Jun 4, 2008

Brazilian Tunable Filter ImagerBrazilian Tunable Filter Imager(BTFI)(BTFI)

Preliminary Design Review (PDR)Preliminary Design Review (PDR)

USP-IAG Universidade de São USP-IAG Universidade de São PauloPaulo

18-19th June 200818-19th June 2008

Claudia Mendes de OliveiraClaudia Mendes de Oliveira

Jun 4, 2008

The purpose of the PDR is to report on the project progress during the design phase and present the detailed design of the optics, mechanics,controls and software of the instrument.

At the time of the PDR, the majority of the design work should be completed and most technical choices been made. The design should be essentially ready to proceed to construction with sufficient detail to obtain accurate costings of staff time, materials and procurements.

The PDR is an opportunity for external reviewers to critically examine the design and identify any shortcomings or changes that need to be made.

The PDR is an important project milestone since a decision will be made at this point whether to proceed with full construction.

Preliminary design review - PDR

Jun 4, 2008

Reviewers

Claude Carignan (Chair, U. of Montreal) Patricio Schurter (Mechanics, CTIO) Marco Bonati (Eletronics/Software, CTIO)

Jun 4, 2008

Collaborating InstitutionsCollaborating Institutions

University of São Paulo, Brazil (IAG, Poli) Instituto National de Pesquisas Espacias, Brazil

(INPE) Laboratório Nacional de Astrofísica, Brazil (LNA) Universidade Estadual de Santa Cruz, Brazil Laboratoire d'Astrophysique de Marseille, France

Jun 4, 2008

Claudia Mendes de Oliveira (USP) - PI Keith Taylor (USP) – Instrument Scientist and Manager Rene Laporte* (INPE) – Mechanical and Optical Engineer César de Oliveira (LNA) – Optical Engineer Cesar Strauss (INPE) – Electronic Engineer (EE) Luiz Reitano (INPE) – Mechanical technician Fernando Lourenço* (USP/INPE) – Mechanical technician Luiz Cavalcanti* (USP) and Denis Andrade* (INPE) – EE Giseli Ramos* and Fernando Fontes (USP) – Software

Engineers Bruno Correa Quint* (USP) – Instrument Physicist Lígia de Oliveira (LNA) – Optical technician Javier Ramirez Fernandez and students (Poli/USP) - EE* Working full-time for the projectScience Team Claudia Mendes de Oliveira (USP) Henri Plana, Jaqueline Vasconcelos and Adriano Cerqueira (U. Santa Cruz) Francisco Jablonski (INPE) Laerte Sodré Jr. and João Steiner (IAG/USP) François Cuisinier and Denise (Obs. Valongo)

Instrument TeamInstrument TeamBTFI project

Jun 4, 2008

Consultants Dani Guzman (AstroInventions) – Eletronics/Detectors Damien Jones (Prime Optics, Qld) – Optical Design Olivier Daigle (U. Montreal) - Detectors Peter Gray (Atacama) - Management Sebastien Blais-Ouellette (PhotonEtc) – iBTF physicist Jean-Luc Gach (LAM) – Optics/Eletronics Carlos Burato (PMEC-sistemas) – ME Olivier Hernandez (U.Montreal) – Science Philippe Amram (LAM) - Science

Jun 4, 2008

Presentation OverviewPresentation Overview Intro, science goals, budget

management (Claudia) Management Overview (KT) Optical and opto-mechanical designs

(KT) Eletronics and software instrument

control Motors, encoders, drivers (Fernando

Fontes) Integration into the SOAR architecture

(Giseli Ramos) Detector controller (Keith/Denis/Javier) System modelling/BTFI efficiencies

(Bruno/KT) Etalon controller (Luiz Cavalcanti -

video) BTFI emulator (KT/Fernando/Giseli) Data reduction (KT) Management summary (KT)

Jun 4, 2008

The BTFI instrument is in fact two instruments in one:

An iBTF Low resolution mode: 5 < R < 3000

A Fabry-Perot instrument High resolution mode: 10000 < R <

35000

In most cases we can also obtain images in a complementary channel, for transparency/seeing monitoring.

Jun 4, 2008

Modes of Operation

Order 1 Order 0 iBTF(Lo-R) Compl. ChanneliBTF(Lo-R) FPP (Hi-R)Compl. Channel FPP (Hi-R)Compl. Channel FPI(Block) . FPP(Hi-R)iBTF(Lo-R) FPP(Hi-R)

Symultaneous observations with Fabry Perot and iBTF are possible!

Jun 4, 2008

BTFI on SOAR – two modes SAM’s GLAO-fed mode (field 3’ x 3’):

For programs which need excellent spatial resolution Centers of AGNs, physics of HII galaxies, mergers,

etc...

Seeing-limited mode (Nasmith IR focus - 3’ x 3’):

May be the mode in use for the first years when SAM LGS may not be available

Dynamics of nearby galaxies, mapping abundance variations in normal galaxies, etc...

Jun 4, 2008

Science Requirements summary

FP observations - kinematics of diffuse emission-line objects

iBTF observations Requirements Summary

Type of data to be acquired – data-cubes Wavelength Range – 3700 to 9000 A Spectral & Spatial Resolution - R=5-35000,

pix=0.12/0.24 arcsec Inst. efficiencies - peak= 18%, SNRs >3 @ 2.10-

17ergs.s-1.cm-2.arcsec-2

Modes of operation - GLAO-fed or seeing-limited Instrument Status on SOAR – hopefully a community

instrument by the time it is

commissioned Operation, Support & Maintenance given by the

Observatory

Jun 4, 2008

Visitor or facility instrument?

Brazil is responsible for building two SOAR facility instruments, approved by the SOAR Board, SIFS (an IFU bench-mounted spectrograph) and STELES (a cross-diserpsed echelle spectrograph).

LNA made a call for proposals for new possible SOAR instruments supported by our National office in November 2007 and we sent in our application for BTFI.

A review panel was formed by LNA and Keith and I presented the state of our work on BTFI for this committee on March 25th/2008.

A report about BTFI was written (“LNA report” - first agenda item) and then given to the LNA Board members, who decided on June 7th 2008 that BTFI should be taken as LNA responsibility.

LNA will investigate if BTFI is interesting to other SOAR partners as a facility instrument. This topic will be discussed by Albert in the next SOAR Board meeting on June 19th/2008.

Jun 4, 2008

SCIENCESCIENCE

BTFI is a very broadly capable BTFI is a very broadly capable facility instrumentfacility instrument

Jun 4, 2008

Seeing-limited mode Dark matter distribution via kinematics of galaxies Internal structure of galaxies, bars, non-circular

motions PNe in external galaxies Kinematics and evolution of planetary nebula Physics and kinematics of HH objects and proplyds Photometric redshifts: redshift estimates, star/galaxy

classification, galaxy spectral type Pre-selection of objects for spectroscopic

observations Physics of Planetary nebulae and HII regions HH objects Galaxy Evolution: metallicity gradient in nearby

galaxies through 2D maps of emission lines: [OII]3727A, Hβ, [OIII]5007A, Hα, [NII].

Seyfert Galaxies, liners and AGNs, star-forming galaxies in groups and clusters Ionization maps using 2D maps of emission lines

and 2D maps of continuum.

Jun 4, 2008

Scientific projects which need BTFI in SAM’s GLAO-

fed mode

Stellar mass loss

Galaxy interaction and merging to z~0.5 Evolution of galaxies at medium z (<0.2) AGN physics at low and medium redshift HII galaxies Kinematics/metallicities of TDGs and

BCGs Measuring the mass of black holes in the

centers of galaxies from the kinematics of

the gas

Jun 4, 2008

• Mass loss from stars is a complex and poorly understood phenomenon, but crucial to discuss stellar and galactic evolution. In particular, the (quasi) spherical symmetry that characterizes the whole evolution of a star breaks in its latest stages, when strong mass loss determines its fate as a white dwarf, a neutron star or a black hole.

• This is (clearly) demonstrated by the extraordinary variety of shapes displayed by planetary nebulae and other stellar ejecta. Any kind of symmetries are found at small and large scales, and multiple outflows are often seen in the same object, indicating complex mass loss time histories.

• After two decades of intense debate, the origin of this anisotropy is still uncertain. Several processes are proposed to explain it, spanning from the emergence of strong magnetic fields when the stellar envelope is lost, to a number of mechanisms acting in interacting binaries like aspherical post-common envelope ejection, or fast collimated winds from accretion discs in mass transfer systems with periods up to 103 yr.

Stellar mass loss with BTFI

Jun 4, 2008

massive star Planetary nebula

Symbiotic star

supernova novaSymbiotic star

Planetary nebula

Examples

Jun 4, 2008

Physics & Kinematics of PNe

- Kinematics gives information on the hydrodynamics of PNe - Interpretation of expansion velocities - Combination of 3D Photoionization +

high spectral and angular resolution will give us the 3D structure of PNe --> non

- sphericity effects ?

Jun 4, 2008

In order to progress in the field, it is necessary to reveal the full 3D geometry and dynamics of the stellar ejecta. This is done by modelling images and spatially resolved high-resolution spectra (radial velocity fields). Long-slit (1D) spectra provide all information for spherical objects (the minority), but clearly lack the adequate information for more complex shapes (the majority). Therefore integral-field spectro-imaging (e.g. Fabry-Perot) is the most powerful way to get information on three of the dimensions (x,y,vradial) of the phase space.

Why BTFI?

A systematic observational effort with modern instrumentation of this type is needed for crucial classes of objects. This is for example the case of proto planetary nebulae; (mainly HST) observations show that it is in this short transition phase between red giants and PNe that the asymmetry arises. Being very young PNe, they are small and a spatial resolution as good as possible is needed to resolve their intrinsic structure.

Jun 4, 2008

The centers of active galaxiesStudy the nuclear activity of nearby galaxies to understand how mass is transferred from galactic scales down to nuclear scales to feed the supermassive blackhole. Small scale disks in the centers of AGNs have been found . We need to map the streaming motions of gas towards the nucleus, along dusty spiral arms, for a sizeable sample of galaxies.

Jun 4, 2008

Through a simple transformation one can go from a line image (S lines)to a map of the low densityand high density clouds.

Mapping low, medium and high densityclouds in AGNs, HII reg.HH objects and stars

Jun 4, 2008

Mapping low, medium and high densityclouds in AGNs

The SII emission from an AGN starburst galaxy. In Color-coded the velocitystructures, in green rest frame

Jun 4, 2008

Plans for the Future (… and Past)

Kick-off meeting: Feb 14/2007 Reviews:

Sep/07: CoDR (passed gate to Preliminary Design Phase)

Jun’08: PDR Dec’08: CDR

Feb’08: 470k proposal approved at FAPESP Mar’08: Prototyping iBTF completed (INPE LNA for

tests) May’08: Preliminary Interface Review @ SOAR Jun’08: Order detectors and controllers (in process,

with FAPESP) Jun’08: Preliminary Design Review Aug’08: Order optics Nov’08: Science with BTFI workshop Dec’08: Critical Design Review Dec’08: Begin construction phase Jun’09: Integration, Assembly & Test Phase begins Dec’09: Commissioning begins

Jun 4, 2008

Budget at CoDR

Bottoms-up total cost = US$722,586 Hardware cost = US$644,586 Estimate In-house Labor =

US$2,559,600 BTFI Equivalent TOTAL COST=

US$3,282,186 Budget detailed costing will continue

as instrument design evolves and refines.

Linked spreadsheets allow continuous updates.

Use by project management to track expenditures.

Jun 16, 2008

Jun 4, 2008

Budget at PDR

Bottoms-up total cost = US$837,350 Hardware cost = US$679,150 Estimate In-house Labor =

US$2,014,280 BTFI Equivalent TOTAL COST=

US$2,851,630 Budget detailed costing will continue

as instrument design evolves and refines.

Linked spreadsheets allow continuous updates.

Use by project management to track expenditures.

Jun 16, 2008

Milestone Schedule

Jun 4, 2008

Jun 4, 2008

Funding sources

FAPESP ARCUS LNA