1 GLAST The Gamma-ray Large Area Space Telescope Status of the Mission F.Longo see

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Presentation transcript:

1 GLAST The Gamma-ray Large Area Space Telescope Status of the Mission F.Longo see

2 Pulsars – rapidly spinning neutron stars with enormous magnetic and electric fields The Gamma-ray Sky in False Color – from EGRET/Compton Gamma Ray Observatory Milky Way – Gamma rays from powerful cosmic ray particles smashing into the tenuous gas between the stars. Blazars – supermassive black holes with huge jets of particles and radiation pointed right at Earth.  Gamma-ray bursts – extreme exploding stars or merging black holes or neutron stars. The Unknown – over half the sources seen by EGRET remain mysterious

3 Gamma-ray Sky Seen by EGRET on CGRO

4 GLAST One-year Simulated Observation red: GeV green: GeV blue: >1.6 GeV

5 Two GLAST instruments: –LAT: high energy (20 MeV – >300 GeV) –GBM: low energy (10 keV – 25 MeV) Huge field of view –LAT: 20% of the sky at any instant; in sky survey mode, expose all parts of sky for ~30 minutes every 3 hours. GBM: whole unocculted sky at any time. Huge energy range, including largely unexplored band 10 GeV GeV Large leap in all key capabilities, transforming our knowledge of the gamma-ray universe. Great discovery potential. Large Area Telescope (LAT) GLAST Burst Monitor (GBM) GLAST Key Features Spacecraft Partner: General Dynamics

6 The GLAST Observatory GBM Bismuth Germanate Detector GBM Sodium Iodide Detector LAT

7 e+e+ e–e–  GLAST LAT: A Telescope Without Lenses Precision Si-strip Tracker (TKR)Precision Si-strip Tracker (TKR) 70 m 2 of silicon detectors arranged in 36 planes. 880,000 channels. Hodoscopic CsI Calorimeter(CAL)Hodoscopic CsI Calorimeter(CAL) 1536 CsI(Tl) crystals in 8 layers, total mass 1.5 tons. Segmented Anticoincidence Detector (ACD)Segmented Anticoincidence Detector (ACD) 89 plastic scintillator tiles. Electronics SystemElectronics System Includes flexible hardware trigger and onboard computing. Calorimeter Tracker ACD [ surrounds 4x4 array of TKR towers]

8 GLAST LAT Collaboration France –IN2P3, CEA/Saclay Italy –INFN, ASI, INAF Japan –Hiroshima University –ISAS –RIKEN –Tokyo Institute of Science & Technology Sweden –Royal Institute of Technology (KTH) –Stockholm University United States –Stanford University (SLAC and HEPL/Physics) –University of California at Santa Cruz - Santa Cruz Institute for Particle Physics –Goddard Space Flight Center –Naval Research Laboratory –Sonoma State University –Ohio State University –University of Washington Principal Investigator: Peter Michelson (Stanford University) ~270 Members (~90 Affiliated Scientists, 37 Postdocs, and 48 Graduate Students) construction managed by Stanford Linear Accelerator Center (SLAC), Stanford University

9 GLAST Prior to Fairing Installation

10

11 GLAST Launch

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

13 Year 1 Science Operations Timeline Overview L AUNCH L +60 days week week week week month 12 m o n t h s spacecraft turn-on checkout LAT, GBM turn-on check out “first light” whole sky initial tuning/calibrations pointed + sky survey tuning Start Year 1 Science Ops Start Year 2 Science Ops in-depth instrument studies sky survey + ~weekly GRB repoints + extraordinary TOOs Release Flaring and Monitored Source Info GBM and LAT GRB Alerts continuous release of new photon data Observatory renaming GI Cycle 1 Funds Release Fellows Year 1 Start LAT 6-month high-confidence source release, GSSC science tools advance release GI Cycle 2 Proposals LAT Year 1 photon data release PLUS LAT Year 1 Catalog and Diffuse Model 2nd GLAST Symposium