The VERITAS Indirect Dark Matter Program - KICP Workshops
The VERITAS Indirect Dark Matter Program - KICP Workshops
The VERITAS Indirect Dark Matter Program - KICP Workshops
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<strong>The</strong> <strong>VERITAS</strong> <strong>Indirect</strong> <strong>Dark</strong> <strong>Matter</strong> <strong>Program</strong><br />
Tuesday, July 17, 12<br />
Andrew W. Smith<br />
University of Utah
Support from:<br />
Smithsonian Inst.<br />
U.S. NSF<br />
U.S. DOE<br />
STFC (U.K.)<br />
NSERC (Canada)<br />
SFI (Ireland)<br />
Tuesday, July 17, 12<br />
<strong>VERITAS</strong><br />
<strong>The</strong> Very Energetic Radiation<br />
Imaging Telescope Array System<br />
-Mt. Hopkins, Az (1268 m a.s.l)<br />
Text<br />
U.S.! !<br />
Adler Planetarium Purdue Univ. of Iowa<br />
Argonne Nat. Lab SAO! Univ. of Massachusetts<br />
Barnard College UCLA! Univ. of Utah<br />
DePauw Univ. UCSC! Washington Univ.<br />
Grinnell College Univ. of Chicago<br />
Iowa St. Univ. Univ. of Delaware<br />
Canada Ireland!<br />
McGill Univ.! Cork Inst. Tech.<br />
! Galway-Mayo Inst.<br />
U.K. N.U.I. Galway<br />
Leeds U. UCD
Tuesday, July 17, 12<br />
Imaging Atmospheric<br />
Cherenkov Technique:<br />
Primary gamma rays<br />
initiate EM showers w<br />
particle v>c:<br />
Cherenkov pulses
<strong>VERITAS</strong><br />
* energy range: 100 GeV to >30 TeV (spectral reconstruction starts at 150 GeV)<br />
Tuesday, July 17, 12<br />
* energy resolution: 15% at 1 TeV<br />
* angular resolution:
<strong>The</strong> <strong>VERITAS</strong> Catalog<br />
Wide range of cosmic sources detected: pulsar wind nebulae, supernova<br />
Tuesday, July 17, 12<br />
remnants, X-ray binaries, many AGN, 1 starburst galaxy, 1 pulsar...
<strong>Indirect</strong> Detection of DM w/IACTs<br />
Assume all the
Target Advantages Disadvantages<br />
Galactic Center Close by, lots of DM Large
ON<br />
OFF<br />
Tuesday, July 17, 12<br />
<strong>VERITAS</strong> Galactic Center Observations<br />
UL Spectrum
<strong>VERITAS</strong> Observations of Fermi-LAT UIDs<br />
Tuesday, July 17, 12<br />
2 FGL J0312.8+2013<br />
10 hour observation<br />
no signal detected<br />
<strong>Program</strong> on-going. Further MW<br />
observations to be taken in<br />
2012/2013<br />
2 FGL J0746.0-0222<br />
9 hour observation<br />
Swift-XRT pointings
<strong>VERITAS</strong> Dwarf Spheroidal Observations<br />
Draco, WIllman I, Ursa Minor, Bootes I<br />
(Acciari et al. 2010, ApJ)<br />
-all ~15 hour observations<br />
No significant excess from any target<br />
NFW Profile used, 90% b-bar<br />
+ 10%
<strong>VERITAS</strong> Dwarf Spheroidal Observations<br />
Deep Observations (~50 hours) of Segue I<br />
(Aliu et al. 2012, Phys. Rev D)<br />
Constraints on low-velocity signal enhancement<br />
(Sommerfeld Boost)<br />
(Latanzi + Silk 2009) Model Arkani-Hamed et al 2009 Model<br />
Tuesday, July 17, 12
Constraints on DM explanation of<br />
Can use <strong>VERITAS</strong> muon model excl.<br />
curve to limit required “boost<br />
Tuesday, July 17, 12<br />
factor” in such models<br />
Pamela excess<br />
Bumps in Pamela/Fermi/HESS e+/e-<br />
data could be explained by leptophilic<br />
DM (annihilation exclusively into<br />
muons) (Bergstrom, Edsjo, Zaharijas,<br />
2009)
Works in Progress: DSph Stacking<br />
DSphs: (Published) Additional Time Taken Total Time<br />
Draco: (18 hours) 35 new hours 53 hours<br />
Ursa Minor (19 hours) 36 new hours 55 hours<br />
Segue I (48 hours) 38 new hours 86 hours<br />
DSph stacking can provide significant increase in<br />
Tuesday, July 17, 12<br />
sensitivity of limits
Expected Improvement<br />
Effective Area vs Energy Trigger Rate vs Energy<br />
Upgraded array will raise sensitivity significantly around 100 GeV (expected<br />
trigger threshold of 75 GeV): Provide marked sensitivity increase for DM<br />
Tuesday, July 17, 12<br />
continuum (and line!) searches.
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