Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 1 DARK2007 Sydney, Sept 24 th -28 th , 2007 The Prospects for the Search for Dark Matter with GLAST Brian L. Winer The Ohio State University LAT Dark Matter and New Physics Working Group
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Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 1
DARK2007Sydney, Sept 24th-28th, 2007
The Prospects for the Search for Dark Matter with GLAST Brian L. WinerThe Ohio State UniversityLAT Dark Matter and New Physics Working Group
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 2
GLAST LAT CollaborationUnited States California State University at Sonoma University of California at Santa Cruz - Santa Cruz Institute of Particle Physics Goddard Space Flight Center – Laboratory for High Energy Astrophysics Naval Research Laboratory The Ohio State University Stanford University (SLAC and HEPL/Physics) University of Washington Washington University, St. LouisFrance IN2P3, CEA/SaclayItaly INFN, ASIJapanese GLAST Collaboration Hiroshima University ISAS, RIKENSwedish GLAST Collaboration Royal Institute of Technology (KTH) Stockholm University
PI: Peter MichelsonPI: Peter Michelson (Stanford & SLAC)
~225 Members (including ~80 Affiliated Scientists, plus 23 Postdocs, and 32 Graduate Students)
Cooperation between NASA and DOE, with key international contributions from France, Italy, Japan and Sweden.
Managed at Stanford Linear Accelerator Center (SLAC).
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 3
GLAST Burst Monitor (GBM) 5 keV - 25 MeV
Large Area Telescope (LAT)20 MeV - 300 GeV
GLAST is a NASA/DOE MissionLaunch: Feb-April 2008Lifetime: 5-years (10-years goal)Orbit: 565 km, circularInclination: 28.5o
GLAST is the next generation after EGRET… factor > 30 improvement in sensitivity
• Large effective area, factor > 5 better than EGRET
• Field of View ~20% of sky, factor 4 greater than EGRET
• Point Spread function factor > 3 better than EGRET for E>1 GeV. On axis >10 GeV, 68% containment < 0.12 degrees
• Smaller deadtime. Minimize rejection of E>10GeV gamma
rays due to backscatter into cosmic ray shield
No expendables (EGRET had spark chamber gas) - long mission without degradation (5-10 years)
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 4
e+ e– Calorimeter
Particle tracking detectors
Conversion foils
Anticoincidenceshield
Basics of a pair conversion telescopes
Basic structure of a pair conversion telescope
Tracker/converter (detection planes + high Z foils): photon conversion and reconstruction of the electron/positron tracks.
Calorimeter: energy measurement.
Anti-coincidence shield (ACD): backgound rejection (cosmic rays flux ~104 higher than the gamma flux).
Signature of a gamma event: No ACD signal 2 tracks (1 Vertex)* Calorimeter signal (~Energy)
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 5
Geometry Detail Over 45,000 volumes, and growing! Interaction Physics QED: derived from GEANT3 with extensions to higher and lower energies (alternate models available)
Hadronic: based on GEISHA (alternate models available)
Propagation Full treatment of multiple scattering Medium-dependent range cut-off Surface-to-surface ray tracing.
Includes information from actual LAT tests detailed instrument response dead channels noise etc.
Overall Deadtime Effects
F. Longo
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 8
Expected GLAST-LAT Performance
Angular resolution of better than 1 degree at energies > 1 GeV
Angular resolution of better than 0.2 degree at energies > 10 GeV
Better than 10% energy resolution for 100 MeV through 100 GeV
About 5% around 1 GeV
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 9
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 24
Galactic Halo Analysis
Use the large statistics of the full sky. Remove the Galactic Center (<10o) from consideration Consider a range of Neutralino Masses Perform a simulaneous fit to both the energy and spatial
distribution. Measure the sensitivity
to observing a signal. Mass vs < v> 1 year of running
A. Sander, R. Hughes, B. Winer
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 25
Sensitivity for Galactic Halo Analysis
<
v>
cm
3-s
-1
A. Sander, R. Hughes, B. Winer
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 26
Acknowledgements
E. Bloom, Y. Edmonds, P. Wang, L. Wai, J. Cohen-Tanugi(SLAC/KIPAC) I. Moskalenko (Stanford) A. Morselli, A. Lionetto (INFN Roma/Tor Vergata) E. Nuss (Montpellier) R. Hughes, A. Sander, B. Winer (Ohio State) L. Bergström, J. Edsjö, A. Sellerholm (Stockholm) A. Moiseev (Goddard)
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 27
Summary
Launch Early 2008! GLAST will shed light on the
multi-GeV EGRET data. The GLAST LAT team is
pursing complementary searches for signatures of particle dark matter. These analyses will continue
to be optimized over the next 4-6 months prior to launch.
We are looking forward to launch and adding a new piece to the puzzle of dark matter.
Brian L. Winer, Ohio State University GLAST DARK2007, University of Sydney Page 28
1st International GLAST symposium, Stanford, USA (Feb 2007)
L. Bergström, J.C., J. Edsjö, A. Sellerholm: Cosmological WIMPs
G. Bertone, T. Bringmann, R. Rando, A. Morselli : Point sources
A. Lionetto: mSUGRA and ED from the Galactic Centre A. Morselli, A. Lionetto, E. Nuss: Galactic Centre Y. Edmonds, E. Bloom, J. C. , J. Scargle, L. Wai: Line
sensitivity A. Sander, B. Winer, R. Hughes, L. Wai: Halo sensitivity L. Wai : Overview P. Wang, E. Bloom, L. Wai: Galactic Satellites