1. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 1 Gamma ray Large Area Space Telescope (GLAST) Eduardo do Couto e Silva SLAC Graduate Student Orientation – Sep 22, 2005 ~ 200 people

2. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 2 GLAST Observatory : Timeline and Overview GLAST will measure the direction, energy and arrival time of celestial  rays Will follow on the measurements by its predecessor (EGRET) with unprecedented capabilities Large Area Telescope will record gamma-rays in the energy range ~ 20 MeV to >300 GeV GLAST Burst Monitor will provide correlative observations of transient events in the energy range ~10 keV – 25 MeV LAT Construction ends Early 2006 Thermal Vacuum Tests First half of 2006 Spacecraft Integration 2006-2007 Launch Date Aug 2007 GLAST Lifetime 5 years (min) YOUR PhD 200X GLAST will open an energy window never explored before

3. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 3 Why  rays ? satellite ~ 500 km centers of galaxies emit gamma rays  Universe is transparent to  rays  not affected by magnetic fields  probes early Universe most violent non-thermal processes found in Nature

4. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 4 Science with GLAST High Energy Sky Survey : –Unidentified EGRET sources and GLAST Source Catalog –unresolved point sources –Population Studies –To avoid peculiarities of individual sources (AGN, Pulsars, SNR…) –Diffuse Gamma ray emission –Galactic and Extragalactic –unresolved point sources –Physics of particle acceleration –Jets in Active Galactic Nuclei (AGN) –energy conversion –shocks in Supernova Remnants (SNR) –role of hadrons in radiation processes High-energy behaviour of transients : –Gamma Ray Bursts –Solar Flares Discovery Potential: –New classes of astrophysical objects –Origin of Extragalactic Background –Searches for Dark Matter and Extra Dimensions –Tests of Lorentz Invariance GLAST LAT strengths: All-sky monitoring Broad range of time scales Energy range

5. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 5 LAT will Redefine the  Ray Sky GLAST 1 year Source classSeen by EGRET Predicted with GLAST Unidentified sources170? Rotation powered pulsars3-6100-500 Blazars50-80>2000 Normal galaxies24-5 Gamma ray bursts5>500 Supernova Remnants/plerions 1-5>10 Radio galaxies1-1? X ray binaries/microquasars 1-1? Starburst galaxies0? Cluster of galaxies0? 10 yrs of data recorded before GLAST !

6. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 6 Relativistic Outflows: AGN jets Most  ray Jets from active galaxies are –Variable: relativistic jets –and point towards us ! Radiation is produced by one or more of the following processes –Synchrotron Self Compton –External Compton –Proton Induced Cascades –Proton Synchrotron Key issues to be addressed –Energetics of the source –jet formation –jet collimation –nature of the plasma –particle acceleration (Buckley, Science, 1998) Adapted from P. Coppi

7. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 7 Particle Acceleration: Origin of Cosmic Rays Supernova Remnants –sites of galactic cosmic ray acceleration Question –Do  rays originate from hadronic or leptonic processes? Supernova remnant RX J1713.7-3946 TeV  rays (color) keV X- rays (contours) GLAST e +/- model   model GLAST Uchiyama (2003) Adapted from Aharonian’s talk at the Texas Symposium 2004 Measurements in the range of 100 MeV to 100 GeV - essential ingredient to resolve the origin (p vs e+/-)

8. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 8 Clumpy haloes increase the signal of high energy  rays ! Origin of Dark Matter Milky Way Dark matter halo z = 20z = 50 z = 5z = 10 z = 0z = 1 B. Moore, www.nbody.net If true, there may well be photons in the energy range probed by GLAST q   q   Neutralino annihilations could create high energy  rays …. Neutralinos may not be the answer! The origin of Dark Matter may come from Extra Dimensions…

9. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 9 Graduate Student on GLAST today… typical graduate student… Data Analysis (is it an instrumental effect or a software bug?) Interpretation (understand how instrument works to get a better handle on the science) Final Explanation It’s fun to understand how a complex system works

10. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 10 It only gets better… Sharpen your knowledge of Science BEFORE Launch (2007) 2 yrs from now YOU will be the first to study one of the most exciting data sets Implement in simulations what YOU have learned (Data Challenges)

11. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 11 Do you want to do Science with GLAST? Cohen-Tanugi, Johann cohen@slac.stanford.edu POST- DOC Wang, Ping pingw@slac.stanford.edu YOU YOUR NAME YOU@slac.stanford.edu GRADUATE STUDENTS STAFF Cameron, Robert rac@slac.stanford.edu do Couto e Silva, Eduardo eduardo@slac.stanford.edu Digel, Seth digel@slac.stanford.edu Madejski, Grzegorz madejski@slac.stanford.edu Tajima, Hiroyasu htajima@slac.stanford.edu Wai, Lawrence L. wai@slac.stanford.edu Dubois, Richard richard@slac.stanford.edu Bloom, Elliott elliott@slac.stanford.edu Blandford, Roger rdb@slac.stanford.edu Kamae, Tsuneyoshi (Tune) kamae@slac.stanford.edu Drell, Persis S. persis@slac.stanford.edu Romani, Roger rwr@astro.stanford.edu Michelson, Peter peterm@stanford.edu FACULTY Healey, Stephen E. sehealey@stanford.edu

12. GLAST LAT ProjectGraduate Student Orientation, Sep 22, 2005 E. do Couto e Silva 12 Come talk to the GLAST Faculty ! Bloom, Elliott elliott@slac.stanford.edu Kamae, Tsuneyoshi (Tune) kamae@slac.stanford.edu Drell, Persis S. persis@slac.stanford.edu Most of the time @ SLAC Romani, Roger rwr@astro.stanford.edu Michelson, Peter peterm@stanford.edu Most of the time @ Stanford Campus Blandford, Roger rdb@slac.stanford.edu Found everywhere… LAT Construction ends Early 2006 Thermal Vacuum Tests First half of 2006 Spacecraft Integration 2006-2007 Launch Date Aug 2007 GLAST Lifetime 5 years (min) YOUR PhD 200X High Energy Sky Survey : –Unidentified EGRET sources and GLAST Source Catalog –unresolved point sources –Population Studies –To avoid peculiarities of individual sources (AGN, Pulsars, SNR…) –Diffuse Gamma ray emission –Galactic and Extragalactic –Unresolved point sources –Physics of particle acceleration –Jets in Active Galactic Nuclei (AGN) –energy conversion –shocks in Supernova remnants (SNR) –role of hadrons in radiation processes High-energy behaviour of transients : –Gamma Ray Bursts –Solar Flares Discovery Potential: –New classes of astrophysical objects –Origin of Extragalactic Background –Searches for Dark Matter and Extra Dimensions –Tests of Lorentz Invariance