Current GLAST related DM work - Istituto Nazionale 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 Tor Vergata

Current GLAST related DM work

SLAC11 June 2005


the PDF file of the book of Proceedings are in :

http://www.roma2.infn.it/iwfs04/iwfs.html

slides in : http://www.fisica.uniud.it/~glast/GammaWorkshop/

Past Activities:


G.Bertone chair


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: fragmentationloss 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)


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)


Enveloping curves ofall the good fits

of the experimentalB/C data

Dashed line: Best fit

DR: diffusion+ reaccelerationDC: diffusion+convection

B/C ratio

In DC model problem withthe ACE data at low energy

DC

DR

A.Lionetto, A.M, V.Zdravkovicastro-ph/0502406, 21 Feb. 05


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


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



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



Positron spectra: PAMELA expectation for DC model

DRB

DC

A.Lionetto, A.M, V.Zdravkovicastro-ph/0502406


Antiproton spectra: Pamela expectation for Diffuse and Convection model

Antiproton spectra: PAMELA expectation for DC model



PAMELA:Cosmic-Ray Antiparticle

Measurements:Antiprotons

fd: Clumpinessfactors needed todisentangle aneutralino inducedcomponent in theantiproton flux

MSSM



PAMELA:Cosmic-RayAntiparticle

Measurements:Antiprotons

χ contributionbackgroundtotal

MSSM

fd: Clumpinessfactors needed todisentangle aneutralino inducedcomponent in theantiproton flux



Positron Ratio and the best fit DC model background with uncertainty band


Antiproton Ratioand the best fitDC modelbackground withuncertainty band


region where0.13 < ΩCDM.h2 < 0.3

Equi-clumpinessfactor densityin respect to a NFW

MSSMEstimated reaches with Pamela


mt =174 GeV

Clumpiness factors fdneeded to disentangle aneutralino inducedcomponent in the antiprotonflux with PAMELA (χ2>1.8)that still give a good fit ofthe present data

Equi-neutralino mass linesastro-ph/0502406, 21 Feb. 05




MSSMEstimated reaches with Pamela


Clumpiness factors fdneeded to disentangle aneutralino inducedcomponent in the antiprotonflux with PAMELAthat still give a good fit ofthe present data

Equi-neutralino mass linesastro-ph/0502406




Estimated reaches with Pamela


Clumpiness factors fdneeded to disentangle aneutralino inducedcomponent in the antiprotonflux with PAMELAthat still give a good fit ofthe present data

Equi-neutralino mass lines

MSSM

astro-ph/0502406


region where0.13 < ΩCDM.h2 < 1

GLAST sensitivity (5 σ) for aneutralino density Nχ of 104 ina ΔΩ=10-5 sr region around thegalactic center

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

Typical Nχ values for ΔΩ=10-5 sr :NFW: Nχ = 104

Moore: Nχ = 9 106

Isotermal: Nχ = 3 101

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

Estimated reaches with GLAST


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


region where0.13 < ΩCDM.h2 < 1

GLAST sensitivity (5 σ) for aneutralino density Nχ of 104

in a ΔΩ=10-5 sr region aroundthe galactic center

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

Typical Nχ values for ΔΩ=10-5 sr :NFW: Nχ = 104

Moore: Nχ = 9 106


Estimated reaches with GLAST


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]


region where 0.13 < ΩCDM.h2 < 0.3

MSSMEstimated reaches with GLAST and Pamela


mt =174 GeV

Clumpiness factors fd needed todisentangle a neutralino inducedcomponent in the antiproton flux withPAMELA (χ2>1.8) that still give a goodfit of the present dataEqui-clumpiness factor density inrespect to a NFW



NFW in a ΔΩ=10-5 sr regionaround the galactic center

same but for Nχ of 105

(clumpines factor 10 )

astro-ph/0502406 and astro-ph/0305075


MSSMEstimated reaches with GLAST and Pamela



Clumpiness factors fd needed todisentangle a neutralino inducedcomponent in the antiproton flux withPAMELA (χ2>1.8) that still give a goodfit of the present dataEqui-clumpiness factor density inrespect to a NFW



NFW in a ΔΩ=10-5 sr regionaround the galactic center

same but for Nχ of 105

(clumpines factor 10 )


~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


Annihilation channel W+W-

Mχ =80 GeV


new σ model for pp-> π0 T.Kamae et al. astro-ph/0410617

GALPROPwith the conventionalcosmic ray spectra(Strong et al. 2004)

new σ model


things to do :

• include new cross sections in Galprop

• interface between DM programs and GLAST simulation

• Matrix of performances of GLAST and calorimeter alone

• others DM models ->> see Andrea Lionetto talks

...?


next Workshop ?

Fourth Workshop onScience with the New Generation ofHigh Energy Gamma-ray Experiments

Elba ?beginning of June 06 ?

next DM & Exotic Physics Group Workshop ?December 05 or Jan 06 ?


the end


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



Signal rate from Supersymmetry

governed by supersymmetric parameters

governed by halo distribution

gamma-ray flux from neutralino annihilation

J(ϕ):


EGRET, E > 1GeVMayer-Hasselwanderet al, 1998


Poin source locationfor 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] 3820 x 20 field IBIS/ISGRI 20–40 keV1 pixel ~ 5 arcmin

Poin source locationfor GLAST~ 5 arcmin

20 x 20 field EGRET, E > 1GeV


Other hints? WMAP data

Excess microwave emission observed in the inner Galaxy (1-2 Kpc, 7-14 deg)consistent with synchrotron emission from highly relativistic e+ e- produced by100 GeV dark matter particle annihilation.

D. P. Finkbeiner astro-ph/0409027

Aldo Morselli, INFN, Sezione di Roma 2 & Università di Roma Tor Vergata, [email protected] 400.024 parsecs

M=10-6 Msun

Z=26

Earth-Mass halos “observed” in high-resolution simulationsDiemand, Moore & Stadel, Nature 433 (2005) 389-391

.. contact Lidia Pieri


Where is the galaxy ?R.Minchin et al.astro-ph/050231216 Feb 2005

VIRGOHI21contain no stars,a cloud ofhydrogen atomsof 108 solar mass,but it is isthousand timesmore massive


Mini-Spikes in Mini-HalosZhao & Silk, 2005

IMBH forms by gasaccretion, mass ~10^3--10^4 Solar masses

Accretion time-scalelonger than the localdynamical time,

Formation of mini-spikeof r^-1.5 density

Other scenarios couldproduce even moremassive black holes (mass10^5 Msun).

r -1.5

BH

Mini-Spike

Mini-Halo or “clump”

log ρ(

r)

log (r)


new σ model for pp-> π0 T.Kamae et al. astro-ph/0410617


f = dark matter fraction concentrated in clumps

d gives the overdensity due to a clumps in respect to the local halo density.In the presence of many small clumps the antiproton flux is given by:


PAMELAexpectations forthree years for

antiproton spectrafor DRB model

astro-ph/0502406


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


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

MAGIC (exp)MAGIC (real)

MAGIC 2 (exp)

MAGIC


GLASTScheme

Gamma-RayLarge Area SpaceTelescope


PAMELA scientific program

energy range particles/3 years

Antiproton 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 Rays

Actual 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.


The Satellite: Resurs DK1- Soyuz-TM Launcher

from Baikonur

- Launch in 2005

- Lifetime >3 years

- PAMELA mounted insidea Pressurized Container,attached to Satellite

- Earth-Observation-Satellite

Current GLAST related DM work - Istituto Nazionale di...

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