CF2 Instrumentation Jim Buckley for the CF2 working group M. Cahill-Rowley, R. Cotta, A. Drlica-Wagner, S. Funk, J. Hewett, A. Ismail, T. Rizzo and M. Wood (SLAC and Irvine Particle Theory groups)
Direct and Indirect Detection γ γ γ γ γ γ [hep-ph] arXiv:1011.4514 L. Bergstrom et al. Xenon100 Detector Proposed CTA SC camera module with 25 2” MAPMTs • Scientific complementarity • Technical complementarity Snowmass 2013 CF2: Indirect Detection James Buckley
CF2 Experiments γ γ γ γ γ γ Current and planned indirect detection experiments. Table 1-1. Status Experiment Target Location Major Support Comments Current AMS e + /e − , ISS NASA Magnet Spectrome- anti-nuclei ter, Running Fermi Photons, Satellite NASA, DOE Pair Telescope and e + /e − Calorimeter, Run- ning HESS Photons, Namibia German BMBF, Max Planck Society, Atmospheric e − French Ministry for Research, CNRS- Cherenkov IN2P3, UK PPARC, South Africa Telescope (ACT), Running IceCube/ Neutrinos Antarctica NSF, DOE, International *Belgium, Ice Cherenkov, DeepCore Germany, Japan, Sweden) Running MAGIC Photons, La Palma German BMBF and MPG, INFN, ACT, Running e + /e − WSwiss SNF, Spanish MICINN, CPAN, Bulgarian NSF, Academy of Finland, DFG, Polish MNiSzW PAMELA e + /e − Satellite VERITAS Photons, Arizona, DOE, NSF, SAO ACT, Running e + /e − USA e + /e − Planned CALET ISS Japan JAXA, Italy ASI, NASA Calorimeter CTA Photons ground- ACT International (MinCyT, CNEA, CONICET, based CNRS-INSU, CNRS-IN2P3, Irfu-CEA, ANR, (TBD) MPI, BMBF, DESY, Helmholtz Association, MIUR, NOVA, NWO, Poland, MICINN, CDTI, CPAN, Swedish Research Council, Royal Swedish Academy of Sciences, SNSF, Durham UK, NSF, DOE GAMMA- Photons Satellite Russian Space Agency, Russian Pair Telescope 400 Academy of Sciences, INFN GAPS Anti- Balloon NASA, JAXA TOF, X-ray and deuterons (LDB) Pion detection HAWC Photons, Sierra Ne- NSF/DOE Water Cherenkov, e + /e − gra Air Shower Surface Array PINGU Neutrinos Antarctica NSF Ice Cherenkov Snowmass 2013 CF2: Indirect Detection James Buckley
Indirect Detection γ γ γ γ γ γ Fermi VERITAS γ ν Super-K ICECUBE Super K e − , e + , p, ¯ p PAMELA AMS Snowmass 2013 CF2: Indirect Detection James Buckley
Gamma-Ray Detection γ γ γ γ γ γ • Both space-based and ground-based instruments use electromagnetic calorimeters, but for ground-based instruments the earth’s atmosphere is basically a continuous 27 rad. length total absorption calorimeter, viewed with an array of telescopes. Snowmass 2013 CF2: Indirect Detection James Buckley
VERITAS Array γ γ γ γ γ γ • First Light in April 2007 Snowmass 2013 CF2: Indirect Detection James Buckley
VERITAS Array γ γ γ γ γ γ • 10 mCrab sensitivity - 5 σ detection at 1% Crab (2x10 -13 erg cm -2 s -1 @ 1 TeV) in 28 hrs. • First Light in April 2007 • Effective area 10 5 m 2 above 500 GeV • Angular resolution <0.1 deg • Energy range 150 GeV - 30 TeV, 15% resolution (for spectral measurements) Snowmass 2013 CF2: Indirect Detection James Buckley
VERITAS Array γ γ γ γ γ γ • 10 mCrab sensitivity - 5 σ detection at 1% Crab (2x10 -13 erg cm -2 s -1 @ 1 TeV) in 28 hrs. • First Light in April 2007 • Effective area 10 5 m 2 above 500 GeV • Angular resolution <0.1 deg • Energy range 150 GeV - 30 TeV, 15% resolution (for spectral measurements) Snowmass 2013 CF2: Indirect Detection James Buckley
VERITAS Array γ γ γ γ γ γ • 10 mCrab sensitivity - 5 σ detection at 1% Crab (2x10 -13 erg cm -2 s -1 @ 1 TeV) in 28 hrs. • First Light in April 2007 • Effective area 10 5 m 2 above 500 GeV • Angular resolution <0.1 deg • Energy range 150 GeV - 30 TeV, 15% resolution (for spectral measurements) Snowmass 2013 CF2: Indirect Detection James Buckley
VERITAS Array γ γ γ γ γ γ • 10 mCrab sensitivity - 5 σ detection at 1% Crab (2x10 -13 erg cm -2 s -1 @ 1 TeV) in 28 hrs. • First Light in April 2007 • Effective area 10 5 m 2 above 500 GeV • Angular resolution <0.1 deg • Energy range 150 GeV - 30 TeV, 15% resolution (for spectral measurements) Snowmass 2013 CF2: Indirect Detection James Buckley
VERITAS Array γ γ γ γ γ γ • 10 mCrab sensitivity - 5 σ detection at 1% Crab (2x10 -13 erg cm -2 s -1 @ 1 TeV) in 28 hrs. • First Light in April 2007 • Effective area 10 5 m 2 above 500 GeV • Angular resolution <0.1 deg • Energy range 150 GeV - 30 TeV, 15% resolution (for spectral measurements) Snowmass 2013 CF2: Indirect Detection James Buckley
VERITAS Array γ γ γ γ γ γ • 10 mCrab sensitivity - 5 σ detection at 1% Crab (2x10 -13 erg cm -2 s -1 @ 1 TeV) in 28 hrs. • First Light in April 2007 • Effective area 10 5 m 2 above 500 GeV • Angular resolution <0.1 deg • Energy range 150 GeV - 30 TeV, 15% resolution (for spectral measurements) Snowmass 2013 CF2: Indirect Detection James Buckley
VERITAS Array γ γ γ γ γ γ • 10 mCrab sensitivity - 5 σ detection at 1% Crab (2x10 -13 erg cm -2 s -1 @ 1 TeV) in 28 hrs. • First Light in April 2007 • Effective area 10 5 m 2 above 500 GeV • Angular resolution <0.1 deg • Energy range 150 GeV - 30 TeV, 15% resolution (for spectral measurements) Snowmass 2013 CF2: Indirect Detection James Buckley
Technical Details γ γ γ γ γ γ Stage et al. 2006 Telescope (x 4) 12-m diameter Davies-Cotton f 1.0, 110 m2 area Snowmass 2013 CF2: Indirect Detection James Buckley
Technical Details γ γ γ γ γ γ Camera (x 4) 499 PMTs, 3.5 o FOV Stage et al. 2006 Telescope (x 4) 12-m diameter Davies-Cotton f 1.0, 110 m2 area Snowmass 2013 CF2: Indirect Detection James Buckley
Technical Details γ γ γ γ γ γ Camera (x 4) 499 PMTs, 3.5 o FOV Stage et al. 2006 Telescope (x 4) Mirror Facets (x 350) 12-m diameter Davies-Cotton Reflectivity ~ 88% f 1.0, 110 m2 area (Recoated every 2 years) Snowmass 2013 CF2: Indirect Detection James Buckley
Technical Details γ γ γ γ γ γ Camera (x 4) 499 PMTs, 3.5 o FOV Electronics Stage et al. 2006 500 Msp FADC, CFD trigger, 3-fold adjacent pixels and 2/4 telescope coincidence Telescope (x 4) Mirror Facets (x 350) 12-m diameter Davies-Cotton Reflectivity ~ 88% f 1.0, 110 m2 area (Recoated every 2 years) Snowmass 2013 CF2: Indirect Detection James Buckley
Technical Details γ γ γ γ γ γ Camera (x 4) 499 PMTs, 3.5 o FOV Electronics Stage et al. 2006 500 Msp FADC, CFD trigger, 3-fold adjacent pixels and 2/4 telescope coincidence Telescope (x 4) Mirror Facets (x 350) 12-m diameter Davies-Cotton Reflectivity ~ 88% f 1.0, 110 m2 area (Recoated every 2 years) Snowmass 2013 CF2: Indirect Detection James Buckley
Gamma-Ray Instruments γ γ γ γ γ γ Fermi (JB) Snowmass 2013 CF2: Indirect Detection James Buckley
Neutrino Detection γ γ γ γ γ γ (simulated neutrino event in ICECUBE) Snowmass 2013 CF2: Indirect Detection James Buckley
CTA-US γ γ γ γ γ γ ~2-3x improvement Fermi (3yr) in core energy range from US contribution Hybrid-1 (50 hr) Prod-1 Array I (50 hr) DC-MST (Single Mirror) SC-MST (Dual Mirror) 0.1° Hybrid-1 Hybrid-1 DC-MST SC-MST 0.03° 100 GeV 1 TeV Snowmass 2013 CF2: Indirect Detection James Buckley
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