GLAST and the future of High Energy Gamma-ray astrophysicsstatistics.roma2.infn.it/~morselli/GLAST_Morselli_Monteporzio_r.pdf · •Rivelatori su satellite - Rivelano il fotone primario

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 1 18 April 2008Aldo Morselli

INFN, Sezione di Roma 2 & Università di Roma Tor Vergata

GLAST and the future of HighEnergy Gamma-ray astrophysics

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 22

The CAPRICE 94flight


The TS93 and CAPRICE silicon-tungsten imaging calorimeter.

48 cm

48 cm


MASS 89


~1993

High Energy Gamma Experiments Experiments



GILDA


Elements of a pair-conversion telescope

• photons materialize into matter-antimatterpairs: Eγ --> me+c2 + me-c2

• electron and positron carry information about the direction, energy and polarization of the γ-ray

(energy measurement)

9Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected]

EGRETEGRET•Rivelatori su satellite- Rivelano il fotone primario- Anticoincidenza- Tracking detector- Calorimetro

Area Efficace

convoluzione dell’area geometricacon la efficienza di rivelazione

CARATTERISTICHE DI EGRETEγ Δ E/E Δθ (FWHM) Aeff (cm2)

(MeV) FWHM gradi100 26% 5.5 930500 20% 2 1570

1,000 19% 1.2 130010,000 26% 0.4 690

TE

NEA

)()(eff

!=


New Detector Technology• Silicon strip detector

Strip-shapedPN diode

50-500micron wide

300-500micron thick

VLSI amplifier

Stable particle tracker that allows micron-level tracking of gamma-rays

Well known technology in Particle Physics experiments.Used by our collaboration in balloon experiments (MASS, TS93, CAPRICE),on MIR Space Station ( SilEye) and on satellite (NINA)


Silicon Strip Detector Principle


Fractional energy loss for e+ and e- in lead

Photon total cross sectionsInteraction of electrons and photons with matter

Pair

0.9957

0.541

0.792

0.400.5

Prob Int.x/X0


MultipleMultipleScatteringScattering

0.01

0.1

1

10

0.1 1 10

0.15Xo(deg)0.07Xo(deg)0.05Xo(deg)

pro

ject

ed a

ngula

r dis

trib

uti

on (

deg

rees

)E(GeV)

0

1

2

3

4

5

6

0.1 1 10

0.15Xo(deg)0.07Xo(deg)0.05Xo(deg)

pro

ject

ed a

ngula

r dis

trib

uti

on (

deg

rees

)

E(GeV)

E(GeV)


EGRET(Spark Chamber) VS. GLAST(Silicon Strip Detector)

EGRET on Compton GRO(1991-2000)

GLAST Large Area Telescope(2006-2015)


GLAST Orbit


Gamma -ray mission deadtime


EGRET Superbowl Gamma Ray Burst




AGILE: inside the cube…

ANTICOINCIDENCE

HARD X-RAYIMAGER (SUPER-AGILE)

GAMMA-RAY IMAGER

SILICON TRACKER

(MINI) CALORIMETER


12 and 13 of June5th Science AGILE Workshop "AGILE's FIRST YEAR OF GAMMA-RAYASTROPHYSICS” 12-13 June, 2008ESRIN, Frascati

AGILE first 9 months


Overview of LATOverview of LAT•• Precision Si-strip Tracker (TKR) Precision Si-strip Tracker (TKR) ~80 m2

Si, 18 XY tracking planes. Single-sidedsilicon strip detectors (228 µm pitch)Measure the photon direction; gammaID.

•• Hodoscopic CsI Calorimeter(CAL)Hodoscopic CsI Calorimeter(CAL)Array of 1536 CsI(Tl) crystals in 8layers. Measure the photon energy;image the shower.

•• Segmented Anticoincidence DetectorSegmented Anticoincidence Detector(ACD)(ACD) 89 plastic scintillator tiles and 8ribbons. Reject background ofcharged cosmic rays; segmentationremoves self-veto effects at highenergy.

•• Electronics System Electronics System Includes flexible,robust hardware trigger and softwarefilters in flight software.

Systems work together to identify and measure the flux of cosmic gamma raysSystems work together to identify and measure the flux of cosmic gamma rayswith energy 20 MeV - >300 GeV.with energy 20 MeV - >300 GeV.

16 towers-TKR+CAL+DAQ

Tracker

Calorimeter

ThermalBlanket

AnticoincidenceShieldElectronics


GLASTScheme

Gamma-RayLarge Area SpaceTelescope


• http://people.roma2.infn.it/~aldo/GLASTpaperModel.pdf

GLAST paper ModelGLAST paper Model


The GLAST Participating InstitutionsAmerican Institutions SU-HEPL Stanford University, Hanson Experimental Physics Laboratory , , SU-SLAC Stanford Linear Accelerator Center, Particle Astrophysics group GSFC-NASA-LHEA Goddard Space Flight Center, Laboratory for High Energy Astrophysics NRL - U. S. Naval Research Laboratory, E. O. Hulburt Center for Space Research, X-ray and gamma-ray branches UCSC- SCIPP University of California at Santa Cruz, Santa Cruz Institute of Particle Physics SSU- California State University at Sonoma, Department of Physics & Astronomy , WUStL-Washington University, St. Louis UW- University of Washington , TAMUK- Texas A&M University-Kingsville, Ohio State UniversityItalian Institutions INFN - Istituto Nazionale di Fisica Nucleare and Univ. of Bari, Padova, Perugia, Pisa, Roma2, Trieste, Udine ASI - Italian Space Agency IASF- Milano, RomaJapanese Institutions University of Tokyo ICRR - Institute for Cosmic-Ray Research ISAS- Institute for Space and Astronautical Science Hiroshima UniversityFrench Institutions CEA/DAPNIA Commissariat à l'Energie Atomique, Département d'Astrophysique, de physique des Particules,

de physique Nucliaire et de l'Instrumentation Associée, CEA, Saclay IN2P3 Institut National de Physique Nucléaire et de Physique des Particules, IN2P3 IN2P3/LPNHE-X Laboratoire de Physique Nucléaire des Hautes Energies de l'École Polytechnique IN2P3/PCC Laboratoire de Physique Corpusculaire et Cosmologie, Collège de France IN2P3/CENBG Centre d'études nucléaires de Bordeaux Gradignan

IN2P3/LPTA Laboratoire de Physique Theorique et Astroparticules, MontpellierSwedish Institutions KTHRoyal Institute of Technology Stockholms Universitet Collaboration members: ~225

Members: 77Affiliated Sci. ~80Postdocs: 23Graduate Students 32


Tracker Production OverviewTracker Production Overview

Readout CablesUCSC, SLAC

SSD Procurement, TestingJapan, Italy, SLAC

Electronics Design,Fabrication & TestUCSC, SLAC (Teledyne)

Tracker ModuleAssembly and TestItaly

Tray Assembly andTestItaly (G&A, Mipot)

SSD Ladder AssemblyItaly (G&A, Mipot)

Composite Panel & ConvertersEngineering:SLAC, Italy (Hytec, COI)Procurement: Italy (Plyform)

2592

10,368

342

648

18

Module Structure (walls, flexures,thermal-gasket, fasteners)Engineering: SLAC, Italy (Hytec)Procurement: SLAC, Italy

342


Tray assembly in G&A

Tray positioning

Ladder positioning

Microbonding

•160 bare panels produced•100 tested and qualified for integrationwith ladders•completed trays for 3.3 towers•6 assembly chain ready•Max assembly rate : 3 trays/day/shift




228 µm


EncapsulationDam & Fill encapsulation

Dam Nusil 1142Fill Nusil 15-2500

Requirements:1. Height <0.5mm2. Lateral overflow <0.05mm3. Coverage of all the bondings and pads

Fast system to checkencapsulation height

228 µm pitch


Ladders testingLadders probe station: 5 probes are used to measure body and

single strip I, C to check sanity of each single channel

Flight ladders production status: Completed and tested (INFN BA/RM2/PG)

1900 Under construction 800 rejected ~ 1% 0.016% bad chans caused by bonding or

probing 2µm RMS alignment spread All results in good agreement with what

expected from SSDs

Depletion voltage

0

20

40

60

80

100

120

140

160

180

200

0

10

20

30

40

50

60

70

80

90

100

110

120

130

140

150

Depletion voltage (V)

Measured

Expected

Measured Expected

Average 65.888 65.759

Min 25 35

Max 115 117.5

RMS 18.788 17.765

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 32Tray Test at INFN Roma 2


Tray test at INFN

Stack of trays:• functional tests/CR burn-in for a whole tower in parallel• external trigger capability• 4 stacks operating in parallel at INFN (Pi/Pg/Rm2/Ba)


GLAST @ SLAC

12/16 Towers in the GRID on 7/10/05

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 3516/16 Towers in the GRID on 20/10/05

GLAST @ SLAC


The LAT Tracker numbers

11500 sensors11500 sensors360 trays360 trays18 towers18 towers

~ 1M channels~ 1M channels83 m83 m22 SiSi surface surface

> 240K functional test> 240K functional testrecorded in DBrecorded in DB

~ 30M strip tested~ 30M strip tested(30 test/strip on average)(30 test/strip on average)

> 60 physicist and engineers involved> 60 physicist and engineers involvedin the in the italianitalian teams from INFN teams from INFN

(Trieste, (Trieste, UdineUdine, , PadovaPadova, Pisa, , Pisa, PerugiaPerugia,,Roma2, Roma2, BariBari) in partnership with ASI) in partnership with ASI


Celebrations for the end of Tracker construction

52 attendees from INFN, ASI, SLAC, NASA,italian industrial partners


Both the LAT and GBMwere integrated to theSpacecraft at GeneralDynamics in Phoenix,Arizona.

the LAT and the NaIGBM modules mountedonto the spacecraft.

GLAST During Integration


Full sky simulation of GLAST Science

Catalogs

Diffuse Emission

AGN

Pulsars & SNRs

UIDs

Galaxies

Dark Matter

GRBs

Solar System Sources

Realistic 55 days (precession period) of LAT obs!Uncertainty in instrument response & background, + realistic science modelsSee: APOD May 31, 2006


LAT MC Derived Performancethick section

thin section

thick+thin sections

thin section

thick section

thick+thin sections

thin section

thick section


LAT Point Spread Function• Crucial aspect of analyses of DM subhalos and for disentangling point sources around the

galactic center.• LAT PSF depends strongly on many details, such as where the photon converts in the

Tracker, whether there is a measurement gap close to the conversion, the incidence angle,etc.

Example simulation ofphotons near normalincidence converting inthe thin section.

3.2° at 100 MeV

0.5° at 1 GeV

0.1° at 10 GeV

Remember, only ~1/2 ofthe effective are is in thethin section!

• Non-gaussian tails and mis-measured events are important.• LAT analyses generally make use of parameterizations of the “Instrument

Response Function” (IRF).

Gaussian tail Mismeasuredevents go out to90° or more!

Typically ×3


GLAST LAT Energy Resolution• Critical for detection of lines.• ΔE/E is roughly around 10%, but varies with energy and angle

– Impacted by leakage out the back, especially above 10 GeV– Improves at larger angle due to increasing thickness

• Not shown here are large non-Gaussian tails– Large gaps between calorimeter modules demand large corrections for some events,

especially near normal incidence.– Algorithms are biased toward avoiding over-correcting upwards, to avoid dangerous

large tails toward high energy.


EGRET (>100 MeV)Simulated LAT (>100 MeV, 1 yr)Simulated LAT (>1 GeV, 1 yr)

The Gamma-Ray Sky• Comparing EGRET to GLAST:

– Illustrating the anticipated improvement inour knowledge of the sky


Why studyWhy study γ γ’’s?s?– γ rays offer a direct view into Nature’s largest accelerators.– the Universe is mainly transparent to γ rays with < 20 GeV that can probe

cosmological volumes. Any opacity is energy-dependent for higher energy.– Most particle relics of the early universe produce γ rays when they annihilate or

decay.

Two GLAST instruments:LAT: 20 MeV 300 GeVGBM: 10 keV 30 MeVLaunch: December 20075-year mission (10-year goal)LEO @ 550km, ~26o

Large Area Telescope(LAT)

GLAST Burst Monitor(GBM)


Energy versus time for X and Gamma ray detectors


High galactic latitudes(Φb=2 10-5 γ cm-2 s-1 sr -1 (100 MeV/E)1.1). Cerenkov telescopes sensitivities (Veritas,MAGIC, Whipple, Hess, Celeste, Stacee, Hegra) are for 50 hours of observations.Large field of view detectorssensitivities (AGILE, GLAST, Milagro, ARGO, AMS) are for 1 year of observation.

Sensitivity of γ-ray detectors


EGRET on CGRO firmly established the field of high-energy gamma-ray astrophysicsand demonstrated the importance and potential of this energy band.

GLAST is the next great step beyond EGRET, providing a leap in capabilities:• Very large Field of View (FOV) (~20% of sky), factor 4 greater than EGRET

• Broadband (4 decades in energy, including the essentially unexplored region E > 10 GeV)

• Unprecedented Point Spread function (PSF) for gamma rays (factor > 3 better than EGRET for E>1GeV). On axis >10 GeV, 68% containment < 0.12 degrees (7.2 arc-minutes)

• Large effective area (factor > 5 better than EGRET)

•• Results in factor > 30 improvement in sensitivity below < 10 GeV, and >100 at higher energies.Results in factor > 30 improvement in sensitivity below < 10 GeV, and >100 at higher energies.

• Much smaller deadtime per event (27 µsec, factor ~4,000 better than EGRET - 0.1 s)

• No expendables long mission without degradation (5 year requirement , 10 year goal).

GLAST LAT High Energy CapabilitiesGLAST LAT High Energy Capabilities


GLAST addresses a broad science menu of interest toGLAST addresses a broad science menu of interest toboth the High Energy Particle Physics and High Energyboth the High Energy Particle Physics and High Energy

Astrophysics communities.Astrophysics communities.• Systems with (super-massive) black holes & relativistic jets

• Gamma-ray bursts (GRBs)

• Pulsars

• Origin of Cosmic Rays

• Probing the era of galaxy formation

• Discovery! Particle Dark Matter? Other relics from the Big Bang? Extra dimensions? New source classes?


Test of Quantum Gravity Test of Quantum Gravity (2)(2) Δt = ~ α E/EQG D/c

D ~ 2 1028 cm EQG ~1019 GeV c~3 1010 cm Δt(ms) ~ 60 ΔE(GeV)

E1

E2

E1

E2

Δti=0 Δtf=0t=ti

E1

E2

t=tf

E1

E2

even at pulsars distance: • D ~ 6 1021 cm Δt(µs) ~ 100 EQG ~1014 GeV


Violation of the Lorentz-Invariance?Violation of the Lorentz-Invariance?Light dispersion due to quantum gravity effects?Light dispersion due to quantum gravity effects?

Mrk 501, MAGIC, astro-ph/0702008

0.15-0.25 TeV

0.25-0.6 TeV

0.6-1.2 TeV

1.2-10 TeV 4 min lag

1st order

H.E.S.S.astro/ph:0706.0797PKS 2155−304


GRB studies with GLASTGRB studies with GLAST

EGRET observed delayed GeV emission from the GRB of February 17, 1994, including a 20 GeV photon that arrived 80 minutes after the burst began. GLAST will make the definitive measurements of the high-energy behaviour of GRBs and GRB afterglows.


GRB studies with GLAST GRB studies with GLAST (2)(2)

• Broad band spectral information: ~ 200 keV - 30 GeV• Rapid (few seconds) communication of GRB quicklook results• Single γ angular resolution ~10 arcmin at high energies for good source localization.

• Study of the initial impulsive phase: Δt< 1 ms

• Expected detection rate (above 50 MeV): 50-100 yr -1




Flux absorption due to the interaction with the infrared and microwave backgroundFlux absorption due to the interaction with the infrared and microwave background

γ ray source

Microwave and infrared background

Earth

Ε=ω2

γ

γ

e+

e-

Ε=ω1

ϑ

if the center of mass energy is:

photons interactions produce electron positron pairs


Energy density of the extragalactic diffuse background radiationEnergy density of the extragalactic diffuse background radiation

Hegra

Far Infrared Near Infrared

Average models

102

12.5 1.25 0.125125125012500 λ (µm)Characteristic absorbed γ ray energy (TeV): 110 0.1103 Eγ (TeV)

Dust Starlight

, astro/ph/9802308E2 n

(E) (

ev/c

m3 )


Transparency of the UniverseTransparency of the Universe

100 GeV

IR

radio

2.7 kOur galaxy

Super Cluster

γ γ e+ e-

p γ e+ e-

p γ π + π -Z~1 ~ 2 1028 cm

Z~0.03 ~2 1026 cm

E(eV)

Dist

ance

(mpc

)

1010 1012 1014 1016 1018 1020 1022 1024

10 TeV

10-3

10-2

10-1

100

101

102

103

104

105

(Mrk521)

Z~0.53, 2C279

Z~10-6 cm

Andromeda(700 kpc, 2.9Mly)LMC(50 kpc, 179kly)

Virgo Cluster 60mly, 18mpc


Flux absorption due to the interaction with the infrared and microwave background Flux absorption due to the interaction with the infrared and microwave background (2)(2)

Ε=ω1

γ

γ

e+

e-

Ε=ω2

ϑ ω1 and ω1 are respectively the energies of the low and the high energies gamma ray and ϑ is their angle of incidence.

The cross section of the process γγ −> e+e- is:

where re is the classical radius of the electron and:


Flux absorption due to the interaction with the infrared and microwave background Flux absorption due to the interaction with the infrared and microwave background (3)(3)

γ

γ

e+

e-

Ε=ω1

Ε=ω2

ϑ

the ratio between the flux I(L) at a distance L from the sourceand the initial flux I can be written as:

I(L)/Io=exp(-kγ L)where kγ is the absorption coefficient:

that contains the cross section and the low energy photon distribution.For the microwave spectrum:


Flux absorption due to the interactionFlux absorption due to the interactionwith the infrared and microwave backgroundwith the infrared and microwave background

an example on 3C279:• fixed background• different values of the Hubble constant

10-12

10-11

10-10

10-9

10-8

10-7

101

102

103

3C279

F(>

E)

cm

-2 s

-1

E(GeV)

Fb=1.52 10-3 E-2.55

Ho=100 km s -1 Mpc -1

Ho=75 km s -1 Mpc -1

Ho=50 km s -1 Mpc -1

F(>E

) cm

-2 s-1


V.Vitale, Journal Club8 March, Roma


Where should we look for WIMPswith GLAST?

• Galactic center• Galactic satellites• Galactic halo• Extra-galactic




EGRET data & Susy models

~2 degrees around the galactic center

EGRET data

Annihilation channel W+W-

Mχ =80.3 GeV

background model(Galprop)WIMP annihilation (DarkSusy)Total Contribution

A.Morselli, A. Lionetto, A. Cesarini, F. Fucito, P. Ullio, astro-ph/0211327

Nb=1.82 1021

Nχ=8. 51 104

Typical Nχ values:NFW: Nχ = 104

Moore: Nχ = 9 106

Isotermal: Nχ = 3 101


Signal rate from Supersymmetry

governed by supersymmetric parameters

governed by halo distribution

gamma-ray flux from neutralino annihilation

J(ϕ):


GLAST


~2 degrees aroundthe galactic center,2 years data

(Galprop)(one example from DarkSusy)

GLAST Expectation & Susy models

astro-ph/0305075A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astroparticle Physics, 21, 267-285, June 2004 [astro-ph/0305075]

Nb=1.82 1021

Nχ=8.51 104

Typical Nχ values:NFW: Nχ = 104

Moore: Nχ = 9 106

Isotermal: Nχ = 3 101

Annihilation channel W+W-

Mχ =80 GeV


EGRET,E > 1GeV

Mayer-Hasselwanderet al, 1998

Integral data 20 x 20 field IBIS/ISGRI 20–40 keV


1 pixel ~ 5 arcmin

20 x 20 field IBIS/ISGRI 20–40 keV

Point source locationfor GLAST~ 5 arcmin

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 7020 x 20 field IBIS/ISGRI 20–40 keV1 pixel ~ 5 arcmin

Point source locationfor GLAST~ 5 arcmin

20 x 20 field EGRET, E > 1GeV


Supersymmetry introduces free parameters:In the MSSM, with Grand Unification assumptions, the masses and couplings of theSUSY particles as well as their production cross sections, are entirely described once

5 parameters are fixed:

• M1/2 the common mass of supersymmetric partners of gauge fields (gauginos)

• m0 the common mass for scalar fermions at the GUT scale

• µ the higgs mixing parameters that appears in the neutralino and chargino mass matrices

• A is the proportionality factor between the supersymmetry breaking trilinear couplings and theYukawa couplings

• tang β = v2 / v1 = <H2> / <H1> the ratio between the two vacuum expectation values of the Higgs fields


tg(β)=55, sign(µ)=+1

YES

NOBackground

Signal

Signal and Background are separated ?mSUGRA

Signal

Background


Signal

no electroweaksymmetry breaking

tg(β)=55, sign(µ)=+1Signal and Background are separated ?

NO

Background

YESNO

YES

YESYES

YES

YES

YES

YES

YES

YESYES YES

NONO

NO

NO

NO

NO NO

NO

NO

NO

NO

NO

NO

cMSSM


Signal

no elecroweaksymmetry breaking

tg(β)=55, sign(µ)=+1Signal and Background are separated ?

NO

Background

YESNO

YES

YESYES

YES

YES

YES

YES

YES

YESYES YES

NONO

NO

NO

NO

NO NO

NO

NO

NO

NO

NO

NO

cMSSM


GLAST limits


WMAP 33σ allowed region


mSUGRA

Sensitivityplot for 5yearsobservationof mSUGRAfor GLASTfor tg(b)=55.

GLAST 3σsensitivity isshown at theblue line andbelow fortruncatedNFW haloprofile

3σ Sensitivity plot for for GLAST for a truncated (NFW) halo profile


3σ Sensitivity plot for for GLAST for a truncated (NFW) halo profiletg(β)=55, sign(µ)=+1

equi neutralinomass curves

GLAST limits


WMAP 33σ allowed region

mχ=400 GeV

mχ=200 GeV

mχ=300 GeV

mSUGRA

Sensitivityplot for 5yearsobservationof mSUGRAfor GLASTfor tg(b)=55.

GLAST 3σsensitivity isshown at theblue line andbelow fortruncatedNFW haloprofile


LHC limits 100 fb-1

LC500

GLAST limitsLC1000 limits

PAMELA Limitsboost factor 10

accelerator limits@ 100 fb-1 from H.Baer et al.,hep-ph/0405210

GLAST, PAMELA, LHC, LC Sensitivities to Dark Matter SearchmSUGRASensitivity plotfor 5 yearsobservation ofmSUGRA forGLAST fortg(b)=55and for otherexperiments.GLAST 3σsensitivity isshown at theblue line andbelow fortruncated NFWhalo profile


accelerator limits@ 100 fb-1 from H.Baer et al.,hep-ph/0405210

GLAST, PAMELA, LHC, LC Sensitivities to Dark Matter SearchmSUGRASensitivity plotfor 5 yearsobservation ofmSUGRA forGLAST fortg(b)=55and for otherexperiments.GLAST 3σsensitivity isshown at theblue line andbelow fortruncated NFWhalo profile



LHC limits

LC1000 limits

mh0 < 114.3 GeVWMAP 33 σ allowed region

GLAST limits


LC500

Sensitivity plot for observation of mSUGRA for a number of acceleratorexperiments and GLAST for tg(β)=10. GLAST 3σ sensitivity is shown at the blueline and below a for truncated Navarro Frank and White (NFW) halo profile

mSUGRA




WMAP 33 σ allowed region

GLAST 3 σ limits

5 years of data

Sensitivity plot for GLAST for a truncated NFW halo profile mSUGRA

Sensitivityplot forobservationof mSUGRAfor GLASTfortg(β)=60.GLAST 3σsensitivity isshown at theblue line andbelow fortruncatedNFW haloprofile


Model independent results for the GC• Assume a truncated NFW profile • Assume a dominant annihilationchannel(good assumption except for τ+ τ- )

Differential yieldfor eachannihilationchannel

WIMP mass=200GeV

figure from: A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio,Astroparticle Physics, 21, 267-285, June 2004 [astro-ph/0305075]


Galactic Diffuse in the CentralGalaxyGalprop Conventional Galprop Optimized

IC

IC

brems bremsEG EG

totaltotal

EGRET EGRETCOMPTEL COMPTEL

Strong et al. 2007, Ann.Rev. 57 (astro-ph/0701517)

π0 π0

These two models exemplify (but probably do not encompass) the range of uncertaintyin the diffuse background prediction. Since the IC and π0 contributions are different inshape, the shape of the total can be adjusted significantly without violatingindependent astrophysical constraints.

Inverse Compton candominate at high E!


Model independent results for the GC5 years ofoperations,truncatedNFW


Model independent results for the GC5 years of operations,truncated NFW


Model independent results for the GC5 years ofoperations,truncatedNFW


Model independent results for the Sagittarius

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 87CAPE CANAVERAL, Fla.04/03/2008 --- On Pad 17-B at Cape Canaveral Air Force Station in Florida, United Launch Alliance technicians checkthe list of activities completed on the mating of the nine solid rocket boosters to the Delta II rocket for the launch of GLAST.

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 8804/03/2008 CAPE CANAVERAL, On Pad 17-B the Delta IIrocket for GLAST


• August 2004Assembling of first tower completed

• Middle of October 2005Completion of the LAT – Environmental testing

• February 2006Delivery to NRL–

• 31 Jan. 2008Kennedy Space Flight Center 16 May

LAUNCH

GLAST Master Schedule

•June 2008

Science operation begins!

more info : http://people.roma2.infn.it/glast/


GLAST Current Schedule Ahead• 1st Stage Launch Vehicle on Stand March 18• Complete S/C integration April 2• Mission Readiness Review April 22• Complete observatory testing April 25• Fuel Spacecraft April 29• Move observatory to SLC-17b May 1• Flight Readiness Review May 12• Launch Readiness Review May 15• Mission briefing for invited guests at the KSC Visitor Complex May 15• Launch** May 16• LAT Turn On L+14• LAT First Light L+19• Complete On-orbit C/O L+60

** two-hour window each day, starting at 11:45AM


• Mission: GLAST (Gamma-ray Large Area Space Telescope)• Location: Astrotech payload processing facility• Launch Vehicle: Delta II 7920-H Launch Pad: 17-B• Launch Date: May 16, 2008• Launch Window: 11:45 a.m. - 1:40 p.m. EDT At Pad 17-B on Cape

Canaveral Air Force Station, the Delta II first stage and nine solid rocketboosters have been erected. During preparations to hoist the second stageatop the first stage, an incident occurred which caused an adapter beamassociated with the lifting operation to fracture. As a result, the stackingoperation was immediately stopped. A team has been appointed toinvestigate the incident. Once the team has concluded its investigation and isable to determine there was no damage to the second stage, a new date forstacking will be set, possibly as early as next week.


Conclusion

GLAST launch is currentlyscheduled for May. 162008.･ Guest InvestigatorProgram Proposals

http://glast.gsfc.nasa.gov/ssc/proposals/GI_Program_Background.html


Summary• GLAST, together with the other gamma-ray

observatories, will address many important questions:– How do Nature’s most powerful accelerators work?– What are the unidentified sources found by EGRET?– What is the origin of the diffuse background?– What is the origin of cosmic rays?– What is the high energy behavior of gamma ray bursts?– When did galaxies form?– What else out there is shining gamma rays? New sources (e.g., galaxy

clusters)? Are there high-energy relics from the Big Bang? Are therefurther surprises in the poorly-measured energy region?

• Huge leap in key capabilities enables large menu of known exciting science andlarge discovery potential.

• Part of the bigger picture of experiments at the interface between particlephysics and astrophysics.

Much to do Much to do ‒‒ join the fun!! join the fun!!


Through most of history, the cosmos has beenviewed as eternally tranquil


`

During the 20th century the quest to broaden our view of theuniverse has shown us the vastness of the Universe andrevealed violent cosmic phenomena and mysteries


ExploringNature’s

Highest EnergyProcesses

• PAMELAJune 2006Launched• AGILE

Apr. 2007Launched• GLAST:May. 2008

launch


IMBH mini-spikes observation prediction


IMBH mini-spikes observation prediction

G. Bertone, T. Bringmann, R. Rando, G. Busetto, A. Morselli astro-ph/0612387

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5 σ , 55 days

tenths of sources with novariability, no counter partand similar spectrum.Possible smoking gun ?

159/200 simulatedskymaps that do notviolate EGRET limits

number of observed mini-spikes


ConclusionDiscovery Potential for Supersymmetry

• GLAST will explore a good portionof the supersymmetric parameter space

• Search complementary to antimatter,

LHC and Direct Search


add. slides

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 101G. Bertone, T. Bringmann, R. Rando, G. Busetto, A. Morselli astro-ph/0612387

EGRET’sfaintestdetectedsource

DM point sources in the sky for mχ=150 GeVintense diffusegamma-raybackground(in the galactic plane)

obs.time: 2 months obs.time: 2 months

for a 150 GeV mass we can estimate the mass of the DM particle with a precision of 25 GeV (10% @ 1TeV)


minimum flux above 100 MeV, in units of [ph m-2 s-1 ]

G. Bertone, T. Bringmann, R. Rando, G. Busetto, A. Morselli astro-ph/0612387

DM particle with mass mχ = 150 GeV annihilating into b bar, after a 2 monthsobservation period

GLAST sensitivity map for the detection ofpoint sources of Dark Matter annihilation

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 103G. Bertone, T. Bringmann, R. Rando, G. Busetto, A. Morselli astro-ph/0612387

minimum flux above 100 MeV, in units of [ph m-2 s-1 ]

DM particle with mass mχ = 150 GeV annihilating into b bar, after a 2 monthsobservation period

GLAST sensitivity map for the identificationof point sources of Dark Matter annihilation


how to discriminate a DM from a mereastrophysical origin of gamma-ray point sources ?

• The GLAST LAT is expected to observemore than a hundred of Active Galactic Nuclei(AGNs) in ~ 2 months, some of which would,due to EBL attenuation, feature a spectralsignature similar to that of DM annihilations.However, a population of DM sources wouldexhibit distinctive features that should allowto discrminate the from AGNs, such as thelow energy spectral index of ~ 1.5 and theabsence of variability


Galactic CenterHESS SpectrumUnbroken power-law.

Hard spectrum Γ = 2.2.No evidence for variability on

a variety of time scales.

Consistent withSGR A* to 6’’ and slightly extended.

SGR A

Good agreementbetween HESS andMAGIC (large zenithangle observation).

astro-ph/0512469


EGRET, GLAST, HESS

it might still bethat a DMcomponent could besingled out, e.g. theEGRET source (?):a DM source can fitthe EGRET data;GLAST woulddetect its spectraland angularsignatures andidentify withoutambiguity such DMsource!


This talk

SeeE.Nusstalk


Model independent results for the GC


Exluded byHESS & MAGIC


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