aldo morselli, infn, sezione di roma 2 & università di...
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 1
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 2
Aldo MorselliINFN, Sezione di Roma 2 &
Università di Roma TorVergata
Università di Padova10 Ottobre 2006
Search for DarkMatter in Space
with PAMELAand GLASTexperiments
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 3
Dark Matter really exist ? ΩΛ
Ωm
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 4
color image from the Magellan images of the merging cluster 1E0657−5 58
200 kpc
Chandra image of the cluster
weak lensing reconstruction
NEWS: Dark Matter really exist ? astro:ph/0608407
Due to the collision of two clusters, the dissipationless stellarcomponent and the fluid-likeX-ray emitting plasma are spatiallysegregated
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 5
Neutralino WIMPs
Assume χ present in the galactic halo• χ is its own antiparticle => can annihilate in galactic haloproducing gamma-rays, antiprotons, positrons….• Antimatter not produced in large quantities through standard processes(secondary production through p + p --> p + X)• So, any extra contribution from exotic sources (χ χ annihilation) is aninteresting signature• ie: χ χ --> p + X• Produced from (e. g.) χ χ --> q / g / gauge boson / Higgs boson andsubsequent decay and/ or hadronisation.
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 6
Propagation Equation for Cosmic Rays in the Milky Way
convection velocity field that correspondsto galactic wind and it has a cylindricalsymmetry, as the geometry of the galaxy.It’s z-component is the only one differentfrom zero and increases linearly with thedistance from the galactic plane
loss term: fragmentation
loss term: radioactive decay
diffusion coefficient is function of rigidity
diffusioncoefficient in theimpulse space,quasi-linear MHD:
primary spectra injection index
implemented in Galprop ( Strong & Moskalenko, available on the Web)
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 7
Enveloping curves ofall the good fits
of the experimentalB/C data
Dashed line: Best fit
B/C ratio
In DC model problem withthe ACE data at low energy
A.Lionetto, A.Morselli, V.ZdravkovicJCAP09(2005)010 astro-ph/0502406
DR: diffusion+ reaccelerationDC: diffusion+convection
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 8
Allowed values for the propagation parameters for DR propagation
Allowed values for the propagation parameters for DC propagation
halo size diffusion constant diff index Alfven velocity
injection indexesVc gradient diff indexdiff constanthalo size
prim specinjection index
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 9
Proton spectra: Upper and lower bounds of due to the uncertainties of propagation parameters
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 10
Helium spectra: Upper and lower bounds of due to the uncertainties of propagation parameters
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 11
(Sc+Ti+V)/Fe Ratio that correspondsto the best fit of B/C;
Prim/Sec consistency check
DR uncertanty band DC uncertanty band
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 12
Electron spectra
DRB
DC
DR
Local interstellar spectra
Top of the atmosphere spectra
DC
DRDRB
A.Lionetto, A.Morselli, V.ZdravkovicJCAP09(2005)010 [astro-ph/0502406]
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 13
Positron spectra
A.Lionetto, A.Morselli, V.ZdravkovicJCAP09(2005)010 [astro-ph/0502406]
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 14
Antiproton spectra: Upper and lower bounds of due to the uncertainties of propagation parameters
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 15
MASS Matter Antimatter Space Spectrometer ( 89&91 )
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 16MASS 89 flight
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 17MASS 89 flight
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 18MASS 89
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 19
PAMELA Payload for Antimatter Matter Exploration
and Light Nuclei Astrophysics
In orbit on June 15, 2006, on board of the DK1satellite by a Soyuz rocket from the Bajkonourlaunch site.From July 11 Pamela is in continuous datataking mode
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 20
Mass&Thermal ModelFull cycle of vibration/shock/tranport tests
Technological ModelPreliminary AcceptanceTests with EGSE: powerON/OFF, telecommands,data transmission
Flight ModelIntegration, beam tests;pre-flight operations
PAMELA models
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PAMELA
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Flight data: 0.171 GV positron
Flight data: 0.169 GV electron
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Pamelain the cleanroom of RomaTor Vergata4/08/05
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 25
Pamelain Samara,Russia 4/09/05
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 26
PAMELA scientific program
energy range particles/3 yearsAntiproton flux 80 MeV - 190 GeV >3 104
Positron flux 50 MeV – 270 GeV >3 105
Electron flux up to 400 GeV 6 106
Proton flux up to 700 GeV 3 108
Electron/positron flux up to 2 TeVLight Nuclei (up to Z=6) up to 200 GeV/n He/Be/C: 4 107/4/5
AntiNuclei search (sensitivity of 3 10-8 in He/He)
Unprecedented Statistics and new Energy Range in Cosmic RaysActual limits: antip&positrons ≈ 40 GeV
PAMELA is a magnetic spectrometer which will fly on a Russian satellite by Fall 2005.Its scientific scope is the measurement of the antiproton and positron spectra up to fewhundred GeV, of the proton and electron spectra up to 700 GeV and that of light nuclei.
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 27
PAMELA @ Baikonur 28/03/06
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PAMELA @ Baikonur 28/03/06
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 29
The Satellite: Resurs DK1- Soyuz-TM Launcher
from Baikonur- Launch in 2005- Lifetime >3 years- PAMELA mounted inside
a Pressurized Container,attached to Satellite
- Earth-Observation-Satellite
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Transport from Progress building to Launch Pad 13-6-2006
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RESURSRESURSDK1DK1
SatelliteSatellite
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PAMELA @ Baikonur 14/06/06
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PAMELA Launch 15/06/06
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 36
PAMELA Launch15/06/06
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 37
Flight data: 18 GV antiproton
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Flight data: 2.8 GV electron
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Flight data: 1.56 GV Flight data: 1.56 GV positronpositron
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PAMELA event
Flight data: 4.2 GV electron
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Flight data: ~500 GV electron ?
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PAMELA event
Flight data: 14.4 GVnon-interacting proton
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 43
Flight data: 15 GVFlight data: 15 GVnon non interactinginteracting antiprotonantiproton
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 44
PAMELA event
Flight data: 36 GV interacting proton
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 45
PAMELA event
Flight data: 9.7 GVnon-interactingHelium Nucleus
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 46
PAMELA event
Flight data: 13 GV Interacting
Helium Nucleus
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 47
CalorimeterSelf-Trigger
Z = 15
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 48
Calorimeter Self-Trigger
Z = 16
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 49
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 50
e-
e+
p
Total detected energy in the calorimeter [MIP] versus rigidity [GV]
RR
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 51
e- e+ p
He
dE/dx in the calorimeter versus rigidity [GV]
RR
dE/dx
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 52
PAMELA• In the period 11/07-26/09 PAMELA hascollected data for ~ 1475h, i.e. ~61 days for atotal of ~9x107 events with a G.F.~ 20 cm2 sr and ~70% efficiency•So up to Sept. 26 we have ~ 15 Caprice98 and2.8 HEAT-PBAR flights
~ 380 antiprotons (~80 between 10 and 190 GeVand 3800 positrons ( ~580 between 4.5 e 50 GeVand 2 between 50 e 190 GeV )
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 53
Antiprotons & Positrons
3344.5-50 GeV1035-16.4 GeV
~32300.05-270 GeV~5804.5-270 GeV
e+
Secondary fluxby Moskalenko &Strong
783-49 GeV2.4 cont. & 13 atm.
313-49 GeV1.8 cont. & 7 atm.
~3000.1-190 GeV~7810-190 GeV
pSecondary fluxby L. Bergstromusing C94 p flux
HEAT flightsCAPRICE98PAMELA
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 54
Positron spectra: PAMELA expectation for DC model
DRB
DC
A.Lionetto, A.Morselli, V.ZdravkovicJCAP09(2005)010 [astro-ph/0502406]
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 55
Positron ratio: PAMELA expectation for DC model
DRB
DC
A.Lionetto, A.Morselli, V.ZdravkovicJCAP09(2005)010 [astro-ph/0502406]
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 56
Antiproton spectra: Pamela expectation for Diffuse and Convection model in 3 yr
Antiproton spectra: PAMELA expectation for DC model
A.Lionetto, A.Morselli, V.Zdravkovic, JCAP09(2005)010
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 57
Antiproton Ratioand the best fitDC modelbackground withuncertainty band
A.Lionetto, A.Morselli, V.ZdravkovicJCAP09(2005)010 [astro-ph/0502406]
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 58
PAMELA:Cosmic-Ray Antiparticle
Measurements: Antiprotons
fd: Clumpiness factors neededto disentangle a neutralinoinduced component in theantiproton flux
A.Lionetto, A.Morselli, V.ZdravkovicJCAP09(2005)010 [astro-ph/0502406]
an example in mSUGRA
f = the dark matter fractionconcentrated in clumpsd = the overdensity due to aclump with respect to the localhalo density
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 59
PAMELA:Cosmic-RayAntiparticle
Measurements:Antiprotons
χ contributionbackgroundtotal
MSSM
fd: Clumpinessfactors needed todisentangle aneutralino inducedcomponent in theantiproton flux
A.Lionetto, A.Morselli, V.ZdravkovicJCAP09(2005)010 [astro-ph/0502406]
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 60
tg(β)=55, sign(µ)=+1
YES
NOBackground
Signal
Signal and Background are separated ?mSUGRA
Signal
Background
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 61
tg(β)=55, sign(µ)=+1
YES
NOBackground
Signal
Signal and Background are separated ?
YES
YES
YESYES YES
YES
YES
YES
YES
YESYES
YESYES
NO
NO
NO
NO
NO
NO
NONO
NO
NO
NONO
NO
Signal
Background
mSUGRA
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 62
tg(β)=55, sign(µ)=+1
YES
NOBackground
Signal
Signal and Background are separated ?
YES
YES
YESYES YES
YES
YES
YES
YES
YESYES
YESYES
NO
NO
NO
NO
NO
NO
NONO
NO
NO
NONO
NO
Signal
Background
mSUGRA
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 63
PAMELA WIMP Detection SensitivitymSUGRA
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 64
Antiproton spectra: Pamela expectation for Diffuse and Convection model in 3 yr
Antiproton spectra: PAMELA expectation for DC model
A.Lionetto, A.Morselli, V.Zdravkovic, JCAP09(2005)010
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 65
PAMELA WIMP Detection SensitivitymSUGRA
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 66
larger valuesof tg(B) giveslarger signalsboth inantiprotonsand gammas
PAMELA WIMP Detection SensitivitymSUGRA
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 68
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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 70
Signal rate from Supersymmetry
governed by supersymmetric parameters
governed by halo distribution
gamma-ray flux from neutralino annihilation
J(ϕ):
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 71
~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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 72
The Galactic center
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 73
The Central Cusp of Stars -- mostly B stars
DM < 5% M_black hole insideS2 orbit
0.04 pc
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 74
EGRET,E > 1GeV
Mayer-Hasselwanderet al, 1998
Integral data 20 x 20 field IBIS/ISGRI 20–40 keV
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 75
1 pixel ~ 5 arcmin
20 x 20 field IBIS/ISGRI 20–40 keV
Poin source locationfor GLAST~ 5 arcmin
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 7620 x 20 field IBIS/ISGRI 20–40 keV1 pixel ~ 5 arcmin
Poin source locationfor GLAST~ 5 arcmin
20 x 20 field EGRET, E > 1GeV
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 77
Galactic Center: HESS
HESS Coll.Nature & astro-ph/0603021
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 78
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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 79
Diffuse emission from the GC ridge
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 80
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!
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 81
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, Nuc. Phys. 113B (2002) 213 [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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 82
~2 degrees aroundthe galactic center,2 years data
(Galprop)(one example from DarkSusy)
GLAST Expectation & Susy models
A.Cesarini, F.Fucito, A.Lionetto, A.Morselli, P.Ullio, Astrop. Phys., 21, 267, 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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 83
Results of simulations for the mSUGRA point with parameters M1/2=420, M0=380, tanβ=53 GeV ( LCC4 point in Baltz et al (2006) )
mχ~ 170 GeV , Ωh2 = 0.114
Φ(Eγ>100 MeV) ~ 3 10-7 cm-2 s-1 in 300 × 300 Map (DarkSusy)
NFW - LCC4
GallDiffuse (GLAPROP)
1 Year operation
30 deg*30 deg count map obtained from GLAST simulations for a NFW profile with LCC4 mSUGRA parameters after one yearGLAST operation. This DM counts map has to be compared with the expected background as computed with the GALPROPcode (on the left)
The dark matter halo used for the GLAST indirect search sensitivityestimate is a truncated Navarro Frank and White (NFW) halo profile.
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 84
Differential spectra (GC centered)
DM signal
DM + Bkg
Bkg signal
DM Signal
Bkg signal
Resulting differential spectra from LCC4 and Background simulations for two regions (3degand 0.1deg radius) centered at the Galactic Centre.
3 deg. region,ΔΩ ~ 10-2 sr
0.1 deg. region,ΔΩ ~ 10-5 sr
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 85
GLAST limits
no electroweaksymmetry breaking
WMAP 3allowed region (95% C.L)
tg(β)=55, sign(µ)=+1
3σ Sensitivity plot for for GLAST for a truncated (NFW) halo profilemSUGRA
Sensitivityplot for 5yearsobservationof mSUGRAfor GLASTfor tg(b)=55.
GLAST 3σsensitivity isshown at theblue line andbelow fortruncatedNFW haloprofile
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 86
35σ Sensitivity plot for for GLAST for a truncated (NFW) haloprofile tg(β)=55, sign(µ)=+1
equi neutralinomass curves
GLAST limits
no electroweaksymmetry breaking
WMAP 3allowed region (95% C.L)
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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 87
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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 88
no electroweaksymmetry breaking
LHC limits
LC1000 limits
LCC2
mh0 < 114.3 GeVWMAP 33 σ allowed region
GLAST limits
tg(β)=10, sign(µ)=+1
LC500
Sensitivity plot for observation of mSUGRA for a number of acceleratorexperiments and GLAST for tg(β)=10. GLAST 5σ sensitivity is shown at the blueline and below a for truncated Navarro Frank and White (NFW) halo profile
LCC2 fromE.Baltz et al.hep-ph/0602187
mSUGRA
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 89
no electroweaksymmetry breaking
tg(β)=60, sign(µ)=+1
WMAP 35 σ allowed region
GLAST 5 σ limits
5 years of data
5σ Sensitivity plot for for GLAST for a truncated NFW halo profile mSUGRA
Sensitivityplot forobservationof mSUGRAfor GLASTfortg(β)=60.GLAST 5σsensitivity isshown at theblue line andbelow a fortruncatedNFW haloprofile
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 90
G.Isidoria and P.Paradisi hep-ph/0605012
large tgβ regionsfavoured in flavourphysics:
• suppression of B -> τν• sizable enhancement of (g-2)µ• small non-standard effects in ∆MBs and B(B→Xsγ)
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 91
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 92
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 93
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 94you need a factor ~ 10- 50 with respect to the “ standard” mSugra scenarioConclusion:
GLAST limitsfor clumpiness factor 10
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 95
Preliminary computation indicates that, in the energy rangeEγ > 5 GeV, GLAST could detect γ-rays from GC via LKPannihilations with moderate boost factors
Connection with ground based Cherenkov arrays (continuum and gamma ray lines) is needed to disantangle KK signal fromstandard astrophysical signal (~ E-2 spectra)
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 96
Where should we look for WIMPswith GLAST?
• Galactic center• Galactic satellites• Galactic halo• Extra-galactic
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 97
GLAST is on the trail of Dark Matter GLAST LAT Team
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 98
Example: dark matter satellite
Optimistic case:70 counts signal,
43 countsbackground within1.5 deg of clump
center
55-days GLAST in-orbit counts map (E>1GeV)
GalacticCenter
30-deglatitude
Larry Way et al. for the DM&NPWorking Group
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 99
The search for milky way halo substructure WIMPannihilations using the GLAST LAT
Dark matter calculationwith semi-analyticmethod of Taylor &Babul 2004, 2005
Background estimateusing EGRET above1GeV (sourcesubtracted)
M=100GeV <σ v> = 2.3x10-26cm3s-1
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 100
GLAST
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 101
Energy versus time for X and Gamma ray detectors
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 102
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 ofview detectors sensitivities (AGILE, GLAST, Milagro, ARGO, AMS) are for 1 year of observation.
Sensitivity of γ-ray detectors
AMS trk
AMS Cal
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 103
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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 104
Current GLAST Collaboration Science Groupsand their Coordinators
1a. Catalog Seth Digel (SU-SLAC); Isabelle Grenier (CEA/ Saclay)
1b. Diffuse (Galactic and Extragalactic) and Molecular Clouds Seth Digel (SU-SLAC); Isabelle Grenier (CEA/ Saclay)
2. Blazars and Other AGNs –Paolo Giommi (ASI), Benoit Lott (Bordeaux)
3. Pulsars, SNRs, and Plerions - Roger Romani (Stanford); David Thompson (GSFC)
4. Unidentified Sources, Population Studies, and Other Galaxies Patrizia Caraveo (IASF ); Olaf Reimer (Stanford)
5. Dark Matter and New Physics - Elliott Bloom (SU-SLAC); Aldo Morselli (INFN–Rome)
6. Gamma-Ray Bursts - Jay Norris (GSFC); Nicola Omodei (INFN-Pisa)
7. Solar System Sources - Gerry Share (NRL)
8. Calibration and Analysis Methods - William Atwood (UCSC); Steve Ritz (GSFC)
9. Multiwavelength Coordination Group – Roger Blandford (SU – KIPAC); David Thompson (GSFC)
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GLASTScheme
Gamma-RayLarge Area SpaceTelescope
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GLAST @ SLAC
12/16 Towers in the GRID on 7/10/05
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16/16 Towers in the GRID on 20/10/05
GLAST @ SLAC
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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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 109
Celebrations for the end of Tracker construction
52 attendees from INFN, ASI, SLAC, NASA,italian industrial partners
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 110
GLAST mission status
November 2005 ACD on the LAT
> All elements of the GLAST mission have completed the fabrication phase and are well into integration.
> LAT, GBM, and spacecraft assembly complete by mid 2006.
> Delivery of the instruments for observatory integration spring/summer 2006.
> Observatory integration and test summer 2006 through summer CY07.
Short term activities for the collaboration :
> Data Challenge 2 : March->May 2006
> Beam tests at CERN in summer/autumn 2006
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 111
09/10/06 : LAT Instrumentofficially accepted by NASA
• Well it is official! NASA formally accepted the LATInstrument today and has handed it over to GeneralDynamics for integration with the spacecraft. TheLAT Instrument, integrated and tested at SLAC, isthe culmination of years of planning and countlesshours of hard work from teams across the globe.The instrument has performed beautifully throughenvironmental tests and has exceeded itsperformance goals in many cases.
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 112
• August 2004Assembling of first tower completed
• Middle of October 2005Completion of the LAT – Environmental testing
• February 2006Delivery to NRL–
• September 2007Kennedy Space Flight Center LAUNCH
GLAST Master Schedule
•November 2007
Science operation begins!
more info : http://people.roma2.infn.it/glast/
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 113
Conclusion• from 15 June 2006 PAMELA is in the sky !• Will give strong constraints on propagation parameters.• Discovery Potential for Supersymmetry • September 2007 : GLAST will be launchedfrom Kennedy Space Flight Center• Complementary Discovery Potential for Supersymmetry • Both searches complementary to LHC and Direct Search
GLAST Symposium @ Stanford ( 1-2 Feb. 2007)
Roma Conference on Astroparticle ( 20-22 June 2007)
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 114
Through most of history, the cosmos has beenviewed as eternally tranquil
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 115
`
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
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Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 116
ExploringNature’s
Highest EnergyProcesses
• PAMELA inthe sky
• AGILEMar. 2007
Launch• GLAST:Sept. 2007
launch
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add.slides
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Propagation parameters uncertainties• Geometrical and dynamical parameters of the propagation• Pbar and Isotopes Production Cross Section ( ~ 20 % )• Gas distribution in the galaxy
• Secondary to primary CR ratios are the most sensitive quantities to parameterschanging; B/C are measured with the highest statistic
• Good fits of B/C experimental data constrain possible variations of the unknownparameters; + consistency wit the other prim/sec CR ratios
• Standard statistical test:
Heliospheric modulation z(depends on rigidity)
for uncertainties with another propagation code see:Donato F, Fornengo N, Maurin D, Salati P and Taillet R 2003 Phys. Rev. D 69 06350
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AGILE Mission• AGILE is an Scientific Mission supported by ASI (PhaseB:
June 1999) with scientific and programmatic participation byINAF and INFN dedicated to gamma-ray astrophysics
(Imaging 30 MeV-50 GeV, 10-40 keV)• Planned to be operational in 2006• Mission entirely dedicated to gamma-ray astrophysics (E>30
MeV) during the period 2006-2008• Emphasis to rapid reaction to transients• Multiwavelength follow-up program• Small Mission with a Guest Observer Program• Total satellite mass ~ 350 kg• Scientific Instrument mass: 120 kg
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The AGILE TEAMA. Argan, P.Caraveo, A. Chen, F. Gianotti, G. Ghirlanda, A. GiulianiS. Mereghetti, A. Pellizzoni, F.Perotti, M.Tavani (PI), S.VercelloneCNR-IASF, MilanoV.Cocco, T. Froysland, A.Morselli, P. Picozza, C. PittoriINFN, Sezione di Roma 2 andDipartimento di Fisica, Universita’ di Roma ''Tor Vergata'' G. Barbiellini (CoPi), F.Longo, G. Fedel, M.Prest, E.Vallazza INFN, Sezione di Trieste andDipartimento di Fisica, Universita’ di Trieste E. Costa, E. Del Monte, M. Feroci, E. Morelli, M. Rapisarda, A. Rubini, P. SoffittaCNR-IASF, RomaN. Auricchio, E. Celesti, G. Di Cocco, C. Labanti, E. Rossi, M. TrifoglioCNR-IASF, BolognaF.Boffelli, P.Cattaneo, F.MauriINFN, Sezione di PaviaP. Lipari, D. Zanello INFN, Sezione di Roma 1 andDipartimento di Fisica, Universita’ di Roma ''La Sapienza''
Tor Vergata
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AGILE Main industrial contractors
• Carlo Gavazzi Space• Alcatel-AleniaSpazio -Laben• Oerlikon Contraves• Telespazio
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AGILE @ BTF (Beam Test Facility inLNF -INFN, Frascati
( 20/11/05)
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AGILE @ BTF (Beam Test Facility inLNF -INFN, Frascati
( 20/11/05)
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PSLV Polar Satellite LaunchVehicle :The AGILE Launcher from AntrixCorporation Limited
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AGILE MissionSchedule• Payload completion: October 2005
• Instrument calibration at INFN-LNF-BTF: Nov. 2005
• P/L qualification & final testing by early Dec. 2005
• MITA spacecraft ready by Nov. 2005
• AGILE launch (PSLV) campaign: March-April 2007・ ・Start of AGILE scientific operations: summer 2007
more info: http://people.roma2.infn.it/agile/
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Effective Area for the Galactic Center
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GLAST Performance
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the method:
•We choose all the values of the parameters (Nb , Nχ) that satisfy the condition
we fixed Nb to the maximumvalue allowed by the abovecondition (when Nχ=0)The points indicate the regionswhere we can discriminate theneutralino signalwith GLAST at 5 sigma level intwo years.
backgroundneutralino signal
~2 degreesaround thegalactic center
background model(Galprop)
gamma from χ annihilation(one example from DarkSusy)
EGRET data
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Indirect Detection through Cosmic Rays
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f = the dark matter fraction concentrated in clumps
d = the overdensity due to a clump with respect to the local halo density
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> Whole sky 'realistic' simulation (Data Challenge2 Instrument Response Function)> One Year observations, 30 deg radius FOV Galactic Center centered
GLAST simulations
Dark Matter NFW profile,mB(1)~ 500 GeV
Diffuse background based onGALPROP code(Point source substracted)