1 HAWC: Continuous, Wide Field of View Observations of the Very High Energy Sky Brenda Dingus, LANL...
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Transcript of 1 HAWC: Continuous, Wide Field of View Observations of the Very High Energy Sky Brenda Dingus, LANL...
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HAWC:Continuous, Wide Field of View Observations of the Very High Energy Sky
Brenda Dingus, LANLHAWC US Spokesperson14 Nov 2013
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Nature’s Particle Accelerators:Gamma-Ray Sources
HST Image of M87
Active Galactic Nuclei:Black Hole producing
relativistic jet of particles
Short Gamma-Ray Burst:
Binary Neutron Star Coalescing
Artist Conception of Short GRBs
Long Gamma-Ray Burst:Massive Star Collapsing
into a Black Hole
Pulsar Wind Nebula:Spinning Neutron Star powering a relativistic
wind
Chandra Image of Crab
HESS TeV
+ x-ray
Supernova Remnant
X-ray Binaries/Microquas
ars
Ext
raG
alac
tic
G
alac
tic
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Electrons:Synchrotron Emission•Probes Magnetic Field, Electron Energy
Inverse Compton Scattering•Probes Photon Field, Electron Energy
Synchrotron Self Compton•If photon field is synchrotron, then electron energies are determined•Quadratic relation between variability of TeV (IC) and X-rays (synch)
Hadrons:p + p -> p+ + po +… -> e + n + g +…
p + g -> p+ + po +… -> e + n + g +…
Gamma-Rays Probe Accelerated Particles
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Active Galactic Nuclei
Massive Black Hole Accelerates Jet of Particles to Relativistic Velocities=> Synchrotron Emission and Inverse Compton and/or Proton Cascades
BeppoSAXMAGIC, CAT
M. HayashidaUrry
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Active Galactic Nuclei Flares~40 known TeV AGN
• IACT observations of <<1% duty cycle/AGN detect no flaring in most HAWC’s will monitor all Northern AGN with 20% duty cycle/day (5 hrs) regardless of sun, moon, or weather
HAWC’s 5 s sensitivity is (10,1,0.1) Crab in (3 min, 5 hrs, 1/3 yr)
Worldwide Dataset of TeV Observations by IACTs of Mrk421
1 month
Tluczykont et al. 2010
3 minutes
5 hours
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Fermi observation of GRB090510, z=0.9
• Highest Observed Energy was 33 GeV with 16 g-rays >1 GeV
• Constrained Lorentz Invariance at the Plank Mass scale
HAWC would detect this GRB if it occurred in FOV.
Gilmore& Taboada, (arXiv:1306.1127), predict 1.65 GRB/yr detected by HAWC
Gamma-Ray Bursts
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Wide Field of View, Continuous Operations
Gamma-Ray Detectors
FermiAGILEEGRET
TeV Sensitivity
HAWCARGO
Milagro Tibet AS
VERITASHESS
MAGIC
8http://arxiv.org/abs/1306.5800 Astroparticle Physics in press
HAWC SensitivityDifferential Sensitivity per Quarter Decade of Energy
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HAWC Sensitivity
Angular Resolution Hadron Rejection
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Known sources are shown, but most of the high latitude sky has not been observed at TeV energies
HAWC’s Field Of View
Sources from TeVCAT.uchicago.edu
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HAWC Design builds on the success of Milagro
Milagro “1st Generation” Water Cherenkov gamma-ray detector• 2650m (8600’) elevation near Los
Alamos, NM• Covered pond of 4000 m2 • Operated 2000-2008HAWC “2nd Generation” Water Cherenkov gamma-ray detector• 4100m (13500’) elevation near Puebla,
Mexico• 300 water tanks spread over 25000 m2
• Construction 2010-14, Operation 2013-19
• 15 x Milagro’s sensitivity with 10 x lower energy threshold
©Aurore Simonnet
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HAWC Design
180 meters
140
meters
300 close packed water tanks (7.3m dia x 4.5 m deep of 200,000 liters) each with 4 upward facing photomultiplier tubes at the bottom
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HAWC Site Location in Mexico
• High Altitude Site of 4100 m with temperate climate and existing infrastructure
• 17 R.L. of atmospheric overburdenvs 27 R.L. at sea level
• Latitude of 19 deg N
Pico de Orizaba 5600 m
(18,500’)
Large Millimeter Telescope
(50m dia. dish)
HAWC
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The HAWC Collaboration
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The HAWC CollaborationLos Alamos National Laboratory: Brenda Dingus (US
spokesperson), : Gus Sinnis, John Pretz, Patrick Younk, Gerd Kunde, Pat Harding
University of Maryland: Jordan Goodman, Andrew Smith, Jim Braun, David Berley, Brian Baughman, Josh Wood
University of Wisconsin: Stefan Westerhoff, Segev BenZvi, Mike Duvernois, Zig Hampel-Arias, Dan Fiorino, Ian Wisher, Asif Imran, Tom Weisgarber
University of Utah: Dave Kieda, Wayne Springer, Ahron BarberUniv. of California, Irvine: Gaurang Yodh, Peter KarnMichigan State University: Jim Linnemann, Kirsten Tollefson,
Dan Edmunds, Udara Abeysekara, Tilan UkwattaGeorge Mason University: Robert EllsworthColorado State University: Miguel Mostafa, Dave Warner,
Megan Longo, Paco Salesa Grues, Michael GussertUniversity of New Hampshire: James RyanPennsylvania State University: Tyce DeYoung, Dmitry Zaborov,
Kathryne Sparks University of Alabama: Patrick ToaleUniversity of New Mexico: John Matthews, Robert LauerMichigan Technical University: Petra Hüntemeyer, Emanuele
Bonamente, Nathan Kelley-Hoskins, Michelle Hui, Hugo Ayala, Hao Zhou
NASA/Goddard Space Flight Center: Julie McEnery, Elizabeth Hays, Vlasios Vasileiou
Georgia Institute of Technology: Ignacio Taboada, Andreas Tepe, Dirk Lennarz
HAWC Technical Staff: Michael Schneider, Scott Delay
Instituto Nacional de Astrofísica Óptica y Electrónica (INAOE): Alberto Carramiñana (Mexico Spokesperson), Eduardo Mendoza,
Luis Carrasco, William Wall, Daniel Rosa, Ibrahim Torres, Sergey Silich, Jason Walters
Universidad Nacional Autónoma de México (UNAM): Instituto de Astronomía; Maria Magdalena Gonzalez, Marco Martos, Sergio Mendoza, Dany Page, William Lee, Hector Hernández, Deborah Dultzin, Erika Benitez Instituto de Física: Rubén Alfaro Molina,
Varlen Grabski, Andres Sandoval Espinosa, Ernesto Belmont Moreno, Saul Aguilar Slazar Institudo de Ciencias Nucleares; Lukas Nellen, Gustaov Medina Tanco, Jaun Carlos D’Olivo Institudo de Geofísica:
José Valdés Galicia, Alejandro Lara, Rogelio Caballero Benemérita Universidad Autónoma de Puebla: Humberto Salazar
Ibarguen, Arturo Fernández, Caupatitzio Ramirez, Oscar Martínez, Eduardo Moreno Barbosa, Lorenzo Diaz, Alfonso Rosado
Universidad Autónoma de Chiapas: Cesar Álvarez Ochoa, Eli Santos Rodriguez, Roberto Arceo Reyes, Jorge Jara Jiménez
Universidad de Guadalajara: Eduardo de la Fuente, Enrique VelazquezUniversidad Michoacana de San Nicolás de Hidalgo: Luis Villaseñor,
Umberto Cotti, Juan Carlos Arteaga Velazquez, Pedro A. Miranda-Romagnoli, Roberto Noriega Papaqui, Eucario Gonzalo
Centrode Investigacion y de Estudios Avanzados: Arnulfo ZepedaUniversidad de Guanajuato: David Delepine, Gerardo Moreno, Edgar
Casimiro Linares, Marco Reyes, Luis Ureña, Mauro Napsuciale, Victor Migenes
CIC Instituto Politécnico Nacional: Jesus Martinez
USA: 16 institutions,
57 people
Mexico:15 institutions,
54 people
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11/2010
02/2012
08/2012
01/2013
05/2013
Important Dates13M USD project
funding began Feb 2011
Operations with 100 water Cherenkov detectors in Aug 2013
Observatory complete in Aug 2014
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HAWC on 4 Nov 2013
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DAQ, Analysis, & Archiving
VM
E B
ack
pla
ne
VM
E B
ack
pla
ne
Front EndBoards
CAENV1190TDC
128 PMTs
ReadoutComputer
Trigger andReconstruction
Client
Front EndBoards
CAENV1190TDC
128 PMTs
ReadoutComputer
Trigger andReconstruction
Client
Trigger andReconstruction
Client
Trigger andReconstruction
Client
Analysis, Monitoring,
Archiving
Raw Data500 MB/s
Triggered Data20 MB/s
x10
24 Hour Raw Data
50 TB
2 WeekTriggered Data
25 TB
1 WeekTriggered Data Portable Disk
• DAQ and Monitoring from off site with internet connection
• Reconstruction, analysis, and transient search performed on site
• Prompt receipt and notification of transients via internet to GCN, IAU, AMON, . . .
• Each week data is hand carried to Mexico City for transfer via internet to US (@ 50 MB/sec)
• 4 PB/year of data is archived in both US and Mexico
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We’re detecting Gamma Rays!
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• Operations began last summer with 1/3 of full detector
• HAWC Construction will be complete by the end of 2014
• Current work on calibration, reconstruction, and analysis algorithms is progressing well
• HAWC has detected known TeV sources of Crab, Mrk 421, and Mrk 501already
• New TeV sources coming soon!
Summary