GLAST LAT Project Graduate 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?Why gamma rays?

satellite

~ 500 km

centers of galaxiesemit 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 Observatory : Overview GLAST will measure the direction, energy and arrival time of celestial GLAST will measure the direction, energy and arrival time of celestial rays rays

Will follow on the measurements by its predecessor (EGRET) with unprecedented capabilities

LAT Principal Investigator: Peter MichelsonGBM 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 2006 - Sep 2007

Launch DateEnd 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 CatalogEGRET Source CatalogGLAST Survey: ~10,000 sources (2 years)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…The sky seen by GLAST…

GLAST LAT Simulations GLAST LAT Simulations

great for rotation student projects! great for rotation student projects!

and we have Terabytes of LAT data from pre-launch tests and we have Terabytes of LAT data from pre-launch tests including test beamincluding test beam

of several particles types and energies of several particles types and energies

Graduate Student Orientation Sep 21, 2006

E. do Couto e Silva SLAC/KIPAC

AGN (Blazars): Emission MechanismsAGN (Blazars): Emission Mechanisms

Most of the EGRET AGNs were Most of the EGRET AGNs were blazarsblazars• Variability: relativistic jetsVariability: relativistic jets• Jets point towards us !Jets point towards us !

Key issues to be addressedKey issues to be addressed• Energetics of the sourceEnergetics of the source• jet formationjet formation• jet collimationjet collimation• nature of the plasma nature 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 BurstsKey Issues in Gamma Ray Bursts

GRB OriginGRB Origin• Triggering mechanismTriggering mechanism

• Energy sourceEnergy source

• Jet productionJet production

GRB EvolutionGRB Evolution• Particle content of GRB Particle content of GRB

outflowoutflow

• Efficiency in energy Efficiency in energy transport and conversiontransport and conversion

• Role of B fieldsRole of B fields

• Nature of high energy Nature of high energy emissionsemissions

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?SNR: Sites of Hadronic Acceleration? Supernova Remnants: Supernova Remnants:

• by-products of Supernova explosionsby-products of Supernova explosions

• expected sites of galactic cosmic ray acceleration expected sites of galactic cosmic ray acceleration

• non-thermal emission (X-rays and non-thermal emission (X-rays and -rays)-rays) Measurements in the range of 100MeV-100GeV Measurements in the range of 100MeV-100GeV

• essential ingredient to resolve the origin (essential ingredient to resolve the origin (pp vs vs ee+/-)+/-)

Adapted from Aharonian’s talk at the Texas Symposium 2004

Question:Question:Do Do rays originate rays originate from hadronic or from hadronic or

leptonic processes?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?Origin of Dark Matter: a particle candidate?Dark matter halo z = 20z = 50

z = 5z = 10

z = 0z = 1

B. Moore, www.nbody.net

If true, there may well bephotons in the energy range probed

by GLAST

0214

0113

31211

01

~~~~HaHaWaBa

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…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…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 CollaborationGLAST LAT Collaboration FranceFrance

• IN2P3, CEA/SaclayIN2P3, CEA/Saclay

ItalyItaly• INFN, ASIINFN, ASI

JapanJapan• Hiroshima UniversityHiroshima University• ISAS, RIKENISAS, RIKEN

United StatesUnited States• California State University at SonomaCalifornia State University at Sonoma• University of California at Santa Cruz - Santa Cruz Institute of Particle Physics University 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

SwedenSweden• 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: Principal Investigator: Peter MichelsonPeter Michelson (Stanford & SLAC)

~225 Members (includes ~80 Affiliated Scientists, 23 Postdocs,

and 32 Graduate Students)

GLAST LAT Project Graduate Student Orientation, Sep 21 , 2006

E. do Couto e Silva 13

Do you want to do Science with GLAST?Do you want to do Science with GLAST?

SLACRESEARCH

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, Lawrence L.

waiwai@slac.stanford.edu@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

GLAST LAT Project Graduate Student Orientation, Sep 21 , 2006

E. do Couto e Silva 14

Do you want to do Science with GLAST?Do you want to do Science with GLAST?

Cohen-Tanugi, Johann

cohen@slac.stanford.edu

SLAC POST- DOCS

Wang, Ping

pingw@slac.stanford.edu

YOU

YOUR NAME

YOU@slac.stanford.edu

SLAC GRADUATE STUDENTS

Edmonds, Yvonne Vasetta

yedmonds@slac.stanford.edu

Paneque, David

dpaneque@slac.stanford.edu

Funk, Stefan

funk@slac.stanford.edu

Carson, Jennifer

carson@slac.stanford.edu

Bouvier, Aurelien

bouvier@slac.stanford.edu

Healey, Stephen E.

sehealey@stanford.edu

Lee, Shiu Hang (Herman)

shia520@slac.stanford.edu

GLAST LAT Project Graduate Student Orientation, Sep 21 , 2006

E. do Couto e Silva 15

Come talk to the GLAST Faculty !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…

Spacecraft Integration

Sep 2006- Sep 2007

Launch DateEnd 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 Project Graduate Student Orientation, Sep 21 , 2006

E. do Couto e Silva 16

See you soon…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 email !

– Location: 3rd floor Varian conference room

• Deadline to decide about joining GLAST @ SLAC : Oct 2, 2006 !– we will tell you who to contact when you come to the next

session