Aldo Morselli, INFN, Sezione di Roma 2 & Università di...

Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 1


Aldo MorselliINFN, Sezione di Roma 2 &

Università di Roma TorVergata

Università di Padova10 Ottobre 2006

Search for DarkMatter in Space

with PAMELAand GLASTexperiments


Dark Matter really exist ? ΩΛ

Ωm


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


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.


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)


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


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


Proton spectra: Upper and lower bounds of due to the uncertainties of propagation parameters


Helium spectra: Upper and lower bounds of due to the uncertainties of propagation parameters


(Sc+Ti+V)/Fe Ratio that correspondsto the best fit of B/C;

Prim/Sec consistency check

DR uncertanty band DC uncertanty band


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]


Positron spectra



Antiproton spectra: Upper and lower bounds of due to the uncertainties of propagation parameters


MASS Matter Antimatter Space Spectrometer ( 89&91 )

Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 16MASS 89 flight

Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 17MASS 89 flight

Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 18MASS 89


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


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


PAMELA


Flight data: 0.171 GV positron

Flight data: 0.169 GV electron


Pamelain the cleanroom of RomaTor Vergata4/08/05


Pamelain Samara,Russia 4/09/05


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.


PAMELA @ Baikonur 28/03/06


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


Transport from Progress building to Launch Pad 13-6-2006


RESURSRESURSDK1DK1

SatelliteSatellite


PAMELA Launch 15/06/06


PAMELA Launch15/06/06


Flight data: 18 GV antiproton


Flight data: 1.56 GV Flight data: 1.56 GV positronpositron


PAMELA event



Flight data: ~500 GV electron ?


PAMELA event

Flight data: 14.4 GVnon-interacting proton


Flight data: 15 GVFlight data: 15 GVnon non interactinginteracting antiprotonantiproton


PAMELA event

Flight data: 36 GV interacting proton


PAMELA event

Flight data: 9.7 GVnon-interactingHelium Nucleus


PAMELA event

Flight data: 13 GV Interacting

Helium Nucleus


CalorimeterSelf-Trigger

Z = 15


Calorimeter Self-Trigger

Z = 16


e-

e+

p

Total detected energy in the calorimeter [MIP] versus rigidity [GV]

RR


e- e+ p

He

dE/dx in the calorimeter versus rigidity [GV]

RR

dE/dx


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 )


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


Positron spectra: PAMELA expectation for DC model

DRB

DC



Positron ratio: PAMELA expectation for DC model

DRB

DC



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


Antiproton Ratioand the best fitDC modelbackground withuncertainty band



PAMELA:Cosmic-Ray Antiparticle

Measurements: Antiprotons

fd: Clumpiness factors neededto disentangle a neutralinoinduced component in theantiproton flux


an example in mSUGRA

f = the dark matter fractionconcentrated in clumpsd = the overdensity due to aclump with respect to the localhalo density


PAMELA:Cosmic-RayAntiparticle

Measurements:Antiprotons

χ contributionbackgroundtotal

MSSM

fd: Clumpinessfactors needed todisentangle aneutralino inducedcomponent in theantiproton flux



tg(β)=55, sign(µ)=+1

YES

NOBackground

Signal

Signal and Background are separated ?mSUGRA

Signal

Background



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


PAMELA WIMP Detection SensitivitymSUGRA


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


larger valuesof tg(B) giveslarger signalsboth inantiprotonsand gammas



Sun


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


GLAST


Signal rate from Supersymmetry

governed by supersymmetric parameters

governed by halo distribution

gamma-ray flux from neutralino annihilation

J(ϕ):


~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


Moore: Nχ = 9 106



Mχ =80 GeV


The Galactic center


The Central Cusp of Stars -- mostly B stars

DM < 5% M_black hole insideS2 orbit

0.04 pc


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

Poin source locationfor GLAST~ 5 arcmin

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


Galactic Center: HESS

HESS Coll.Nature & astro-ph/0603021


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


Diffuse emission from the GC ridge


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!


EGRET data & Susy models

~2 degrees around the galactic center

EGRET data


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


Moore: Nχ = 9 106



~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


Moore: Nχ = 9 106



Mχ =80 GeV


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.


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


GLAST limits

no electroweaksymmetry breaking

WMAP 3allowed region (95% C.L)


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


35σ Sensitivity plot for for GLAST for a truncated (NFW) haloprofile tg(β)=55, sign(µ)=+1

equi neutralinomass curves

GLAST limits


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


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



LHC limits

LC1000 limits

LCC2

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 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




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


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)

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


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)


Where should we look for WIMPswith GLAST?

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


GLAST is on the trail of Dark Matter GLAST LAT Team


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


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


GLAST


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 ofview detectors sensitivities (AGILE, GLAST, Milagro, ARGO, AMS) are for 1 year of observation.

Sensitivity of γ-ray detectors

AMS trk

AMS Cal


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


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)

GLASTScheme

Gamma-RayLarge Area SpaceTelescope

GLAST @ SLAC

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

16/16 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


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


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.


• 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/


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)


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

• PAMELA inthe sky

• AGILEMar. 2007

Launch• GLAST:Sept. 2007

launch


add.slides


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


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


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


AGILE Main industrial contractors

• Carlo Gavazzi Space• Alcatel-AleniaSpazio -Laben• Oerlikon Contraves• Telespazio


AGILE @ BTF (Beam Test Facility inLNF -INFN, Frascati

( 20/11/05)

PSLV Polar Satellite LaunchVehicle :The AGILE Launcher from AntrixCorporation Limited


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/


Effective Area for the Galactic Center


GLAST Performance


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


Indirect Detection through Cosmic Rays


f = the dark matter fraction concentrated in clumps

d = the overdensity due to a clump with respect to the local halo density


> 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)

Aldo Morselli, INFN, Sezione di Roma 2 & Università di...

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