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Colliders To Cosmic Rays, Lake Tahoe February 25 – March 1, 2007

GLAST Large Area Telescope Overview Elliott Bloom SLAC - KIPAC Stanford University Representing the GLAST Collaboration. Colliders To Cosmic Rays, Lake Tahoe February 25 – March 1, 2007. Why study g ’s?. Large Area Telescope (LAT). spacecraft partner:. GLAST Burst Monitor (GBM).

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Colliders To Cosmic Rays, Lake Tahoe February 25 – March 1, 2007

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  1. GLAST Large Area Telescope Overview Elliott Bloom SLAC - KIPAC Stanford University Representing the GLAST Collaboration Colliders To Cosmic Rays, Lake Tahoe February 25 – March 1, 2007

  2. Why study g’s? Large Area Telescope (LAT) spacecraft partner: GLAST Burst Monitor (GBM) • g rays offer a direct view into Nature’s largest accelerators. • the Universe is mainly transparent to g rays with < 20 GeV that can probe cosmological volumes (z~700). Any opacity is energy-dependent for higher energy. • Most particle relics of the early universe produce g rays when they annihilate or decay. Two GLAST instruments: LAT: 20 MeV à300 GeV GBM: 10 keV à30 MeV Launch: Fall 2007 5-year mission (10-year goal) LEO @ 550km, ~26o

  3. Overview of LAT  Tracker Grid ACD e– e+ Calorimeter 16 towers-TKR+CAL+DAQ • Precision Si-strip Tracker (TKR) ~80 m2 Si, 18 XY tracking planes. Single-sided silicon strip detectors (228 mm pitch) Measure the photon direction; gamma ID. • Hodoscopic CsI Calorimeter(CAL) Array of 1536 CsI(Tl) crystals in 8 layers. Measure the photon energy; image the shower. • Segmented Anticoincidence Detector (ACD) 89 plastic scintillator tiles and 8 ribbons. Reject background of charged cosmic rays; segmentation removes self-veto effects at high energy. • Electronics System Includes flexible, robust hardware trigger and software filters in flight software. Systems work together to identify and measure the flux of cosmic gamma rays with energy 20 MeV - >300 GeV.

  4. GLAST MISSION ELEMENTS GLAST MISSION ELEMENTS Large Area Telescope & GBM m • sec GPS • - • Telemetry 1 kbps GLAST Spacecraft • TDRSS SN S & Ku DELTA 7920H • • S - - • GN • LAT Instrument Science Operations Center (SLAC) White Sands Schedules Mission Operations Center (MOC) GLAST Science Support Center HEASARC GSFC Archive Schedules GRB Coordinates Network GBM Instrument Operations Center Alerts Data, Command Loads

  5. GLAST LAT Collaboration Principal Investigator: Peter Michelson (Stanford & SLAC) ~225 Members (includes ~80 Affiliated Scientists, 23 Postdocs, and 32 Graduate Students) • France • IN2P3, CEA/Saclay • Italy • INFN, ASI • Japan • Hiroshima University • ISAS, RIKEN • Sweden • Royal Institute of Technology (KTH) • Stockholm University • United 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 • Ohio State University • Stanford University (SLAC and HEPL/Physics) • University of Washington • Washington University, St. Louis Cooperation between NASA and DOE, with key international contributions from France, Italy, Japan and Sweden. Managed at Stanford Linear Accelerator Center (SLAC).

  6. EGRET on CGRO firmly established the field of high-energy gamma-ray astrophysics and demonstrated the importance and potential of this energy band. GLAST is the next great step beyond EGRET, providing a leap in capabilities: Very large Field of View (FOV) (~20% of sky), factor 4 greater than EGRET Broadband (4 decades in energy, including the essentially unexplored region E > 10 GeV) Unprecedented Point Spread function (PSF) for gamma rays (factor > 3 better than EGRET for E>1 GeV). On axis >10 GeV, 68% containment < 0.12 degrees (7.2 arc-minutes) Large effective area (factor > 5 better than EGRET) Results in factor > 30 improvement in sensitivity below < 10 GeV, and >100 at higher energies. Much smaller deadtime per event (27 msec, factor ~4,000 better than EGRET - 0.1 s) No expendablesè long missionwithout degradation (5 year requirement , 10 year goal). GLAST LAT High Energy Capabilities

  7. Dramatic Improvement in Point Spread Function and Source Localization over EGRET EGRET source position error circles are ~0.5°, resulting in counterpart confusion. GLAST will provide much more accurate positions, with ~30 arcsec to ~5 arcmin localizations, depending on brightness. Cygnus region (15x15 deg)

  8. High energy source sensitivity: all-sky scan mode 100 sec During the all-sky survey, GLAST will have sufficient sensitivity after O(1) day to detect (5s) the weakest EGRET sources. EGRET Fluxes • - GRB940217 (100sec) • - PKS 1622-287 flare • - 3C279 flare • - Vela Pulsar • - Crab Pulsar • - 3EG 2020+40 (SNR g Cygni?) • - 3EG 1835+59 • - 3C279 lowest 5s detection • - 3EG 1911-2000 (AGN) • - Mrk 421 • - Weakest 5s EGRET source 1 orbit* 1 day^ *zenith-pointed ^“rocking” all-sky scan: alternating orbits point above/below the orbit plane

  9. GLAST addresses a broad science menu of interest to both the High Energy Particle Physics and High Energy Astrophysics communities. • Systems with super massive black holes & relativistic jets • Gamma-ray bursts (GRBs) • Pulsars • Origin of Cosmic Rays • Probing the era of galaxy formation • Discovery! Particle Dark Matter? Other relics from the Big Bang? Extra dimensions? New source classes? Recommended by the National Academy of Sciences in their 2000 decadal study as the highest priority mid-sized mission

  10. Gammas from lines γ γ c c ? ? c c γ Z0 time • For gg Line, energy = WIMP mass • For WIMP masses > MZ /2 can also have gZ0 line • Measurement of line branching fractions would constrain particle theory Branching fractions are in the range 10-2 - 10-4

  11. Where should we look for WIMPs with GLAST? • Galactic center • Galactic satellites • Galactic halo • Extra-galactic

  12. The Galaxy Shinning in High Energy Gammas from the Annihilation of Dark Matter

  13. http://glast.gsfc.nasa.gov/science/symposium/2007/program.htmlhttp://glast.gsfc.nasa.gov/science/symposium/2007/program.html

  14. GLAST LAT Mounted to Space Craft at General Dynamics in Gilbert, AZ. First communication with MOC on February 25, 2007.

  15. THE LOOK AHEAD • Major scientific conference, the First GLAST Symposium, held February 1-4, 2007 at Stanford University. • Observatory integration and test through late summer 2007. • Launch in late fall 2007… Science Operations begin within 60 days Fabrication Instrument & S/C I&T Launch Observatory I&T 2005 2006 2007

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