GLAST LAT Project Graduate 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

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 2

GLAST Observatory : Timeline and Overview GLAST Observatory : Timeline and Overview

GLAST will measure the direction, energy and arrival time of celestial raysWill 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 DateAug 2007

GLAST Lifetime

5 years (min)

YOUR PhD

200X

GLAST will open

an energy window never explored before

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 3

Why Why rays ? 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

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 4

Science with GLASTScience 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 scalesEnergy range

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 5

LAT will Redefine the LAT will Redefine the Ray Sky Ray Sky

GLAST 1 yearGLAST 1 year

Source class Seen by EGRET

Predicted with

GLAST

Unidentified sources 170 ?

Rotation powered pulsars

3-6 100-500

Blazars 50-80 >2000

Normal galaxies 2 4-5

Gamma ray bursts 5 >500

Supernova Remnants/plerions

1-5 >10

Radio galaxies 1-1 ?

X ray binaries/microquasars

1-1 ?

Starburst galaxies 0 ?

Cluster of galaxies 0 ?

10 yrs of data recorded before GLAST !

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 6

Relativistic Outflows: AGN jetsRelativistic 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

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 7

Particle Acceleration: Origin of Cosmic RaysParticle 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 J1713.7-3946TeV 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+/-)

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 8

Clumpy haloes increase the signal of high energy rays !

Origin of Dark MatterOrigin 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 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…

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 9

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

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 10

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)

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 11

Do you want to do Science with GLAST?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, 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

Healey, Stephen E.

sehealey@stanford.edu

GLAST LAT Project Graduate Student Orientation, Sep 22 , 2005

E. do Couto e Silva 12

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…

LAT Construction ends

Early 2006

Thermal Vacuum Tests

First half of 2006

Spacecraft Integration

2006-2007

Launch DateAug 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