Installation and testing at the Tucson site is in
progress. First GONG network site to be upgraded will be in November 2013.
Improve servo control of turret to minimize intermittent oscillations.
Problem with turret oscillations has been isolated to two of the six existing GONG sites.
Studies have found that existing threshold parameters for switching from ephemeris to guider
during morning sun acquisition are fine‐tuned for each site. Work is in progress to adjust
threshold values in order to mitigate effects on the guider servo during seasonal changes in
light levels.
Renew Tucson site lease and expand network bandwidth to allow transfer of data in near‐real time.
Complete. Second year of two year renewable lease contract with U of A will start on October
1, 2013. Contract with Megapath has been cancelled and new three year contract signed with
Login for expanded network bandwidth.
Expand network bandwidth at LE site to accommodate near real time data transfer.
In April 2013 installation of expanded network hardware was completed, however an existing
Cisco 2911 router needed replacement. By September 2013 all hardware problems had been
resolved and required configuration changes are currently in progress. Funding for increase
cost of expanded bandwidth allocated in FY14 NISP budget.
Engineer a cost effective coating replacement for the turret entrance windows.
Complete. New coating design approved and new entrance windows are on order. Cost has
been reduced by approximately 65% over original design. Delivery is expected by December
2013 with installation starting with scheduled preventative maintenance trips.
F6. Virtual Solar Observatory
Add 6‐12 new data providers and data sets
Ongoing – This year so far, the VSO has added ChroTel from the Kiepenheuer Institute in
Gemrnay, CLIMSO from Pic‐Du‐Midi Observatory in France, and PROBA2/SWAP from the
Royal Observatory in Belgium. The project is currently working on SDO/HMI, CORONOS,
NSO/ISOON, PSPT, TIMED/SEE, IRIS.
Develop spatial search capability.
Use cases and algorithm development underway. Poster (#100.138) presented at the AAS/SPD
Bozeman 2013 meeting.
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F7. NSO Array Camera (NAC)
Install 4 micron polarimetery optics and take first science data with NAC.
Science observations with 4132nm spectro‐polarimetry have been done. We have observed
using the BBSO/Cyra polarization optics, and have seen large splitting in atomic lines in
sunspots, and anomolous Zeeman patterns in molecular lines.
Implement regular 1.6 micron sunspot observations and produce vector magnetograms using modern
spectro‐polarimetric inversion software.
The 1565nm spectro‐polarimetric observations have been made, but a standard data reduction
routine has not been applied to these data.
F8. Spectropolarimeter for Infrared and Optical Regions (SPINOR)
Maintain as a well‐supported user instrument.
SPINOR is operational and available as user instrument
Test possibility to move the SPINOR modulator further downstream in the light path, so that the
instrument can share the light path with other instruments at port 4.
Test has been performed and it has been determined that the SPINOR modulator can be
placed further downstream, just in front of the slit, without detrimental effects on the
observational quality of the data. The use of SPINOR with other instruments on port 4 has also
been tested and there is considerable interest in using SPINOR with other port 4
instrumentation by investigators.
Because of its broad wavelength range, SPINOR is the primary instrument for telescope polarization
calibration measurements on Port 4. Develop and implement user‐friendly software package to
reduce data and calibrate polarimetry.
DST support scientist Christian Beck has taken over the telescope matrix support and
successfully maintains the reduction package.
F9. Facility IR Spectropolarimeter (FIRS)
Maintain as a well‐supported user instrument.
FIRS is operational and available for users
Add Ca II 854.2 nm line as option on the IR arm of the instrument.
No resources have been available for this addition
Replace the aging control computer of the IR arm “coconut” with new hardware for higher
throughput and improved reliability.
New faster computer hardware has been purchased, configured and installed. As a result
throughput has significantly improved.
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F10. Dunn Solar Telescope Control and Critical Hardware (Systems Upgrade)
Gradually replace critical hardware with newer equipment. In the servos for the guider mechanism
need to be replaced.
Keep working on understanding the Instrument Control Computer (ICC) software, and take out
superfluous parts that address operation of outdated telescope mechanisms and instruments.
Continue work towards an upgrade of telescope control system.
Continue work on current control system software to remove redundant source code and code for
instrumentation that is no longer in use in order to better support the transition from the current
system to new systems as they are deployed.
We are now in a good situation with the turret servos with the recent purchase of a spare.
Considerable work in replacing aging/failing computer systems have been taking up much of
our time. Most UNIX based camera control computers have been replaced and we are
currently occupied with replacing the UNIX servers on the observing table as well as most of
the Windows based “virtual camera computers”, most of which are being upgraded to
Windows 7 as part of the process.
We lost the programmer who had been working on the ICC software early in CY2013 and we
will not be able to refill this position. ICC support duties will be spread over the rest of the
software support personel to the extent possible. Before the ICC support programmer left, he
had made considerable progress with the code and we are now able to tweek the operational
code to both support observations and mechanism transition efforts.
F11. Rapid Oscillations in the Solar Atmosphere (ROSA) Imaging System
Make sure that DST operators keep up to speed in operation of ROSA. Investigate path to integrate
data collection into the DST Storage Area Network (SAN).
DST operators are comfortable with operation of the ROSA instrument. This also holds for the
two new faster and mor blue‐sensitive cameras, respectivey, that have been added, including
their new control computers. Work on stream lining data collection continues, but depends on
the efforts of our collaborators at Queens University, Belfast.
F12. Interferometric Bidimensional Spectrometer (IBIS) Camera Upgrade.
Make sure camera upgrade provides high frame rate capabilities. Integrate quick‐look data stream
with control software at the bridge.
IBIS performs at higher frame rates now. There is now also a quick‐look capability available
on the bridge that is being used by the observing staff and investigators for quality assurance.
F13. Dunn Solar Telescope Service Mode Operations
Two DST service mode experiments were conducted in January/February, and October
2013, for one month each. Both were successful in terms of operational lessons learned
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as well as in terms of community interest in submitting proposals—an indication of the
significant interest of the solar community to prepare for ATST style operations.
F14. Establish NSO Headquarters
Establish NSO transition teams for formulating relocating plans to new site and plans for new
Cooperative Agreement with NSF.
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APPENDIX G: NSO FY 2014 STAFFING SUMMARY
*Includesopenpositionscurrentlybeingadvertised
Director's Office
Sunspot Tucson ATST* NISP* Total
Scientists 1.00 7.00 3.00 3.00 11.00 25.00
Engineering/Science Support Staff - 8.00 1.00 31.00 17.50 57.50
Administrative Staff 1.50 5.20 9.80 2.00 18.50
Technical Staff - 7.49 6.00 7.35 20.84
Maintenance & Service Staff - 4.00 - 4.00
2.50 31.69 4.00 49.80 37.85 125.84
AF Supported Science Staff - 2.00 - - 2.00
AF Supported Technical Staff - 1.00 1.00 - - 2.00
Other NSF Projects (AO, FTS/CHEM) - - - - 0.00
Graduate Students - 1.00 1.00 - - 2.00
NASA Supported Science Staff - - 3.00 3.00
NASA Support Engineering Staff - - - 0.50
NASA Supported Technical Staff - - - -
Emeritus Science Staff - 0.50 1.00 - - 1.50
Visiting Scientists - - - -
0.00 4.50 3.00 0.00 3.50 11.00
2.50 36.19 7.00 49.80 41.35 136.84
Total Base Program
Total Other Support
Total Working at NSO
(In Full-Time Equivalents)
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APPENDIX H: SCIENTIFIC STAFF RESEARCH AND SERVICE
(*Grant‐supported staff) Christian Beck, Assistant Scientist
Areas of Interest
Post‐focus instrumentation; data reduction pipelines; high‐resolution spectroscopy and spectro‐
polarimetry of the photosphere and chromosphere; development of inversion tools for
spectroscopy of chromospheric spectral lines.
Recent Research Results
Dr. Beck completed the development of an inversion code for intensity spectra of the
chromospheric Ca II H line at the end of CY 2012. The code and its application to data obtained in
the magnetically quiet Sun are described in two publications in Astronomy and Astrophysics,
yielding a direct measurement of the energy content of acoustic shocks. The results were also used
to investigate the specific contributions to the widely used broadband Ca II H filter on board
Hinode, showing that a significant fraction of the observed intensity off the solar limb does not
come from Ca II H, but from the line blend of H‐epsilon instead.
A second line of investigation was a comparison between numerical simulations of the solar
photosphere and observations in several spectral lines at different spatial resolution to investigate
whether the simulation reproduces observed thermodynamical properties of the photosphere (also
published in A&A). Also shown is a suitable method to determine the spatial point spread
function of observations post‐facto from a comparison of the data to the simulations.
Future Research Plans
The inversion code mentioned above has now been modified for an application to spectra of the
chromospheric Ca II IR line at 854 nm taken at the Dunn Solar Telescope. A preliminary
investigation of data taken in 2013 showed several cases of short loops in the canopy of a sunspot
that returned to the photosphere instead of continuing upwards into the super‐penumbra as it is
commonly assumed. A publication on this is currently in preparation in collaboration with D.
Prasad Choudhary (California State U., Northridge). Observations with a combination of the
instruments, SPINOR and IBIS, are planned for 2014 to obtain simultaneous data in the Ca II lines,
H‐alpha, and Helium 1083 nm as an extension of the study.
Service
Beck completed data pipelines for the reduction of data taken with either the SPINOR or FIRS
instrument at the Dunn Solar Telescope. The software packages, with an instruction manual, are
available for any user of these instrumentsl. Beck is a member of the Sac Peak telescope allocation
committee and has participated in the planning and implementation of the service‐mode
experiment at the DST.
Thomas Berger, Associate Scientist
Areas of Interest
High resolution imaging of the solar atmosphere; birefringent optical instrumentation (Lyot and
Solc filters, waveplates); spectropolarimetry of solar plasmas; plasma dynamics including partial
ionization effects; solar prominence structure and dynamics and their relation to space weather
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phenomena; small‐scale magnetic field structure and radiance; solar telescope operations and data
center software design.
Recent Research Results
Dr. Berger is the Advanced Technology Solar Telescope Project Scientist, leading the definition of
the Critical Science Plan for the telescope in collaboration with the Science Working Group,
working to ensure telescope and instrument scientific integrity during design review processes,
and developing operations and data center concepts to ensure high scientific productivity during
commissioning and operations.
T. Bergerʹs scientific research focuses on the structure and dynamics of solar prominences, with
emphasis on analysis of high‐resolution movies. Using the Hinode/SOT instrument, he discovered
the magnetic Rayleigh‐Taylor instability in solar prominences, the first observed instance of this
important plasma instability in the outer solar atmosphere. Berger recently gave an invited talk on
prominence dynamics at the IAU Symposium 300 on Prominences and their Role in Space Weather in
June 2013 in Paris. He is currently working on two papers related to the Rayleigh‐Taylor instability
in prominences, collaborating with researchers from Kyoto University and Stanford University.
Future Research Plans
T. Berger plans to analyze additional data on prominence instabilities from the SDO/AIA satellite,
concentrating on measuring the thermodynamic characteristics of the plasma via Differential
Emission Measure (DEM) techniques. This research will be extended to studies of the relation of
prominences to coronal cavities and the search for mass and momentum transfers between these
structures. He will also continue research into optimal telescope operations strategies, working
with other solar as well as night‐time telescope operators to optimize ATST operations software
requirements.
Service
T. Berger is a member of the AAS Solar Physics Division committee and chair of the Public Policy
subcommittee. He has participated in three visit days to various agency and congressional staff in
the past two years, working to make the science of solar and space physics valued and understood
by key policy makers in Washington, DC. He has organized and/or chaired several recent
meetings or sessions including the July 2013 ATST/EAST meeting in Oslo, Norway, and the special
ATST session at the annual SPD meeting in Bozeman, Montana. He coordinates the annual
meetings of the ATST Science Working Group and the irregular meetings of sub‐working groups
to the SWG. During the summer of 2013, he supervised a graduate student in research on solar
prominence plasma characteristics using SDO/AIA and Hinode/SOT data.
Luca Bertello, Associate Scientist
Areas of Interest
Solar variability and heliospheric physics, with emphasis on the investigation of physical processes
leading to the different aspects of solar variability and on the calibration of observed solar
magnetic field to enhance the database that supports the analysis of conditions in the Sun’s corona
and heliosphere.
Recent Research Results and Plans for Future Research
Dr. Bertelloʹs most recent research focuses on four different areas: computation of magnetic flux
spatial variance synoptic charts; characterization of the weak magnetic field in vector
measurements; analysis of SOLIS ISS photospheric line parameters and their correlation to the total
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net solar magnetic flux; and investigation of the cyclic and long‐term variation of sunspot
magnetic fields. Some highlights follow.
In a recent paper submitted to Solar Physics, Bertello and collaborators at NSO have described a
technique to compute spatial variance maps of the solar surface magnetic flux density. These maps
can be used to estimate the uncertainty in the results of coronal models. They have tested this
approach by computing a potential‐field‐source‐surface model of the coronal field for a Monte
Carlo simulation of Carrington synoptic magnetic flux maps generated from the variance map.
They show that these uncertainties affect both the locations of the source‐surface neutral lines and
the distributions of coronal holes in the models.
Variations in the line depth and width of solar photospheric spectral lines with the Sunʹs cycle of
magnetic activity may have important implications for the study of the magnetism and dynamo
processes in other stars. Bertello and colleagues are using high‐spectral‐resolution observations
taken with the SOLIS/ISS instrument to investigate properties of several photospheric spectral lines
with different magnetic sensitivity. Preliminary results show that the line depth parameter of
some of those magnetic sensitive lines is well correlated with the total net magnetic flux during the
raising phase of solar cycle 24.
In collaboration with A. Pevtsov (NSO) and other co‐authors, a paper was submitted to Solar
Physics about the study of cyclic and long‐term variation of sunspot magnetic fields. Using 40
years of sunspot field strength measurements from Mt. Wilson, this study shows a solar cycle
variation of the peak field strengths with an amplitude of about 500‐700 Gauss, but no statistically
significant long‐term trends. The paper is currently in press.
Future Research Plans
The main focus of L. Bertello’s future research is on improving the quality of current SOLIS
longitudinal and vector magnetic field observations, and to enhance the capabilities of the SOLIS
ISS instrument.
Service
As a data scientist for SOLIS, Bertello’s major responsibility is to provide the solar and heliophysics
community with high‐quality and reliable data. During 2013, Bertello has participated in a NASA
review panel and has been a reviewer of publications for Solar Physics. As a former lecturer in
physics, Bertello still maintains a strong connection with former UCLA students by helping their
post‐college career with letters of recommendation.
*Olga Burtseva, Assistant Scientist
Areas of Interest
Flares; magnetic field; local helioseismology; solar activity.
Recent Research Results
Dr. Burtseva continues to study the evolution of magnetic field in flaring active regions. In order
to relate abrupt changes of the LOS magnetic field observed during strong flares to the
reconnection processes in the corona and investigate the origin of the magnetic field changes
during flares, comparison of the abrupt permanent field changes with location of the hard X‐ray
(HXR) flare footpoints obtained by the RHESSI instrument is being performed in collaboration
with J. C. Martinez‐Oliveros (UC‐Berkeley, SSL). The chromospheric HXR emission in solar flares
is generally regarded as the footprints of magnetic field lines newly reconnected in the corona.
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Also, the footpoint motions away from the neutral line are considered to be indicative of the
reconnection occurring in different heights of arcade magnetic fields with a displacement speed
proportional to the reconnection rate. First results of the comparison show good spatial and
temporal correlation of the HXR intensity with the magnitude of the magnetic field changes on
examples of three flares observed by GONG instruments.
In order to study the relationship between magnetic field changes and sunspot penumbral
structure, GONG continuum intensity during one of the flares―the X6.5 flare on December 6,
2006, observed as a white‐light flare―has been analyzed and compared with ISOON white light.
Disappearance of penumbral structure seen in white‐light and continuum intensity observations is consistent with past studies.
Future Research Plans
O. Burtseva plans to continue working on the evolution of magnetic field associated with solar
flares observed by GONG and HMI. She will also continue to test the current reconnection models
via the study of HXR, H‐alpha, magnetic and white‐light observations. She will resume her
analysis of temporal variations in the amplitudes and widths of high‐degree acoustic modes with
ring‐diagram technique using GONG, MDI and HMI data.
Serena Criscuoli, Assistant Scientist
Areas of Interest
High‐spatial resolution spectroscopy and spectropolarimetry of the photosphere and chromo‐
sphere; post‐focus instrumentation; radiative transfer; numerical simulations; solar irradiance
variations.
Recent Research Results
Dr. Criscuoli recently published two papers in the Astrophysical Journal. The first paper describes
how, through the analysis of IBIS/DST data, the properties of some iron lines can be employed to
investigate long‐term variations of properties (in particular temperature and magnetic flux) of
quiet Sun. The second paper investigates, through the analysis of magneto‐hydrodynamic simula‐
tions, the effects of the environmental magnetic flux on the physical properties of granulation and
small‐size magnetic features, and explains the physical processes that determine the differences of
physical properties of magnetic and convective structures observed in different regions of the solar
surface. Another paper has also been submitted to ApJ in which Criscuoli employs numerical
simulations to investigate the differences between the “real” photospheric temperature and the one
estimated through measurements of the radiative emission at some continua.
Through the analysis of magneto hydrodynamic simulations, Criscuoli also has been investigating
the effects of data quality and analysis techniques on the shape of the statistical distribution of the
magnetic field of photospheric bright points; a paper on that work has been submitted to
Astronomy and Astrophysics Letters. Another paper, submitted to A&A, investigates, through
comparison of results obtained from the analysis of HMI/SDO and MDI/SOHO data, the effects of
spatial resolution on the shape of the muli‐tfractal spectrum of active regions; this study is relevant
for the development of flare prediction techniques.
Future Research Plans
S. Criscuoli plans to employ magnetohydrodynamic simulations to investigate the observational
signatures of local dynamo and to explain the observed properties of quiet Sun. She also plans to
analyze data acquired during 2012‐2013 with the DST post‐focus instrumentation to investigate the
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contribution of small‐size magnetic features to total and spectral irradiance variations. She also
plans to investigate long‐term variations of properties of quiet sun through the analysis of
variations of properties of Fe I 6301 and 6302 nm lines observed with SOLIS.
Service
During summer 2013, S. Criscuoli mentored an REU and an SRA student. She also supervised a
student from University of Colorado in the framework of a collaboration with LASP. She is a
member of the Sac Peak telescope allocation committee and she has also contributed to the
planning and execution of the two 2013 Cycles of service‐mode observations at the DST. She is
also contributing to the development of software for FIRS and SPINOR data calibration.
David F. Elmore, Instrument Scientist
Areas of Interest
Development of ground‐based spectrograph and filter‐based polarimeters, including both current
instruments at NSO and new instruments for the Advanced Technology Solar Telescope.
Collaboration with NSO staff and visiting scientists to explore new spectropolar‐imetric
capabilities—spectral regions, processing techniques, and measurement calibration.
Recent Research Results
Elmore modeled the polarization properties of individual optical elements for solar research
telescopes and evaluated several techniques for inferring properties of these elements using
calibration and solar observational data.
Future Research Plans
Elmore will continue working with prospective instrument developers to define and develop
instrumentation for the ATST. He will apply his thorough understanding of telescope calibration
at the Dunn Solar Telescope toward development of the telescope calibration plan for the ATST.
He also plans to utilize existing instruments at NSO, such as SPINOR, ProMag, and IBIS, to
advance spectro‐polarimetric techniques.
Service
Elmore is Instrument Scientist for the ATST. In that role he works with instrument builders and
ATST team members to define the instruments and their interfaces. As ATST Instrument Scientist,
Elmore has created a Polarimetry Working Group that is addressing particular issues related to
calibration of the ATST.
James Lewis Fox, Postdoctoral Research Associate
Areas of Interest
Imaging spectroscopy and spectropolarimetry; prominences and filaments; instrumentation;
mathematical inverse theory.
Recent Research Results
Dr. Fox has completed a preliminary telescope polarization model at the Evans Solar Facility. The
model shows the redesigned ProMag instrument with modulation efficiencies that remain above
30% throughout the year. The model has been validated by calibration data taken from January
2013 to June 2013. This result was presented at the Solar Physics Division meeting in July 2013 in
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Bozeman, Montana. A more complete and detailed form has been prepared as a manuscript to be
published as NSO Technical Report ESF‐2013‐001.
Future Research Plans
J. L. Fox is working on removing a fringing pattern from ProMag images, and coaligning the dual‐
beam data to enable sensitive and precise full‐Stokes polarimetry with ProMag data. 175 GB of
data for 408 prominence maps exist for analysis once the data reduction pipeline is complete. He
will perform full Stokes vector inversions of these data (and future data) to obtain images of the 3D
magnetic field in prominences (via the Hanle effect), as well as inversions to obtain scattering
polarization analyses of non‐LTE physical processes in prominences and filaments. The ultimate
goal is to determine diagnostics that predict the onset of prominence activation and eruption for
space weather efforts. Data now exist for prominences before, during, and after an eruption. Fox
continues observing prominences with ProMag at the ESF in the He I lines at 5876 (D3) and 10830 Å.
Service
Fox has taken a leading role in operations at the ESF, somewhat analogous to the role of chief
observer (the ESF no longer has observers). He sees to maintenance and improvement of the
facility, benefiting operations for all ESF users. Fox mentored an REU student during summer
2013 through a successful project observing with ProMag. She obtained simultaneous data in He I
D3 and 10830 on post‐flare loops which are currently being analyzed. Fox is active in education
and public outreach activities, providing educational talks on solar astronomy and observatory
tours for groups of all ages, particularly for hundreds of elementary, middle, and high school
students from New Mexico and around the world. He has also given invited talks at public
astronomy events. He serves on the Sunspot Volunteer Fire Department.
Mark S. Giampapa, Astronomer
Areas of Interest
Solar and stellar magnetic activity; asteroseismology; exoplanet environments.
Recent Research Results
Dr. Giampapa and collaborators Vincenzo Andretta (INAF—Naples), Ansgar Reiners (U.
Göttingen), B. Beeck, and M. Schüssler (Max Planck) are analyzing spectra of the He I triplet lines
at 587.6 nm and 1083.0 nm, respectively, in a sample of G and F dwarf stars with detected coronal
X‐ray emission. The final results will be combined with models previously developed by Andretta
and Giampapa to estimate the area coverage of magnetic active regions on Sun‐like stars based on
these spectral features. This is the first important step toward establishing the empirical
relationship between rotation and the filling factor of magnetic active regions as a significant
constraint for stellar dynamo theory. Giampapa gave a preliminary report on findings at the 2012
Anchorage AAS SPD meeting. He and his colleagues are attempting to improve the terrestrial
water vapor correction for the 5876 line in particular. A paper for submission to The Astrophysical
Journal is planned for FY14.
Future Research Plans
Giampapa, in collaboration with M. Penn (NSO), plans to obtain IR spectra of solar plages in the 3–
4 micron region to measure both photospheric and chromospheric field strengths based on newly
discovered spectral features characterized by significantly higher magnetic sensitivity than
diagnostics in the visible. Along with Ca K spectra of the same plages, the empirical correlation
between chromospheric heating and chromospheric field strength will be investigated. Giampapa
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plans to use the SOLIS ISS for long‐term studies of the Sun‐as‐a‐star, specifically the variation of
line bisector amplitudes in photospheric features during the solar cycle. In collaboration with J.
Hall (Lowell Observatory), Giampapa is planning programs to investigate the magnetic activity of
solar‐type stars that are the hosts of systems with planets in the habitable zone. A proposal to
support this effort was submitted to the NASA Origins of Solar System Program.
Service
M. Giampapa is the Deputy Director for the National Solar Observatory. In this role, he assists the
NSO Director in the development of program plans and budgets, including budgetary decisions
and their implementation, and the preparation of Observatory reports and responses to NSF and
AURA oversight committee requests. He also attends and presents at AURA committee meetings
such as the Solar Observatory Council. Giampapa served as chair of the NSO Scientific Personnel
Committee until early FY 2014. He also carries out supervisory responsibilities for the NSO
Tucson/Kitt Peak program. In this role he has overview responsibilities for the scientific and
instrument development activities at the McMath‐Pierce jointly with McMP Telescope Scientist
Matt Penn. Giampapa is the chair of the NSO Kitt Peak telescope allocation committee and
program scientist for the McMath‐Pierce nighttime program. With Matt Penn, Giampapa is
working with a consortium for divestiture of the McMath‐Pierce by FY 2017. He represents the
NSO in discussions and negotiations with the NOAO, particularly with respect to staff support of
NSO/Kitt Peak operations. He recently completed his term as the Diversity Advocate for the NSO
but continues to work in support of the new NSO DA, John Liebacher. Giampapa is a member of
the Scientific Organizing Committee for the 18th Cambridge Workshop on Cool Stars, Stellar
Systems, and the Sun, to be held in Flagstaff, AZ in June 2014. Like other NSO scientific staff
members, Giampapa participates in educational outreach activities, including K‐12,
undergraduate, graduate, and general public educational programs and activities. Giampapa is an
adjunct astronomer at the University of Arizona.
Irene González Hernández, Associate Scientist
Areas of Interest
Local helioseismology (seismic imaging and ring‐diagram analysis).
Recent Research Results
Dr. González Hernández is currently leading the GONG far‐side project, aimed at calculating daily
far‐side maps of the Sun’s magnetic activity. Daily maps are shown on the GONG Web site
(http://gong.nso.edu/‐data/farside/). These maps are now calibrated into magnetic field strength
and include other features such as AR identification and detection confidence level that are useful
to space weather forecasters. A recent publication by Liewer et al., comparing the helioseismic
maps with direct observations from the STEREO spacecraft, shows the high reliability of the
GONG seismic far‐side maps. The same pipeline is now being used to calculate maps using the
Doppler‐grams from HMI.
The calibration of the far‐side maps into magnetic field strength means that these maps are now
valid input to models that need photospheric magnetic field information and opens the possibility
of many research collaborations; e.g., González Hernández is collaborating with AFOSR personnel
to add far‐side maps to the standard input of the ADAPT photospheric flux transport model. The
analysis of a particular case has shown a substantial improvement in F10 and solar wind
forecasting when using far‐side maps with ADAPT and ADAPT+WSA, respectively.
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González Hernández is also involved in the GONG Ring Diagrams pipeline. Currently, she is
applying the method to investigate the subsurface dynamics of Anti‐Joy active regions. She is also
involved in the analysis of large flows, in particular the profile of the meridional circulation at high
latitudes.
Future Research Plans
I. González Hernández and Manuel Diaz Alfaro (IAC) have worked on a new magnetic index
calculated by integrating helioseismic maps of the whole Sun. The contribution of far‐side
magnetic activity to the index can be calibrated in terms of standard front‐side indexes such as Ly‐
alpha and F10 indices. Once calibrated, the index can be used to forecast EUV and total solar
irradiance weeks in advance by using it as input to irradiance models such as the JB2008.
González Hernández plans to continue her work on the subsurface flows of Anti‐Joy active regions
to prove or disprove the relation between these peculiar active regions with large dynamics under
the solar photosphere.
Service
González Hernández is the NISP solar interior data scientist. In this role, she oversees the quality
of the GONG data, particularly the Dopplergrams, and assists with the distribution of customized
products to external users.
Sanjay Gosain, Postdoctoral Research Associate
Areas of Interest
Observations of solar flares, erupting filaments and CMEs; characterization of magnetic non‐
potentiality in solar active regions using vector magnetograms; high‐spatial resolution spectro‐
polarimetry of solar active regions; solar cycle related magnetic field variations using synoptic
magnetograms; instrumentation, specifically in areas of spectropolarimetry and development of
polarization calibration procedures.
Recent Research Results
Dr. Gosain has done a comparative study of helicity at different layers of the solar atmosphere.
Sunspots with twisted magnetic field configuration in the chromosphere and corona (seen as long‐
lived whirls in SDO AIA images) were chosen. The photospheric magnetic twist was determined
using SOLIS and HMI magnetograms, and the kinetic helicity of subsurface flows beneath these
active regions were deduced by using the ring diagram analysis technique on GONG observations.
An analysis of two cases has been carried out as a pilot study and published. An extension of this
analysis to much larger dataset is planned for deriving statistically significant results.
S. Gosain is also proposing a new idea for fast disambiguation of 180‐degree ambiguity in solar
magnetic fields. The idea is based on the assumption that most of the magnetic field on the Sun is
predominantly a vertical line in the plages and the network region. Analysis of inclination angle of
the magnetic field from SOLIS data reveals that about 65‐80% of the field on the Sun is close to
vertical with inclination angle between 0‐30 degrees. The magnetic field can thus be disambiguated
first with a simple approach that automatically chooses the most vertical configuration. The good
initial guess provided by this approach will help in expediting the iterative disambiguation
schemes like the NPFC method (Georgoulis, 2005), which is implemented in the SOLIS pipeline.
Gosain and colleagues analyzed the giant filament eruption event of 26 Sept 2010 observed by the
STEREO and TESIS satellites. The 3D reconstruction of the eruptive event was carried out using
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different methods, and the resulting height‐time profile of the rising filament were fitted with
different functional forms. Different models have been proposed for the solar eruptions based on
different physical mechanisms. These different models expect different profiles for acceleration of
the ejecta. It is found that for the eruptive event studied, the exponential form fits best with the
observations, i.e., better than the cubic or parabolic rise profile. The exponential rise profile is
expected for the eruptions due to ideal MHD instability, so the observations of Gosain et al.
support this model for the observed event.
Future Research Plans
S. Gosain will indulge in the analysis of the twist patterns in solar active region magnetic fields
during the ascending phase of solar cycle 24 (covering the most recent data for 2012) using SOLIS
full‐disk magnetograms and will combine the results with subsurface kinetic helicity patterns for
the same active regions to make a comprehensive study of temporal behaviour of helicity trends in
photospheric magnetism of active regions and plasma flows in their subsurface layers. The
synoptic maps of current helicity from the SOLIS VSM and synoptic maps of subsurface flows
from GONG observations will be used for these studies.
Analysis of flares, CMEs and eruptive events with SOLIS VSM data together with space‐based data
from SDO will be carried out for selected events. Gosain also plans to participate in the
development of a Stokes polarimeter for the Ca II 854.2 nm line, an upgrade planned for the
current SOLIS/VSM instrument.
Service
S. Gosain developed an IDL program to analyze the SOLIS polarimeter calibration data sequence
and fit the data to infer polarimeter response matrix and deduce the demoulation matrix. The final
cross‐talk in the Stokes parameters is estimated to be below a few (1‐2%) percent. Gosain also
developed a program to adapt the SOLIS Stokes data to be inverted by the Very Fast Inversion of
the Stokes Vector Milne‐Eddington (VFISV ME) inversion code used by the HMI pipeline. The
SOLIS data can now be inverted with the HMI code and the output can be fed to the SOLIS
pipeline for disambiguation. Detailed comparison with HMI full‐disk and Hinode SOT/SP vector
magnetograms is planned.
Brian J. Harker, Postdoctoral Research Associate
Areas of Interest
Stokes spectropolarimetry of the photosphere; Stokes inversion techniques; spectropolarimetric
data reduction; automated tracking and classification of sunspot and active region structure;
parallel processing techniques for data reduction.
Recent Research Results
Dr. Harker has developed a new active region identification code, based on Hermite function
decomposition of the Stokes Q, U, and V profiles, which relies on no user‐tuned parameters or
arbitrary thresholds on, for example, magnetic field strength or intensity. An Astrophysical Journal
Supplement Series paper on the method has been published. Harkerʹs new spectropolarimetric
fringe removal algorithms have been implemented in the SOLIS/VSM vector magnetic field
pipeline, along with a new Milne‐Eddington inversion engine (based on the VFISV code), which
provides truly full‐disc vector magnetic fields in a more stable, and much faster implementation
than that previously used. A paper comparing two “quick‐look” vector magnetic field calculation
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paradigms (in collaboration with V. Bommier of LESIA) has been submitted to the Astrophysical
Journal, in which the authors find that the new Inversion by Central Moments (ICM) method is
fast, accurate, needs no calibration, and is more applicable over a wide range of solar conditions
than a commonly used Integral method which relies on integrated Stokes profiles. Finally, Harker
has collaborated with A. Pevtsov (NSO) to study a patch of transient magnetic field (including a
polarity reversal) observed by SDO/HMI during the M7.9 flare of 13 March 2012. A short‐lived
patch of magnetic field at the umbra/penumbra boundary of NOAA 11429 was found to undergo a
rapid and reversible change in the magnetic field strength and orientation, and the authors
concluded (from the lack of flare‐related line emission and forward‐modeling experiments on
SDO/HMI instrumental/algorithmic characteristics) that the observed change was indeed a real
evolution of the magnetic field, indicating an abrupt rotation of the field vector. An ApJ paper on
these results has been accepted for publication.
Future Research Plans
B. Harker has begun an investigation into the inherent information content and optimal sampling
of Stokes profiles (in collaboration with J. C. del Toro Iniesta of the Instituto de Astrofísica de
Andalucía (IAA), M. Rempel (HAO) and H. Uitenbroek (NSO). The project involves Fourier
analysis of realistic synthetic Stokes profiles synthesized from the MHD simulations of Rempel
(2012), systematically degraded and noise‐corrupted to investigate the effects of sampling and
noise on the frequency content of Stokes profiles. This will be widely applicable to future
instrument design and operations.
Service
B. Harker mentored 2013 NSO REU student Tyler Sinotte (U. Wisconsin, Madison), whose project
was to search for flare‐related changes in Stokes V area and amplitude asymmetries, which might
indicate changes in the gradient(s) of magnetic field and/or velocity along the line‐of‐sight. Tyler
will be presenting his results at the January 2014 AAS meeting in Washington, DC.
John W. Harvey, Astronomer
Areas of Interest
Solar magnetic and velocity fields; helioseismology; instrumentation.
Recent Research Results
During FY 2013, Dr. Harvey worked on SOLIS and GONG instrument development and
maintenance. This work continues to consume nearly all available time so, as has unfortunately
been the case for many years, little research was done. The main research results include a pilot
study of the strength of umbral magnetic fields based on SOLIS VSM intensity spectra. Simple
fitting of a Zeeman triplet to spectra gives field strengths that match closely to the Livingston and
Penn measurements. A data reduction pipeline has been developed and large numbers of
measurements are now available for detailed analysis and a research paper. A large study of
chromospheric magnetic field measurements in a synoptic context with Chinese visitor Chunlan
Jin and former NSO staff member Anna Pietarila was published and showed slightly superior
coronal magnetic field extrapolations compared with photospheric‐based extrapolations. A study
of chromospheric circumfacules led by Pietarila was also published with the major result being
strong support for the hypothesis that shock waves are responsible for the enigmatic reverse shape
of the chromospheric 854.2 nm line of Ca II. Studies of simultaneous chromospheric observations
with the SOLIS VSM and the recently launched IRIS satellite were started. Another study just
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started aims to better understand the frequency and significance of apparent increases of field
strength with height in flares.
Future Research Plans
During FY 2014, J. Harvey will complete construction of the SOLIS FDP visible tunable filter, assist
with completion of the VSM guider, construct a new modulator for chromospheric vector field
measurements, continue to concentrate on improved reduction of SOLIS and GONG data, and
complete research started in 2013. Harvey hopes to be able to concentrate on research after
transition to halftime in 2014. He will prepare his invited memoirs for the journal Solar Physics.
Service
J. Harvey has responsible instrumental and scientific roles in the GONG and SOLIS projects. He
completed his service as a member of the NSO Scientific Personnel Committee in early FY 2014.
During FY 2013, he served on a National Research Council study on filling an impending gap in
solar irradiance measurements. He is a co‐investigator on the IRIS satellite project.
Frank Hill, Senior Scientist
Areas of Interest
Helioseismology; asteroseismology; fluid dynamics of the solar convection zone; the solar activity
cycle; virtual observatories; solar magnetic fields.
Recent Research Results
Dr. Hill continues to perform research in helioseismology. Working with R. Howe and others, Hill
has been tracking the progress of an east‐west zonal flow in the solar interior known as the
torsional oscillation as it slowly migrates from the solar poles to the equator. Recently, it was
found that the background high‐latitude solar differential rotation rate had changed in the rising
phase of cycle 24, masking poleward branch for cycle 25.
Working with S. Kholikov, J. Leibacher, and others, Hill has been developing ways to measure the
deep meridional flow using time‐distance analysis. Preliminary work suggests that there may be at
least two‐cells to the meridional flow as a function of depth. Recent numerical simulations from
the University of Colorado indicate that a multi‐cell meridional flow is consistent with the
observed surface differential rotation, whereas a unicellular flow is not.
Hill continues to work with K. Jain and S. Tripathy on the change of frequencies during the recent
deep minimum and the rise of cycle 24. Recent results show a quasi‐biennial periodicity that may
indicate the presence of a near‐surface dynamo.
Hill has been working with the SDO HMI team to develop their ring‐diagram analysis pipeline to
routinely map the flows in the outer solar convection zone. Hill and his team have been develop‐
ing helioseismology using the SDO Atmospheric Imaging Assembly data, which will provide a
multi‐wavelength capability when combined with HMI and GONG observations.
Future Research Plans
While much of his time is taken up with administrative matters, Hill has started a new research
project with graduate student Teresa Monsue and Drs. Keivan Stassun and Nathan De Lee
(Vanderbilt U.) to construct oscillation power map movies of H‐alpha intensity in flaring and non‐
flaring regions. These movies will show how waves in the chromosphere are affected by flares.
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Service
Hill is the NSO Associate Director for the NSO Integrated Synoptic Program (NISP), which
combines SOLIS and GONG. He continues to participate in the development of the Virtual Solar
Observatory, which was released to the public in December 2004. Hill typically supervises several
staff, currently eight scientists, one manager, and one programmer. He acquired funding from the
US Air Force Weather Agency (AFWA) in 2009 to develop and install an H‐alpha observing
capability in the GONG network. AFWA has subsequently provided operational support for
GONG in FY 2011 and FY 2012. Hill submits around four proposals a year for outside funding.
Hill reviewed ten proposals for the NSF and NASA, as well as five papers for ApJ, Solar Physics,
etc. He served on the scientific organizing committee for three international scientific meetings,
and has been appointed to the European HELAS Board. He is currently working on developing a
new network to obtain multi‐wavelength observations for helioseismology, solar magnetom‐etry,
and space weather.
*Kiran Jain, Associate Scientist
Areas of Interest
Global and local helioseismology – solar cycle variation; multi‐wavelength helioseismology; sub‐
surface flow dynamics; solar activity – irradiance modeling; Sun‐Earth connection.
Recent Research Results
Dr. Jain studied mode parameters using several observables from the SDO (HMI V, HMI Ic, HMI
Ld, HMI Lc, AIA 1600, AIA 1700) and GONG V using symmetric and asymmetric profile models.
Jain and colleagues found that the current model for asymmetry in power spectra is inappropriate
and does not represent the correct profile above the cut‐off frequencies. They suggest a need of re‐
visiting the model in order to study the characteristics of propagating acoustic waves in the solar
atmosphere. Halos in power maps around active regions for different observables were also
studied. It is found that the influence of the active region in power, phase and coherence extends
beyond the surface field concentrations in high frequency bands. Above the acoustic cut‐off
frequency, the behavior is more complicated: power in HMI IC is still suppressed in the presence
of surface magnetic fields, while power in HMI IL and the AIA bands is suppressed in areas of
surface field but enhanced in an extended area around the active region, and power in HMI V is
enhanced in a narrow zone around strong‐field concentra‐tions and suppressed in a wider
surrounding area. This is consistent with the idea of field lines spreading out with height and
affecting the waves through scattering and mode conversion.
Jain also applied the technique of ring‐diagrams to study the temporal variation of the horizontal
velocity in sub‐surface layers beneath AR 11158. This active region had several sunspots rotating
in different directions and also produced many flares, including an X2.2 flare, during its disk
passage. High‐resolution Doppler measurements from SDO/HMI were used, allowing the
investigation of the flow pattern in regions of negative and positive polarities separately. The
study demonstrates that the morphology of a sunspot plays an important role in governing flows
fields or vice versa.
Future Research Plans
Jain will continue to investigate the effect of the choice of observables on helioseismic mode
parameters and subsurface flows using simultaneous data sets. She and colleagues will carry out a
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detailed study of mode parameters obtained with different observables, quantify differences, and
interpret results in context of the formation height and the anticipated phase relationships between
the oscillations at those heights. In the next phase, the plan to determine mode parameters using
cross‐spectrum analysis.
Jain and collaborators will also continue to study the influence of magnetic activity on varying
oscillation frequencies, both locally and globally. They plan to investigate in detail the two‐year
periodicity in global shifts and to compare the frequency shifts during the ascending phase of the
current cycle 24 with the previous cycle.
Service
Jain serves as the science coordinator of the NSF funded International Research Experience for
Students (IRES) program for NSO and is the Program Scientist of the Interior Science Group of the
NSO Integrated Synoptic Program (NISP). In May 2013, she co‐chaired the 27th NSO workshop
entitled “Fifty Years of Seismology of the Sun and Stars” held in Tucson. She has also served as a
panelist in the NASA’s proposal review committee.
Stephen L. Keil, Astronomer
Areas of Interest
Solar activity and variability; astronomical instrumentation; solar convection and magnetism;
coronal waves; educational outreach; the Advanced Technology Solar Telescope.
Recent Research Results
S. Keil worked with REU student Tyler Behm on investigating methods of restoring missing data
in time series and measuring differential rotation in integrated sunlight as seen in the Ca II K‐line.
They also used the daily Ca II K‐line full‐disk spectroheliograms to track the latitudes of K‐line
emission regions from 1976‐2002 and showed they followed a “butterfly” diagram similar to
sunspots. They were able to show a clear signal of differential rotation for some solar cycles using
data from the Evans Solar Facility at Sacramento Peak. Other cycles, while showing some signal,
were more difficult to interpret due to the emergence and decay of active regions. Results were
presented at the AAS SPD meeting in July 2013 and incorporated into a paper. Keil also continued
to compare disk‐integrated Ca K‐line observations obtained from the Evans Solar Facility with
those of SOLIS in order to cross calibrate. Once the cross calibration is completed, the Evans
measurements will cease.
Future Research Plans
Keil plans to continue his work on solar magnetoconvection and waves. He plans to study the
association between MHD and acoustic waves and chromospheric and coronal heating. Keil will
continue investigating changes in chromospheric emissions through measurements of the Ca II K‐
line in both integrated flux and spatially resolved images. This work is part of a program to
understand variations of the solar ultraviolet and extreme ultraviolet flux as inputs to the
terrestrial atmosphere in collaboration with researchers at NASA Ames. Keil will continue to work
with HAO colleagues Steve Tomczyk and Scott McIntosh on coronal waves.
Service
Keil currently serves as advisor to the Director of the National Solar Observatory. He supervises
both graduate and undergraduate students, conducting research programs during the summer,
and works closely with NSO and NOAO educational outreach programs. He provides input to the
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current solar and space physics decadal survey on science objectives and the ATST project. Keil
serves as an advisor for the Akamai outreach program in Hawaiʻi. He presents the NSO program
to Akamai graduates and helps them develop their resumes.
Shukirjon S. Kholikov, Assistant Scientist
Areas of Interest
Helioseismology; data analysis techniques; time‐distance methods.
Recent Research Results
Shukur Kholikov works primarily on time‐distance applications using GONG++ data. He has
developed a time‐distance pipeline, which provides travel‐time maps of daily GONG‐network
data and produces reconstructed images with specified filters. At present, the pipeline has been
tested to produce several types of specific travel time measurements.
The main focus of the pipeline is deep meridional flow measurements. A recent approach in this
field is averaging huge amount of measurements over a long time period to obtain depth profile of
meridional flow. Meridional flow measurements were obtained by using GONG spherical
harmonic (SH) time series for 1995‐2011 using travel‐time differences from velocity images
reconstructed from SH coefficients after applying phase‐velocity and low‐filters. This filtering
technique increases the signal‐to‐noise ratio and thus extends travel‐time measurements to
relatively high latitudes and deep into the convection zone. The obtained depth profile shows a
distinct and significant change in the nature of the time differences at the bottom of the convection
zone. Development of an inversion procedure to extract equatorward components of the deep
meridional flow is in progress.
Another application of the existing time‐distance pipeline has been successfully tested to measure
acoustic travel time perturbations due to emerging active regions. It was shown that some selected
active regions can be predicted one‐to‐two days in prior than they appear at the solar surface.
Future Research Plans
Kholikov will continue to improve the time‐distance pipeline and provide the scientific community
with specific GONG data for local helioseismology analysis. The main focus will be deep
equatorward return flow measurements involving GONG, MDI and HMI data series.
Service
Kholikov is a member of the Kepler Asteroseismic Science Consortium working group. He also
provides time distance measurements and high degree SH time series of GONG data by request. *Rudolf W. Komm, Associate Scientist
Areas of Interest
Helioseismology; dynamics of the solar convection zone; solar activity and variability.
Recent Research Results
Komm continues to perform research in helioseismology. He is deriving solar sub‐surface fluid
dynamics descriptors from GONG data analyzed with a ring‐diagram. Using these descriptors, he
was able to derive, for example, the divergence and vorticity of solar sub‐surface flows and study
their relationship with magnetic activity. Komm is exploring the relationship between the twist of
subsurface flows and the flare production of active regions and started producing daily full‐disk
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maps of the normalized helicity parameter in collaboration with A. Reinard (NOAA/SWPC).
Komm is searching for a signature of helicity flow from the solar interior to the photosphere, in
collaboration with NSO colleagues S. Gosain and A. A. Pevtsov, and has derived the subsurface
helicity of active regions with superpenumbral whirls and the hemispheric helicity rule of
subsurface flows. Komm is studying the solar‐cycle variation of the zonal and the meridional flow
in the near‐surface layers of the solar convection zone, in collaboration with I. González
Hernández, F. Hill, and R. Howe.
Future Research Plans
Komm will continue to explore the dynamics of near‐surface layers and the interaction between
magnetic flux and flows derived from ring‐diagram data, and will focus on the relationship
between subsurface flow characteristics and flare activity in active regions. He will focus on the
daily variations of subsurface flows of active regions and search for a signature of helicity flow
from the solar interior to the photosphere. He will also continue to explore the long‐term variation
of subsurface flows.
Service
Komm continues as coordinator of the Local Helioseismolgy Comparison Group (LoHCo). He
supervises undergraduate and graduate students who participate in NSOʹs summer REU and SRA
programs. John W. Leibacher, Astronomer
Areas of Interest
Helioseismology; atmospheric dynamics; Asteroseismology.
Recent Research Results
Leibacher’s recent work has focused on the evolution of solar active regions as seen by GONG and
SDO/AIA, and the treatment of low‐degree spherical harmonic mode frequencies to better probe
the deep solar interior. In addition, work continues on various aspects of a new technique for
measuring solar subsurface meridional circulation and its variation with the solar cycle, several
solar and instrumental effects that manifest in the meridional circulation measurements (offset of
the solar rotation axis from the classic values and center‐to‐limb darkening shifting the effective
center of the velocity pixels), as well as the variation of the helioseismic signal with altitude in the
solar atmosphere and the inter‐comparison of measurements from different instruments and
different techniques.
Future Research Plans
Ideas about the observational signature of the convective excitation of p‐mode oscillations are
being pursued with data from GONG as well as instruments onboard the SOHO spacecraft with
collaborators at the Institut d’Astrophysique Spatiale (Orsay, France) and the Observatoire de
Paris–Meudon. The application of helioseismic techniques to stellar oscillations is being pursued
in the framework of the CoRoT and Kepler missions, and modifications to the SDO/HMI and AIA
frequency analysis are being pursued. The search for flare‐related changes in the solar interior as
manifested in helioseismic ʺring‐diagramsʺ, and application of gap‐filling strategies to helio‐ and
asteroseismic time series continues.
Service
Leibacher serves as editor of the NSO Newsletter, as Diversity Advocate and NSO member and
vice‐chair of the AURA Workforce Diversity Committee, as representative for outreach activities,
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and organizes the weekly seminar series. He served on the NSO Scientific Personnel Committee
until early FY 2014. Leibacher has been a mentor to several undergraduate (REU) students and
two graduate students using GONG data, has been the external examiner on six PhD theses and a
member of seven PhD juries recently. He maintains the SolarNews WWW site. He is a member of
the Fachbeirat (scientific advisory committee) of the Max‐Planck Society’s Institute for Solar
System Research (Katlenburg–Lindau), chair of the High Altitude Observatory/National Center for
Atmospheric Research External Advisory Committee, advisor to several external projects, and
member of the current NASA Heliophysics Roadmap committee. He is editor‐in‐chief of the
journal Solar Physics.
Valentín Martínez Pillet, NSO Director
Areas of Interest
Solar activity; Sun‐heliosphere connectivity; magnetic field measurements; spectroscopy; polari‐
metry; astronomical instrumentation with an emphasis on the Advanced Technology Solar Telescope.
Recent Research Results
Before joining NSO as Director, Dr. Martínez Pillet was leading the Imaging Magnetograph
eXperiment (IMaX) for the balloon borne SUNRISE solar telescope (a Germany, Spain and USA
collaboration). IMaX/SUNRISE has flown twice from the Artic circle within the Long‐Duration
Balloon program of NASA (June 2009 and June 2013). The data obtained during the first flight has
produced the most accurate description of the quiet Sun magnetic fields, reaching unprecedented
resolutions of 100 km at the solar surface and a sensitivity of a few Gauss. These data have
produced well over 30 papers in the last few years, describing a large variety of processes
including the discovery of small‐scale supersonic magnetized flows. These jets have been recently
identified in the Hinode satellite data that provide full Stokes spectral profiles and allow for a
detailed study of the atmospheric context in which they are generated. Using inversion
techniques, such a study is being performed in the context of the PhD of C. Quintero (IAC). It is
expected that the data from the second flight will produce results of a similar impact.
Dr. Pillet was also leading (as co‐Principal investigator) the design and construction of the
Polarimetric and Helioseismic Imager for the Solar Orbiter mission (a Germany, Spain and France
collaboration).
Future Research Plans
As Director, Dr. Pillet has overall responsibility for the operation of NSO and the effort to develop
the Advanced Technology Solar Telescope, to maintain and rejuvinate the NSO synoptic program,
and prepare for observatory operations at the new NSO directorate site in Boulder, Colorado. Dr.
Pillet plans to maintain an active role in the analysis of the data from the second IMaX/SUNRISE
flight. This flight received ground support from several of the NSO facilities including the SOLIS
VSM instrument. The full‐disk, vector magnetic capabilities of SOLIS nicely complement the high‐
resolution data from IMaX/SUNRISE during this second flight.
Dr. Pillet plans to establish collaborations with the NISP scientists on quantifying the flux history
of active regions with an emphasis on their decay phase.
Service
Dr. Pillet is Director of the National Solar Observatory. In the past, he has provided services for a
variety of international institutions, including: member of the High Altitude Observatory Science
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Advisory Board; member of the ATST Science Working Group; member of the European Space
Agency Solar System Working Group; former President of the International Astronomical Union
Commission 12 on Solar Radiation and Structure; former President of the International
Astronomical Union Division II The Sun and the Heliosphere; and member of the Editorial Board
of the journal Solar Physics.
Dr. Pillet has acted as PhD advisor of three students at the IAC (Tenerife) and of supervisor of
three post‐doctoral scientists from various international institutions.
Matthew J. Penn, Associate Astronomer
Areas of Interest
Spectropolarimetry; near‐IR instrumentation; solar atmosphere; oscillations and magnetic fields.
Recent Research Results
Most recently, Penn has obtained CO 4666 nm eclipse observations and is working on inverting the
data to study the emission with resolution equivalent to that expected from the ATST. Penn
continues to work with W. Livingston on examining the changes in sunspot magnetic fields
through solar cycle 24 and is relating the observed sunspot changes with data from 21 cm
emission; recent work was published in ApJ Letters (Livingston, Penn and Svalgaard, 2012). Penn
has studied solar oscillations using the 4‐micron fundamental lines of CO; results indicate that the
CO lines provide physical diagnostics of the solar atmosphere; recent work was published in ApJ
Letters (Penn, Schad and Cox, 2011).
Future Research Plans
Penn is currently involved in vector magnetic field observations using the 1083 nm and 1565 nm
infrared lines and with imaging and spectroscopy at wavelengths from 4000‐4700 nm.
Service
Penn is involved with the ATST development, particularly the IR and coronal instrumentation for
the ATST (Cryo‐NIRSP and NIRSP‐C) and with a group providing scientific feedback to the ATST
software development group.
As part of his work with the BBSO/NST/Cyra cooled spectrograph instrument, Penn has done
successful imaging and polarimetry experiments at 4700 nm, and new filters have been ordered
for more work in this area. Parts of a polarimeter to operate in the 3000‐5000 nm wavelength range
have been tested and the complete system identified and ordered in FY 2012.
Penn was advisor to graduate student Tom Schad from the UA on new vector magnetic field
measurements using the He 1083 nm spectral line, and inversion code (HAZEL) provided to the
international community by the IAC (Spanish) group; Schad received his PhD in August 2013.
Penn is advising postdoctoral research associate Fraser Watson, a recent graduate from the
University of Glasgow, with additional studies of the long‐term sunspot magnetic field evolution.
Penn is in charge of the NSO summer Research Experiences for Undergraduates (REU) and
Research Experiences for Teachers (RET) programs and works closely with the NSO staff to
maintain the high quality of the NSO REU/RET program.
Gordon J. D. Petrie, Associate Scientist
Areas of Interest
Solar Magnetic Fields
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Recent Research Results
Petrie investigated relationships between active and polar fields via high‐latitude poleward
streams using 40 years of NSO magnetograms. In this work the well‐known weakness of the polar
fields since cycle 23 was associated with changes in the active regions around 2003. Extrapolating
coronal potential‐field models, Petrie found that the coronal multipoles divide neatly into large‐
scale, axisymmetric components following the polar fields and small‐scale, 3D components that
follow the activity. He found that eruption statistics have been enhanced since 2003 because of the
weakness of the polar fields. Having studied Lorentz force changes during six major neutral‐line
flares using a method invented by G. Fisher (UC Berkeley) applied to high‐cadence HMI vector
data, Petrie showed that this method can reliably produce local estimates for large structures
within regions composed of strong magnetic field, such as sunspots and strong neutral lines. He is
investigating links between these Lorentz force changes and sunquakes with helioseismologists.
With 2013 REU student Darryl Seligman (U. Pennsylvania) and NSO’s Rudi Komm, Petrie is
comparing the magnetic and current helicities of active regions to the kinetic helicity of the interior
flows beneath. This may clarify the cause of twisted, sheared emerging fields that ultimately result
in flares and eruptions. Petrie and 2012 REU student Karl Haislmaier (George Mason U.) found
that, although coronal structure often changes during the emergence of active regions, when a
coronal hole appears in the region’s place after it decays the global structure does not change
significantly in response. With NSO colleagues Luca Bertello and Alexei Pevtsov, Petrie showed
that variances in synoptic magnetogram measurements can impact extrapolated field models for
the solar atmosphere.
Service
Petrie developed software that simulates poorly observed and unobserved fields at polar solar
latitudes. This work has been applied to GONG and SOLIS synoptic maps that will appear on the
NISP Web site (they currently appear on the separate GONG and SOLIS pages). Accompanying
potential field modeling products developed with Janet Luhmann (UC Berkeley) will also appear.
Petrie helped NSO programmer Richard Clark to solve a problem with a zero‐point correction
algorithm which is applied to GONG full‐disk mangetograms and which he helped to develop a
few years ago with Jack Harvey and Clark. The problem arose from unanticipated effects of the
ascent of cycle 24 activity. As in the past, Petrie mentored REU students in 2012 and 2013 (see
research results). Haislmaier’s project appeared in the Astrophysical Journal this year and
Seligman’s project is being prepared for publication. Petrie has provided NSO data user support
on accessing and applying NSO magnetogram data for various users including AFRL,
NASA/CCMC, NOAA/SWPC, Predictive Science, U. Michigan, as well as users in Europe. Petrie
participated in NSF proposal merit reviews in late 2012 and 2013. He refereed manuscripts for the
Astrophysical Journal, Solar Physics and the Journal of Geophysical Research.
Alexei A. Pevtsov, Astronomer
Areas of Interest
Solar magnetic fields: topology, evolution, helicity, vector polarimetry; corona: coronal heating, x‐
ray bright points, coronal holes; sunspots: topology, evolution, Evershed flow, penumbral fine
Sstructure; space weather: solar drivers; chromosphere: filaments and prominences, Moreton
waves; solar‐stellar research.
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Recent Research Results
Pevtsov collaborated with NSO and non‐NSO scientists on studies of sunspot magnetic fields,
topology of coronal magnetic fields derived from non‐linear force‐free modeling, cycle variation of
basal chromospheric profiles, kinetic and magnetic helicities on the Sun, magnetic transients
associated with flares, and the effect of errors in synoptic maps on extrapolated fields. He also
worked on improvements to data reduction for observations taken by SOLIS.
Sun‐as‐a‐star spectra were used to study the chromopsheric Ca K line profiles and their change
with the solar cycle. The observed profiles were deconvolved on basal (quiet Sun) and plage
(active Sun) components. Basal profiles represent the lowest state of the solar chromosphere in the
absence of any activity and, thus, are not expected to vary with the solar cycle. To verify the
successful deconvolution, time series of both types (active and quiet Sun) were analyzed for
presence/absence of solar rotation, and no rotational modulation was found in the basal profiles.
Subsequent analysis showed that the basal profiles do show slight changes in phase with the solar
cycle. These changes were interpreted as the result of modulation of flux of acoustic waves
responsible for the basal component of the chromospheric heating.
Future Research Plans
Pevtsov plans to continue his research on properties and evolution of magnetic fields on the Sun
and heliosphere. As a long‐term goal, this research aims at understanding how magnetic fields are
created by the global and local dynamos, how the magnetic field evolves as it travels through
different layers of solar atmosphere and to the Earth orbit, how magnetic fields of localized
features interact with each other, forming a large‐scale field of the Sun, and how magnetic fields
decay. He also plans to continue studies of the Sun‐as‐a‐star using SOLIS/ISS data, including
adding a solar‐stellar component. Pevtsov plans to spend a portion of his research time on studies
related to the NSO synoptic program including development of new data products based on
SOLIS and GONG synoptic magnetograms.
Service
A. Pevtsov is the Solar Atmosphere Program Scientist for the NSO Integrated Synoptic Program
(NISP). In that capacity, he coordinates and leads the research and data analysis efforts by NSO
scientists, postdocs, and scientific programmers associated with the program (which includes
SOLIS and GONG projects). Pevtsov reviewed proposals for NASA and NSF and served as a
reviewer for several professional publications. He supervises the NSO/SP technical library, and is
a member of telescope allocation committees for NSO/SP and SOLIS. In 2013, he mentored one
postdoctoral researcher. He serves on the Usersʹ Committee for HAO’s Mauna Loa Solar
Observatory. He is the chair for the International Astronomical Union (IAU) Working Group on
Coordination of Synoptic Observations of the Sun and the vice‐chair for the IAU Inter‐Division
Working Group on Solar‐Type Stars. He is a member of the Math and Science Advisory Council
(MSAC) for New Mexico State’s Public Education Department.
Kevin Reardon, NSO Data Center Scientist
Areas of Interest
Dynamics and structure of the solar chromosphere; implementation of modern techniques for data
archiving, processing, and discovery; innovative application of imaging spectroscopy techniques;
post‐focus instrumentation development; spectropolarimetry of the solar atmosphere; studies of
inner planets and comets.
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Recent Research Results
K. Reardon has recently been working with Philip Judge (HAO) and Gianna Cauzzi
(INAF/Arcetri) on trying to understand the nature of the fine‐scale, highly dynamic structures in
the solar chromosphere. The high temporal and spatial resolution data obtained with IBIS show
changes along extended fibrils occurring on timescales a just a few seconds, difficult to reconcile
with magnetohydrodynamic evolution in the chromospheric plasma. Reardon and colleagues
published a paper in 2012 and are preparing a follow‐up paper on this subject for submission to
the Astrophysical Journal.
K. Reardon also has recently published a paper in Icarus with Andrew Potter (NSO), Rosemary
Killen (NASA GSFC), and Thomas Bida (Lowell Obs.) with an analysis of the exosphere of
Mercury imaged during the 2006 transit of that planet across the Sun. The authors were able to
map the exospheric column density, scale height, and temperature around the full terminator of
Mercury using the imaging spectroscopy data obtained with IBIS. The differences with respect to
some earlier measurements indicate that terminator processes might play an important role in
determining the characteristics of the exosphere in this region. The authors are continuing their
collaboration, together with Valeria Mangano (INAF/IAPS, Italy), in pursuing daytime
observations of Mercury at the Dunn Solar Telescope with IBIS.
Future Research Plans
K. Reardon will work on the application of new methods for processing the large volumes of data
obtained currently at the DST and the even greater challenges for the data to be obtained with the
ATST. This will include techniques for calibrating and classifying the contents of those data, as
well as data distribution channels, including the Virtual Solar Observatory, that support data
discovery by the community.
K. Reardon will continue to work with Philip Judge and others in seeking a better understanding
of the small‐scale behavior of the solar chromosphere. This will involve observations pushing the
current limits in temporal and spatial scales, as well as spectropolarimetric measurements of the
chromosphere, all coupled with the novel data from the Interface Region Imaging
Spectrograph (IRIS).
K. Reardon is also Co‐PI on a project with Fabio Cavallini and Vincenzo Greco (INAF/Arcetri) to
develop an exploratory design for a tunable narrowband filter in the near‐infrared (0.9‐1.6
microns) for ATST. This design, to be delivered in the coming year, is for a compact dual Fabry‐
Perot system that would permit diffraction‐limited observations over a 90 arcsecond field‐of‐view.
Service
As the NSO Data Center Scientist, Reardon is developing plans and approaches for the processing
and archiving of the data from the ATST, as well as for the implementation of a modern data
center deploying advanced analysis techniques in support of NSOʹs mission.
Reardon has developed tools that allow the solar community to locate and access dataset of interest
from the Dunn Solar Telescope. The system generates summaries of the data obtained at the DST and
provides summary Web pages that provide PIʹs and other users a quick overview of the available data.
This system has been deployed for the two service‐mode observing periods at the DST.
K. Reardon continues to support IBIS as a community instrument, providing guidance to users,
software support, and ongoing improvements to the systems. He was one of the leads in
providing supporting observations from the DST for the Hi‐C, EUNIS, and VERIS sounding rocket
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launches from NASAʹs White Sands Missile Range, as well as for the coordinated observations
with the IRIS mission. He also provided support for observations of comets PANSTARRS and
ISON with the DST, the latter as part of the international campaign to observe this rare sun‐grazing
comet.
Thomas R. Rimmele, Astronomer
Areas of Interest
Sunspots; penumbra; small‐scale magnetic fields; active region dynamics; flares; acoustics waves;
weak fields; adaptive optics; multi‐conjugate adaptive optics; instrumentation.
Recent Research Results
During the past three years, Rimmele has co‐authored more than 30 papers and gave a number of
invited talks at e.g., SPIE, OSA, IAU, EGU and other conferences. His scientific focus is on
advancing the ATST science objectives and the development of adaptive optics technology. In this
context, Rimmele co‐organized the ATST/EAST workshop in Washington, DC in 2011 and served
as editor of the conference proceedings. He served on the scientific organizing committee for two
adaptive optics conferences (AO4ELT, Florence, Italy 2013; Adaptive Optics: Methods, Analysis
and Applications, Arlington, VA 2013). Rimmele leads the NSO solar AO and MCAO programs.
A conventional AO system with a 357‐actuator deformable mirrors has recently been
commissioned at the 1.6‐m NST at BBSO and is producing the highest resolution solar imagery.
An MCAO system with three deformable mirrors is currently undergoing final integration and
testing. These systems serve as pathfinders for the ATST.
Rimmele co‐supervised a graduate student, who has completed his thesis work using narrow‐band
imaging data from the DST. He is currently supervising a graduate student, who is developing
adaptive optics for solar prominences and a postdoc, who is developing MCAO in collaboration
with the Kiepenheuer Institute and NJIT.
Future Research Plans
Rimmele will continue his efforts to perform observations at the highest spatial resolution using
adaptive optics in order to study the properties and the dynamics of small‐scale magnetic
elements. Due to the extensive commitments to service, Rimmele has very limited and continuous‐
ly decreasing amount of time available for research.
Service
Rimmele is NSO Associate Director and PI for the Advanced Technology Solar Telescope, and as
such has overall responsibility for the construction of the ATST and for planning the operations
and executing the ramp up to full operations of ATST in 2019. He is principal investigator of the
NSO Solar Adaptive Optics Program. Rimmele participates in the European Association for Solar
Telescopes (EAST) council meetings as representative on the SOLARNET Board. *Sushanta C. Tripathy, Associate Scientist
Areas of Interest
Helioseismology; solar oscillations and activity cycle; multi‐wavelength helioseismology; sub‐
surface flows of active regions; validation of numerical simulations.
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Recent Research Results
S. Tripathy has continued the investigation of spatial and temporal variations of the high‐degree
mode frequencies calculated over localized regions of the Sun during solar cycles 23 and 24.
Recent work with K. Jain and F. Hill has shown that the magnitude of the frequency shifts
calculated from high‐degree modes are ten times greater than the intermediate‐degree modes and
is found to be consistent with the study of high‐degree mode frequencies measured from global
helioseismology. They also found that both individual multiplets and disk‐averaged frequency
shifts are linearly correlated with solar activity indices instead of a quadratic relationship as
reported earlier.
Tripathy and collaborators have also looked at the mechanism that drives the quasi‐biennial
periodicity (QBP) in the Sun. The intermediate degree modes indicate that the QBP signal strength
has been strong over the ascending phase of the solar cycle 23, but suddenly became weaker in
2003 and has remained weak during the ascending phase of cycle 24. Based on these, it is argued
that cycle 24 would be weaker compared to cycle 23.
Working with the ring‐team, Tripathy has extended the multi‐wavelength analysis to include few
more complex active regions. Using data from GONG, HMI and AIA, they report that the
magnitude of the differences between mode frequencies computed from different spectra is
significantly large at the higher end of the frequency range while the differences between the
Doppler measurements from two different instruments are marginal. They also find that the sub‐
surface flows, in general, are consistent between different observables.
Tripathy and collaborators processed an artificial data set of wave propagation through the GONG
ring‐diagram pipeline and estimated the differential rotation and meridional flow profiles used in
the simulation. The preliminary result shows good agreement with the input model.
Future Research Plans
Tripathy will continue to carry out a statistical analysis of active regions using mutli‐wavelength
data from HMI, AIA, GONG and SOLIS and fit the cross‐spectra for an accurate determination of
mode frequencies and other parameters. He also plans to extend the analysis of realistic numerical
simulations to validate the ring‐diagram technique. Tripathy will continue to investigate the
global and local oscillation frequencies to understand the variations between different solar cycles
and mechanisms that drive the changes in oscillation frequencies.
Service
S. Tripathy organizes the monthly NISP science meeting at NSO. In May 2013, he co‐chaired the
27th NSO workshop entitled “Fifty Years of Seismology of the Sun and Stars” held in Tucson. He
also obtained partial financial support from NSF to organize the workshop. Tripathy participates
in proposal writing to obtain outside funds for NISP‐related projects. In recent past, he has been a
reviewer for NSF scientific proposals. Alexandra Tritschler, Associate Scientist
Areas of Interest
Operational modes of large facilities; tools used by the users and operators of such facilities. High‐
resolution spectroscopy and spectropolarimetry of the photosphere and chromosphere; solar
magnetic fields; fine‐structure of sunspots, simulations of the influence of atmospheric turbulence
and instrumentation on solar observations; post‐focus instrumentation.
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Current and Future Plans
Tritschler’s main science interests have been focused on the high‐resolution (spectral, spatial and
temporal) aspects of solar physics and the fine structure of sunspots and pores in particular. She
intends to pursue this interest further, employing IBIS (as well as FIRS and SPINOR) to determine
the properties of photospheric and chromospheric layers of active regions and to infer their three‐
dimensional dynamic and magnetic structure and to compare those results to forward modeling.
Tritschler will continue to investigate Service Mode Operations in solar physics using the Dunn
Solar Telescope as a test bed for the ATST.
Service
A. Tritschler is the ATSTʹs Operational Scientist and as such leads the development effort of
operational concepts for the ATST. She is responsible for the development and specification of
tools to be used to efficiently operate the ATST. Tritschler leads the Service Mode Operations
effort of the Dunn Solar Telescope in preparation for the ATST. Service Mode Operations of the
DST are offered currently twice per year to the international community. Tritschler has been
mentoring numerous summer REU and SRA students and is a member of the Sacramento Peak
telescope allocation committee for the Dunn Solar Telescope. She is also the colloquium organizer
in Sunspot and was/is actively involved in the organization of traditional Sunspot summer
workshops and sessions at the IAU and AAS/SPD. Tritschler has served on proposal panel
reviews and has been a reviewer of publications for the Astrophysical Journal Letters, Astrophysical
Journal, Astronomy and Astrophysics, Solar Physics, and Astronomical Notes.
Han Uitenbroek, Astronomer
Areas of Interest
Radiative transfer modeling and structure and dynamics of the solar atmosphere; modeling and
measurement of polarized light and interpreting observations.
Recent Research Results
H. Uitenbroek continues to work on expanding and improving his multi‐dimensional numerical
radiative transfer code RH. The RH code has been made available to the community from the
start and is widely used by the solar community and, in some cases, even outside that. The RH
code has been used to calculate Mg II spectra from Rad‐MHD simulations of solar chromospheric
dynamics in preparation for the launch of the IRIS mission. The results have been published in
three ApJ papers that have been released recently. The code has also been used by Adam Kowalski
(NASA GSFC) to model flare spectra in M‐dwarfs, by Holtzeuter (MPS Lindau) et al. to model
non‐LTE iron line spectra in 3D, and by Nelson et al. to model Ellerman bomb spectra in hydrogen
and iron lines. Together with E. Mallorca (Perugia, Italy), Uitenbroek has used the code to
determine that the solar fluorine abundance is about a factor six less than previously thought.
With Serena Criscuoli, Uitenbroek developed a novel method to accurately measure the tempera‐
ture gradient in the solar atmosphere at high spatial resolution using opacity‐conjugate
wavelengths. The ultimate goal is to implement this method in a satellite mission being developed
by the Laboratory for Atmospheric and Space Physics in Boulder, and to use it to refine modeling
of spatially resolved solar irradiance. Together, they also worked on characterizing the center‐to‐
limb variations of irradiance due to small‐scale magnetic elements.
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Future Research Plans
Development and maintenance of the RH code will continue. Concentration will be on the
contribution to irradiance at different wavelengths from small‐scale magnetic elements, forward
modeling of polarized Sunspot spectra, and forward modeling of polarized radiation from
chromospheric structures, both from state‐of‐the‐art 3D Rad‐MHD simulations. Uitenbroek will
also undertake analysis of IRIS spectra and comparison of its spectra with forward modeling of the
Mg II lines.
Service
Uitenbroek is the program scientist for the Dunn Solar Telescope at Sac Peak. In addition, he
serves as chair of the Sac Peak Telescope Allocation Committee, leads the IT department in
Sunspot, and is part of the NSO Scientific Personnel Committee (SPC). With Alexandra Tritschler,
Uitenbroek leads the REU/RET effort at Sacramento peak. About fifteen different researchers from
different institutes, some even outside the field of solar physics, have requested copies of
Uitenbroekʹs transfer (RH) code. He actively supports those users with updates and helps with
running the code. He is Co‐I on the IRIS SMEX proposal by Lockheed that was launched by NASA
in June 2013. The RH code is provided on the IRIS data distribution Web page for downloading.
Uitenbroek is also member of the planning working group for the next Japanese solar satellite
Solar C. He regularly serves as referee for papers and on review panels for proposals.
Fraser Watson, Postdoctoral Research Associate
Areas of Interest
Long‐term sunspot properties; changes in the solar cycle; automated image processing; synoptic
data analysis; spectro‐polarimetric analysis of sunspot data.
Recent Research Results
F. Watsonʹs most recent research result comes from an analysis of sunspot magnetic field data from
SOHO/MDI and SDO/HMI. A review of sunspot fields over the solar cycle measured in a synoptic
way show a decrease in sunspot umbral field strengths that is only a third of what has been
previously reported. Further analysis shows bias in the Livingston data set used to derive the
previously reported results due to changes in sunspot sampling over the lifetime of the data
catalogue. This result will be of great importance in studies of the solar cycle and the solar dynamo
and is being prepared for publication.
Future Research Plans
The sunspot data from the McMath‐Pierce Solar Telescope will be compared with spectro‐
polarimetric sunspot observations from the Dunn Solar Telescope to allow for cross calibration of
the two instruments being used. This will also allow for some analysis into the capabilities of the
Advanced Technology Solar Telescope. The sunspot catalogue obtained from MDI and HMI data
will be further probed to determine a number of properties and how they vary over the solar cycle.
Again, this is of use in dynamo models and studies of changes in solar cycle.
Service
F. Watson assists in the synoptic observing program at the McMath‐Pierce Solar Telescope, and
recently assisted in the service‐mode observing program at the Dunn Solar Telescope. Over the
past year, he has represented NSO at seven public outreach events. He has served on two NASA
grant review panels and as a referee for the journal Solar Physics.
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Friedrich Wöger, Associate Scientist
Areas of Interest
Image reconstruction techniques; adaptive optics; two‐dimensional spectroscopy, and spectro‐
polarimetry; ATST visible broadband imager (VBI); ATST data handling system (DHS).
Recent Research Results
Wöger is the principle investigator of the VBI, and as such is overseeing the construction of the
hard‐ and software elements of the instrument. The VBI is in the process of being set up at NSO’s
Boulder location for thorough testing of all optical, mechanical and software assemblies, such as
early versions of the VBI control software. The NSO laboratory in Boulder will allow end‐to‐end
testing of the VBI and many ATST sub‐sytems.
Wöger has been working on a theory to compute the transfer function of Earthʹs turbulent
atmosphere and the adaptive optics system directly from the data delivered by the adaptive optics
system. This is important to achieve high photometric precision in images reconstructed using
speckle reconstruction algorithms. He is currently working on a theory that extends the validity of
the transfer function models to very large field of views.
Wöger has been involved in research related to alternate wavefront sensing instruments for solar
adaptive optics, and multi‐conjugate adaptive optics in collaboration with Jose Marino (NSO).
Wöger, with Marino, evaluated the feasibility of a Shack‐Hartmann wavefront sensing approach
for layer oriented sensing of Earth’s turbulent sensor. This approach will have limitations when
applied to solar multi‐conjugate adaptive optics as a thorough theoretical and experimental study
has shown.
Future Research Plans
Wöger is planning to work on improved methods for image reconstruction for data acquired with
2D spectroscopic and spectro‐polarimetric instruments, such as ATST VTF data. These algorithms
will be based on speckle interferometry and allow the acquisition of data at diffraction‐limited
resolution. He continues to work on developing accurate models for atmospheric transfer func‐
tions, and is interested in investigating expanding current models for use with multi‐conjugate
adaptive optics systems.
Service
Wöger is the scientist responsible for the VBI and, with the VBI team, is continuously assessing the
progress of the VBI’s construction. He is involved in the ATST data handling system development
as the ATST Data Handling Scientist, with the responsibility of overseeing the proper imple‐
mentation of the requirements defined for the system and creating a complete data model for
ATST. In his function as the ATST Wavefront Correction Scientist, Wöger is guiding the ATST
WFC team towards a Critical Design Review by reviewing all WFC documentation that describes
derived design requirements and the design itself. He also has a role in the optical design effort
for the wavefront sensors.
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APPENDIX I: ACRONYM GLOSSARY
A&E Architecture and Engineering
ADAPT Air Force Data Assimilative Photospheric flux Transport
AFRL Air Force Research Laboratory
AFWA Air Force Weather Agency
AIA Atmospheric Imaging Assembly (SDO)
AISES American Indian Science and Engineering Society
aO Active Optics
AO Adaptive Optics
AR Active Region
ARRA American Recovery and Reinvestment Act
ASP Advanced Stokes Polarimeter
ATI Advanced Technology Instrumentation (NSF)
ATM Atmospheric Sciences (Division of NSF)
ATRC Advanced Technology Research Center (University of Hawai‘i)
ATST Advanced Technology Solar Telescope
AURA Association of Universities for Research in Astronomy, Inc.
BLNR Bureau of Land and Natural Resources
BBSO Big Bear Solar Observatory
CAM Cost Account Manager (ATST)
CCMC Community Coordinated Modeling Center
CD‐ROM Compact Disk – Read Only Memory
CDR Critical Design Review
CDUP Conservation District User Permit
CfA Center for Astrophysics (Harvard Smithsonian)
CfAO Center for Adaptive Optics
CHU Critical Hardware Upgrade
CISM Center for Integrated Space Weather Modeling
CLEA Contemporary Laboratory Exercises in Astronomy
CMEs Coronal Mass Ejections
CNC Computer Numerical Controlled
CoDR Conceptual Design Review
CoRoT COnvection ROtation and planetary Transits (French Space Agency CNES)
CoSEC Collaborative Sun‐Earth Connection
CR Carrington Rotation
CSF Common Services Framework
CSP Critical Science Plan
CU University of Colorado, Boulder
DA Diversity Advocate
DB‐P Dual‐beam Polarizer (McMath‐Pierce Telescope)
D&D Design & Development
DASL Data and Activities for Solar Learning
DEIS Draft Environmental Impact Statement
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DEM Differential Emission Measure
DHS Data Handling System
DL‐NIRSP Diffraction‐Limited Near‐Infrared Spectropolarimeter (ATST)
DLSP Diffraction‐Limited Spectro‐Polarimeter
DLT Digital Linear Tape
DM Deformable Mirror
DMAC Data Management and Analysis Center (GONG)
DoD Department of Defense
DRD Design Requirements Document
DRMS Decision, Risk and Management Sciences (NSF)
DST Dunn Solar Telescope
EAST European Association for Solar Telescopes
EGSO European Grid of Solar Observations
EIS Environmental Impact Statement
EIT Extreme ultraviolet Imaging Telescope (SOHO)
EPO Educational and Public Outreach
ESF Evans Solar Facility
EST European Solar Telescope
ETS Engineering and Technical Services (NOAO)
FDP Full‐Disk Patrol (SOLIS)
FDR Final Design Review
FEIS Final Environmental Impact Statement
FIRS Facility Infrared Spectropolarimeter
FLC Ferroelectric Liquid Crystal
FOV Field of View
FPGA Field Programmable Gate Array
FTEs Full Time Equivalents
FTS Fourier Transform Spectrometer
FY Fiscal Year
GB Giga Bytes
GNAT Global Network of Astronomical Telescopes, Inc. (Tucson)
GOES Geostationary Operational Environmental Satellites (NASA and NOAA)
GONG Global Oscillation Network Group
GSFC Goddard Space Flight Center (NASA)
GUI Graphical User Interface
HAO High Altitude Observatory
HMI Helioseismic and Magnetic Imager
HOAO High Order Adaptive Optics
HR Human Resources
HSG Horizontal Spectrograph
HXR Hard X‐Ray
IAA Instituto de Astrofísica de Andalucía (Spain)
IAC Instituto de Astrofísica de Canarias (Spain)
IBIS Interferometric BIdimensional Spectrometer (Arcetri Observatory)
ICD Interface Control Document
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ICM Inversion by Central Moments
ICS Instrument Control System
IDL Interactive Data Language
IfA Institute for Astronomy (University of Hawai`i)
IFU Integrated Field Unit (McMath‐Pierce Solar Telescope Facility)
IHY International Heliophysical Year
IMaX Imaging Magnetograph eXperiment (SUNRISE)
IR Infrared
IRES International Research Experience for Students (NSF)
IRIS SMEX Interface Region Imaging Spectrograph Small Explorer Mission (NASA)
ISOON Improved Solar Observing Optical Network (now O‐SPAN)
ISP Integrated Synoptic Program (NSO)
ISS Integrated Sunlight Spectrometer (SOLIS)
IT&C Integration, Testing, & Commissioning
KAOS Kiepenheuer Adaptive Optics System
KCE KC Environmental (Maui)
KIS Kiepenheuer Institute for Solar Physics (Freiburg, Germany)
KPNO Kitt Peak National Observatory
KPVT Kitt Peak Vacuum Telescope
LAPLACE Life and PLAnets Center (University of Arizona)
LASP Laboratory for Atmospheric and Space Physics (University of Colorado, Boulder)
LESIA Laboratoire dʹétudes patiales et dʹinstrumentation en astrophysique (Paris
Observatory)
LMSAL Lockheed Martin Solar and Astrophysics Laboratory
LoHCo Local Helioseismolgy Comparison Group
LRP Long Range Plan
LTE Local Thermodynamic Equilibrium
LWS Living With a Star
MBP Magnetic Bright Point
McMP McMath‐Pierce
MCAO Multi‐Conjugate Adaptive Optics
MCC Maui Community College
MDI Michelson Doppler Imager (SOHO)
ME Milne‐Eddington
MEDB Maui Economic Development Board
MHD Magnetohydrodynamic
MKIR Mauna Kea Infrared
MREFC Major Research Equipment Facilities Construction (NSF)
MRI Major Research Instrumentation (NSF)
MSAC Math and Science Advisory Council (State of New Mexico)
MSFC Marshall Space Flight Center (NASA)
MWO Mt. Wilson Observatory (California)
NAC NSO Array Camera
NAI NASA Astrobiology Institute
NAS National Academy of Sciences
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NASA National Aeronautics and Space Administration
NASM National Air and Space Museum
NCAR National Center for Atmospheric Research
NDSC Network for the Detection of Stratospheric Change
NHPA National Historic Preservation Act
NHWG Native Hawaiian Working Group
NIR Near Infrared
NJIT New Jersey Institute of Technology
NLFFF Non‐Linear Force‐Free Field
NLTE Non‐Local Thermodynamic Equilibrium
NMDOT New Mexico Department of Transportation
NOAA National Oceanic and Atmospheric Administration
NOAO National Optical Astronomy Observatory
NPDES National Pollutant Discharge Elimination System
NPFC Non‐Potential Field Calculation
NRC National Research Council
NSBP National Society of Black Physicists
NSF National Science Foundation
NSF/AST National Science Foundation, Division of Astronomical Sciences
NSF/ATM National Science Foundation, Division of Atmospheric Sciences
NSHP National Society of Hispanic Physicsts
NSO National Solar Observatory
NSO/SP National Solar Observatory Sacramento Peak
NSO/T National Solar Observatory Tucson
NST New Solar Telescope (NJIT Big Bear Solar Observatory)
NWNH New World New Horizons (Astro2010: Astronomy & Astrophysics Decadal Survey)
NWRA/CoRA NorthWest Research Associates/Colorado Research Associates
OCD Operations Concept Definition Document (ATST)
OCS Observatory Control System
OMB Office of Management and Budget
O‐SPAN Optical Solar Patrol Network (formerly ISOON)
PAARE Partnerships in Astronomy & Astrophysics Research & Education (NSF)
PAEO Public Affairs and Educational Outreach (NOAO)
PCA Principal Component Analysis
PDR Preliminary Design Review
PI Principal Investigator
PMCS Project Management Control System
ProMag PROminence Magnetometer (HAO)
PSPT Precision Solar Photometric Telescope
QA/QC Quality Assurance/Quality Control
QBP Quasi‐Biennial Periodicity
QL Quick‐Look
QSA Quasi‐Static Alignment
QU Queens University (Belfast, Ireland)
RASL Research in Active Solar Longitudes
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RDSA Reference Design Studies and Analyses
RET Research Experiences for Teachers
REU Research Experiences for Undergraduates
RFP Request for Proposal
RHESSI Reuven Ramaty High Energy Solar Spectroscopic Imager (NASA)
RISE/PSPT Radiative Inputs from Sun to Earth/Precision Solar Photometric Telescope
RMS Root‐Mean‐Square
ROD Record of Decision
ROSA Rapid Oscillations in the Solar Atmosphere
SACNAS Society for the Advancement of Chicanos an Native Americans in Science
SAN Storage Area Network
SASSA Spatially Averaged Signed Shear Angle
SCB Sequential Chromospheric Brightening
SCOPE Southwest Consortium of Observatories for Public Education
SDO Solar Dynamic Observatory
SDR Solar Differential Rotation
SFC Space Flight Center (NASA)
SH Spherical Harmonic
SMO Service‐Mode Operations
S&O Support and Operations (ATST)
SOC Solar Observatory Council (AURA)
SOHO Solar and Heliospheric Observatory
SOI Solar Oscillations Investigations (SOHO)
SOLIS Synoptic Optical Long‐term Investigations of the Sun
SONG Stellar Oscillation Network Group
SOT Solar Optical Telescope
SOT/SP Solar Optical Telescope Spectro‐Polarimeter (Hinode)
SOW Statement of Work
SPINOR Spectro‐Polarimeter for Infrared and Optical Regions
SPD Solar Physics Division (AAS)
SPRING Solar Physics Research Integrated Network Group (European Union)
SRA Summer Research Assistant
SRD Science Requirements Document
SREC Southern Rockies Education Centers
SSL Space Sciences Laboratory (UC Berkeley)
SSP Source Selection Plan (ATST)
SST Swedish Solar Telescope
SW Solar Wind
SSWG Site Survey Working Group (ATST)
SWG Science Working Group (ATST)
SWMF Space Weather Modeling Framework
SWPC Space Weather Prediction Center (NOAA)
SWRI Southwest Research Institute
STARA Sunspot Tracking and Recognition Algorithm
STEM Science, Technology, Engineering and Mathematics
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STEP Summer Teacher Enrichment Program
SUMI Solar Ultraviolet Magnetograph Investigation (NASA, MSFC)
SUP Special Use Permit
TAC Telescope Time Allocation Committee
TB Tera Bytes
TCS Telescope Control System
TLRBSE Teacher Leaders in Research Based Science Education
TMA Telescope Mount Assembly
TIMED/SEE Thermosphere Ionosphere Mesosphere Energetics and Dynamics / Solar EUV
Experiment (NASA)
TRACE Transition Region and Coronal Explorer
UA University of Arizona
UH University of Hawaii
UBF Universal Birefringent Filter
UPS Uninterruptible Power Supply
USAF United States Air Force
USF&WS US Fish and Wildlife Service
VBI Visible‐light Broadband Imager (ATST)
VCCS Virtual Camera Control System (Dunn Solar Telescope)
VFISV Very Fast Inversion of the Stokes Vector (Inversion Code, HMI)
ViSP Visible Spectropolarimeter (ATST)
VSM Vector Spectromagnetograph (SOLIS)
VSO Virtual Solar Observatory
VTF Visible Tunable Filter (ATST)
WBS Work Breakdown Structure
WCCS Wavefront Correction Control System
WDC Workforce and Diversity Committee (AURA)
WHI Whole Heliospheric Interval
WSA Wang‐Sheeley‐Arge (Solar Wind Model)
WSDL Web Service Description Language
WWW World Wide Web