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

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

Aldo Morselli INFN, Sezione di Roma 2 &

Università di Roma Tor Vergata

16 - August 2004

Search for Dark Matter with GLAST

ICHEP'04 32nd International Conference on High Energy PhysicsAugust 16 - 22, 2004 Beijing, China


What is the Universe made of ?

Bright stars: 0.5% Baryons (total): 4.4% ± 0.4% Matter: 27% ± 4% Cold Dark Matter: 22.6% ± 4% Neutrinos: < 0.15% Dark Energy: 73% ± 6% h=0.71 + 0.04 - 0.03

WMAP+SN+HSTastro-ph/0302209

astro-ph 0007333

Dark Energy

CDM

BaryonsCold Dark Matter


Neutralino WIMPs

Assume present in the galactic halo• 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 ( annihilation) is aninteresting signature• ie: --> p + X• Produced from (e. g.) --> q / g / gauge boson / Higgs boson andsubsequent decay and/ or hadronisation.


Propagation Equation for Cosmic Rays in the Milky Way

convection velocity field that corresponds to galactic wind and it has a cylindrical symmetry, as the geometry of the galaxy. It’s z-component is the only one different from zero and increases linearly with the distance from the galactic plane

loss term: fragmentation

loss term: radioactive decay

diffusion coefficient is function of rigidity

diffusion coefficient in the impulse space,quasi-linear MHD:

primary spectra injection index

implemented in Galprop ( Strong & Moskalenko, available on the Web)


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 parameters changing; B/C are measured with the highest statistic

• Good fits of B/C experimental data constrain possible variations of the unknown parameters; + consistency wit the other prim/sec CR ratios

• Standard statistical test:

Heliospheric modulation z(depends on rigidity) (Perko,1997)


Enveloping curves ofall the good fits

of the experimental B/C data

DR: diffusion+

reacceleration

Dashed line:Best fit


Enveloping curves ofall the good fits

of the experimental B/C data

Dashed line: Best fit

DC: diffusion+convection

B/C ratio

In DC model problem with the ACE data at low energy

DC

DR


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 upperdiff indexdiff constanthalo size

prim specinjection index


Upper and lower bounds of positron spectra due to the uncertainties of

propagation parameters in the case of DR model

30% under 1GeV

25% around 1GeV

around 15% at 10GeV


Upper and lower bounds of antiproton spectra

due to the uncertainties of propagation

parameters in the case of DR model

from10% - 13%in all the

energy range


Prim/Sec consistency check

forDR model

Dashed: (Sc+Ti+V)/Fe spectra that

corresponds to the best fit of B/C;

enveloping curves of all fits that are

produced with good parameters

set


AMS98

Background from normal secondary production

Signal from 964 GeVneutralino annihilations (P.Ullio, astro-ph 9904086)

Mass91 data from XXVI ICRC, OG.1.1.21 , 1999

Caprice94 data from ApJ, 487, 415, 1997

Caprice98 data fromApJ, 561, (2001), 787. astro-ph/0103513

Distortion of the secondary antiproton flux induced by a signal from a heavy Higgsino-like neutralino.

Particles and photons are sensitive todifferent neutralinos. Gaugino-like particles are more likely to produce an observable flux of antiprotons whereas Higgsino-like annihilations are more likely to produce an observable gamma-ray signature

∆ BESS data from Phys.Rev.Lett, 2000, 84, 1078

AMS: Phys Rep 366 6 2002 331

BESS 00


MASS Matter Antimatter Space Spectrometer ( 89&91 )

TOFTRACKING SYSTEMTOFCALORIMETERGAS CHERENKOV1 mMAGNET


The CAPRICE 94 flight

Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 15MASS 89 flight

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


The PAMELAApparatus

Magnetic Magnetic spectrometespectrometerr

TRDTRD

CalorimeterCalorimeter

ToFToF

AnticoincidenceAnticoincidenceshieldshield

Shower tail catcher Shower tail catcher scintillatorscintillator

Neutron Detector


PAMELA StatusPAMELA StatusDetectors are ready and compling with the design performances

Detectors tested at PS / SPSTest facilities as Prototypes and in FM configuration

SPS, July 2000FMSPS, September 2003

Magnet/Tracker,CalorimeterSPS, July 2002

Integration of PAMELA FMunderway at INFN – Roma2


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


PAMELA Capabilities

PAMELA will explore:Antiproton flux 80 MeV - 190 GeVPositron flux 50 MeV – 270 GeVElectron flux up to 400 GeVProton flux up to 700 GeVElectron/positron flux up to 2 TeVLight nuclei (up to Z=6) up to 200 GeV/n

Antinuclei search (sensitivity of 10-7 in He/He)

more on PAMELA:

http://wizard.roma2.infn.it/


The PAMELA Launch is on February 2005 from Baikonur


PAMELAexpectations

for three years for

antiproton spectra for DR model

antiproton


PAMELAexpectations

for three years for positron

spectra for DC model


PAMELA: Cosmic-Ray Antiparticle Measurements: Antiprotons

Secondary production A.M.and V.Z. withGalprop, DC, Phi=550 Mv

Primary production from annihilation (m() ~ 1 TeV)Ullio 99

updated from P. Picozza and A. Morselli, astro-ph/0211286

Secondary productionSimon et al.

Secondary production A.M.and V.Z. withGalprop, DR, Phi=550 Mv


Signal rate from Supersymmetry

governed by supersymmetric parameters

governed by halo distribution

gamma-ray flux from neutralino annihilation

J():


EGRET, E > 1GeV

Mayer-Hasselwander et al, 1998


Poin source location for GLAST~ 5 arcmin

1 pixel ~ 5 arcmin

20 x 20 field IBIS/ISGRI 20–40 keV

Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 2920 x 20 field IBIS/ISGRI 20–40 keV1 pixel ~ 5 arcmin

Poin source location for GLAST~ 5 arcmin

20 x 20 field EGRET, E > 1GeV


EGRET data & Susy models

~2 degrees around the galactic center

EGRET data

Annihilation channel W+W-

M =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

N=8. 51 104 Typical N values:NFW: N = 104

Moore: N = 9 106

Isotermal: N = 3 101


GLAST: see Monica Pepe

talk


~2 degrees around the 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

N=8.51 104 Typical N values:NFW: N = 104

Moore: N = 9 106


Annihilation channel W+W-

M =80 GeV


region where

0.13 < CDMh< 1

GLAST sensitivity (5 ) for a neutralino density N of 104 in a=10-5 sr region around the galactic center

Minimal Supersymmetric Standard Model with:A0 = 0, > 0, mt =174 GeV

Typical N values for =10-5 sr :NFW: N = 104

Moore: N = 9 106


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

Estimated reaches with GLAST

region where

0.09 < CDMh< 0.13

if GLAST do not see Supersymmetrythis region is excluded for a NFW halo mh0 <114.3 GeV GeV


region where

0.13 < CDMh< 1

GLAST sensitivity (5 ) for a neutralino density N of 104 in a=10-5 sr region around the galactic center

Minimal Supersymmetric Standard Model with:A0 = 0, > 0, mt =174 GeV

Typical N values for =10-5 sr :NFW: N = 104

Moore: N = 9 106


Estimated reaches with GLAST

region where

0.09 < CDMh< 0.13

if GLAST do not see Supersymmetrythis region is excluded for a NFW halo mh0 <114.3 GeV GeV

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


Supersymmetry breaking


Mixed Anomaly mediated -gauge mediated model:

Tesi Alessandro Cesarini:http://people.roma2.infn.it/~glast/Glast_thesis.html


Acc.Bounds

Tachyons

No EWSB

region where

0.1 < CDMh< 0.3

GLAST sensitivity for a neutralino density N of 104 in a=10-5 sr region around the galactic center

AMSB-GMSB modelsix free parameters

Typical N values:NFW: N = 104

Moore: N = 9 106


Mixed Anomaly mediated -gauge mediated model:Test with GLAST

PRELIMIN

ARY


Cangaroo

Hess

Cangaroo consistent with ~ 2 TeV MHess > 12 TeV M

Whipple

HESS Coll.astro-ph/0408145


Conclusions

• GLAST will explore a good portionof the supersymmetric parameter space

… and this is only an additional item for GLAST !


GLAST will be an important step in gamma ray astronomy ( ~10 000 sources compared to ~ 200 of EGRET)

A partnership between High Energy Physics and Astrophysics

Beam test and software development well on the way

Wide range of possible answers/discoveries

Gold era for multiwavelenght studies

2nd Conclusions


Extra slides


MAGIC sensitivity based on the availabilityof high efficiency PMT’s

All sensitivities are at 5Cerenkov telescopes sensitivities(Veritas, MAGIC, Whipple, Hess, Celeste, Stacee, Hegra)are for 50 hours of observations.Large field of view detectors sensitivities (AGILE, GLAST, Milagro, ARGO, AMSare for 1 year of observation.

10-14

10-13

10-12

10-11

10-10

10-9

10-8

10-7

10-1

100

101

102

103

104

Photon Energy (GeV)

EGRET

GLAST

MILAGRO

ARGO

Crab Nebula

Past experiments Future experiments

Whipple

MAGIC

VERITAS

CELESTE, STACEE

Large field of View experiments

HEGRACerenkov detectors in operation

5 sigma, 50 hours, > 10 events

HESS

AGILE

Aldo Morselli 15/2/02

AMS

Sensitivity of -ray detectors

cal


Energy versus time for X and Gamma ray detectors


GLAST Performance


AMS CalAMS Trk

EGRET


Electron-Proton Separation (Calorimeter)

SPS TestBeam Data:p & e-

200 GeV/c


Differential yield for each annihilation channel

WIMP mass=200GeV

total yields

yields not due to 0decay


Differential yield

for b bar

neutralino mass


effective area distribution of observing time with inclination angle for the declination of the Galactic center. This is for a sky survey with +/-35 deg rocking and with the inclusion of the loss of exposure due to SAA (South Atlantic Anomaly) passages. The target direction was considered to be viewable if its zenith angle was no more than 105 deg. The fractions are for one precession period of the orbit (54.9 days). The main numbers are :Fraction of time in SAA: 0.142 Fraction of non-SAA time that source is not occulted: 0.592 Net fraction of time that source can be observed: 0.508 The figure divides this fraction into inclination angle ranges, the sum of all values is 1


Usual assumptions:ρDM=0.3GeV/cm3,β=10-3,

Truncated Maxwellian velocity,distributionvrms=270 /km s

vSun=220 km/s

?

αβα

ρρ

/)())/(1()/(

)()(

−+=

arar

rr c

From rotation curves

a =core radius of halo

αβ

Isothermal profile 2 2 0 =0 no cusp

Navarro-Frenk-White 1 3 1

Moore et al… 1.5 3 1.5

Kravtsov et al.(a) 2 3 0.2 Kravtsov et al.(b) 2 3 0.4

Distribution of Matter in Galaxy


J():

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