GLAST LAT ProjectGraduate Student Orientation, Sep 21, 2006 E. do Couto e Silva 1 Gamma ray Large Area Space Telescope (GLAST) Eduardo do Couto e Silva SLAC Graduate Student Orientation – Sep 21, 2006 ~ 200 people

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC Why gamma 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

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC GLAST Observatory : 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 LAT Principal Investigator: Peter Michelson GBM Principal Investigator: Charles Meegan 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 Spacecraft Integration Sep Sep 2007 Launch Date End of 2007 GLAST Lifetime 5 years (min) YOUR PhD 200X GLAST will open an energy window never explored before

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC EGRET Source Catalog GLAST Survey: ~10,000 sources (2 years)

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC The sky seen by GLAST… GLAST LAT Simulations great for rotation student projects! and we have Terabytes of LAT data from pre-launch tests including test beam of several particles types and energies

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC AGN (Blazars): Emission Mechanisms  Most of the EGRET AGNs were blazars Variability: relativistic jetsVariability: relativistic jets Jets point towards us !Jets point towards us !  Key issues to be addressed Energetics of the sourceEnergetics of the source jet formationjet formation jet collimationjet collimation nature of the plasmanature of the plasma particle accelerationparticle acceleration radiation processesradiation processes (Buckley, Science, 1998)

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC Key Issues in Gamma Ray Bursts  GRB Origin Triggering mechanismTriggering mechanism Energy sourceEnergy source Jet productionJet production  GRB Evolution Particle content of GRB outflowParticle content of GRB outflow Efficiency in energy transport and conversionEfficiency in energy transport and conversion Role of B fieldsRole of B fields Nature of high energy emissionsNature of high energy emissions GLAST will…. place strong constraints on physical conditions within the source region (may include bursts from the first generation of stars)

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC SNR: Sites of Hadronic Acceleration?  Supernova Remnants: by-products of Supernova explosionsby-products of Supernova explosions expected sites of galactic cosmic ray accelerationexpected sites of galactic cosmic ray acceleration non-thermal emission (X-rays and  -rays)non-thermal emission (X-rays and  -rays)  Measurements in the range of 100MeV-100GeV essential ingredient to resolve the origin (p vs e+/-)essential ingredient to resolve the origin (p vs e+/-) Adapted from Aharonian’s talk at the Texas Symposium 2004 Question: Do  rays originate from hadronic or leptonic processes? LAT Energy Range

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC Clumpy haloes increase the signal of high energy  rays ! Origin of Dark Matter: a particle candidate? Dark matter halo z = 20z = 50 z = 5z = 10 z = 0z = 1 B. Moore, 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…

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC 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

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC 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)

Graduate Student Orientation Sep 21, 2006 E. do Couto e Silva SLAC/KIPAC GLAST LAT Collaboration  France IN2P3, CEA/SaclayIN2P3, CEA/Saclay  Italy INFN, ASIINFN, ASI  Japan Hiroshima UniversityHiroshima University ISAS, RIKENISAS, RIKEN  United States California State University at SonomaCalifornia State University at Sonoma University of California at Santa Cruz - Santa Cruz Institute of Particle PhysicsUniversity of California at Santa Cruz - Santa Cruz Institute of Particle Physics Goddard Space Flight Center – Laboratory for High Energy AstrophysicsGoddard Space Flight Center – Laboratory for High Energy Astrophysics Naval Research LaboratoryNaval Research Laboratory Ohio State UniversityOhio State University Stanford University (SLAC and HEPL/Physics)Stanford University (SLAC and HEPL/Physics) University of WashingtonUniversity of Washington Washington University, St. LouisWashington University, St. Louis  Sweden Royal Institute of Technology (KTH)Royal Institute of Technology (KTH) Stockholm UniversityStockholm University Cooperation between NASA and DOE, with key international contributions from France, Italy, Japan and Sweden. Managed at Stanford Linear Accelerator Center (SLAC). Principal Investigator: Peter Michelson Peter Michelson (Stanford & SLAC) ~225 Members (includes ~80 Affiliated Scientists, 23 Postdocs, and 32 Graduate Students)

GLAST LAT ProjectGraduate Student Orientation, Sep 21, 2006 E. do Couto e Silva 13 Do you want to do Science with GLAST? SLAC RESEARCH STAFF Cameron, Robert do Couto e Silva, Eduardo Digel, Seth Madejski, Grzegorz Tajima, Hiroyasu Wai, Lawrence L. Dubois, Richard Bloom, Elliott Blandford, Roger Kamae, Tsuneyoshi (Tune) Drell, Persis S. Romani, Roger Michelson, Peter FACULTY

GLAST LAT ProjectGraduate Student Orientation, Sep 21, 2006 E. do Couto e Silva 14 Do you want to do Science with GLAST? Cohen-Tanugi, Johann SLAC POST- DOCS Wang, Ping YOU YOUR NAME SLAC GRADUATE STUDENTS Edmonds, Yvonne Vasetta Paneque, David Funk, Stefan Carson, Jennifer Bouvier, Aurelien Healey, Stephen E. Lee, Shiu Hang (Herman)

GLAST LAT ProjectGraduate Student Orientation, Sep 21, 2006 E. do Couto e Silva 15 Come talk to the GLAST Faculty ! Bloom, Elliott Kamae, Tsuneyoshi (Tune) Drell, Persis S. Most of the SLAC Romani, Roger Michelson, Peter Most of the Stanford Campus Blandford, Roger Found everywhere… Spacecraft Integration Sep Sep 2007 Launch Date End of 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

GLAST LAT ProjectGraduate Student Orientation, Sep 21, 2006 E. do Couto e Silva 16 See you soon… This Friday –you will meet more GLAST colleagues from Campus and campus research staff –stay tuned ! Next Wednesday (Sep 27, 4 pm ) –Special GLAST Session with more details ! »we will remind you by ! –Location: 3 rd floor Varian conference room Deadline to decide about joining SLAC : Oct 2, 2006 ! –we will tell you who to contact when you come to the next session