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

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

Andrea Lionetto INFN, Sezione di Roma 2 &

Università di Roma Tor Vergata

Dark Activities

ASI Workshop, Frascati 3 Luglio 2007

Dark Matter really exist ?

= M + = 1.020.02

~ 0.73

M~ 0.27

CDM ~ 0.23

b ~ 0.04

HDM, < 0.01{

““Concordance model”Concordance model”

CDM~ 6 b

color image from the Magellan images of the merging cluster 1E0657−558

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 stellar component and the fluid-likeX-ray emitting plasma are spatially segregated

Dark Matter Ring around

Galaxy Cluster CL0024+17

M.Jee et al.,arXiv:0705.2171

1 high-speed line-of-sight collision of two massive clusters~ 1-2 Gyr ago



1% Stars

7% Gas in vir. structures

7% WH Gas in IGM

85% DARK MATTER

Baryons

Non-baryonic

An Inventory of Matter in the Universe

So, what is Dark Matter?



Particle Physics after Big Bang

SupersymmetryParticle Sparticle

For unbroken supersymmetry there is a mass degeneracy

Sparticle have not be found at accelerators so far

Supersymmetry is broken

Supersymmetry breaking schemes:• gravity-mediated scenarios• Gauge mediated scenarios• Anomaly mediated scenarios

Running couplings

Neutralino WIMPs

Assume are present in the galactic halo• Majorana particle => can annihilate in pairs in the 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 an interesting signature• ie: --> p + X• Produced from (e. g.) --> q / g / gauge boson / Higgs boson and subsequent decay and/ or hadronisation.

PAMELA Payload for Antimatter Matter Exploration and Light Nuclei

AstrophysicsIn orbit on June 15, 2006, on board of the DK1 satellite by a Soyuz rocket from the Bajkonour launch site.First switch-on on June 21 2006From July 11 Pamela is in continuous data taking mode


PAMELA


PAMELA: Cosmic-Ray Antiparticle

Measurements: Antiprotons

fd: Clumpiness factors needed to disentangle a neutralino induced component in the antiproton flux

A.Lionetto, A.Morselli, V.Zdravkovic

JCAP09(2005)010 [astro-ph/0502406]

an example in mSUGRA

f = the dark matter fraction concentrated in clumpsd = the overdensity due to a clump with respect to the local halo density


PAMELA: Cosmic-Ray Antiparticle

Measurements: Antiprotons

contributionbackgroundtotal

MSSMMSSM

fd: Clumpiness factors needed to disentangle a neutralino induced component in the antiproton flux

A.Lionetto, A.Morselli, V.Zdravkovic

JCAP09(2005)010 [astro-ph/0502406]

Where should we look for WIMPs with GLAST?

• Galactic center• Galactic

satellites• Galactic halo• Extra-galactic


Sun

Galactic Center

Signal rate from Supersymmetry

governed by supersymmetric parameters

governed by halo distribution

gamma-ray flux from neutralino annihilation

J():

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

Differential yield for each annihilation channel

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]


neutralino mass

Differential yield

for b bar


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


~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

Isotermal: N = 3 101

Annihilation channel W+W-

M =80 GeV

Model independent results for the GC

3

Max background Min background


EGRET,

E > 1GeV

Mayer-Hasselwander et 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 location for GLAST~ 5 arcmin

Galactic Center

HESS and MAGIC SpectrumUnbroken power-law.

Hard spectrum = 2.2.No evidence for variability on

a variety of time scales.

Consistent with SGR A* to 6’’ and slightly extended.

SGR A

Good agreement

between HESS

and MAGIC (large zenith angle

observation). astro-ph/0512469


EGRET, GLAST, HESS, MAGIC

it might still be that a DM component could be singled out, e.g. the EGRET source (?):a DM source can fit the EGRET data; GLAST would detect its spectral and angular signatures and identify without ambiguity such DM source!

Model independent results for the GC

3

Max background Min background

Excluded by HESS and MAGIC

Satellites

Optimistic case: 70 counts signal, 43

counts background

within 1.5 deg of clump center

55-days GLAST in-orbit counts map (E>1GeV)

GalacticCenter

30-deglatitude

Larry Wai et al. for the DM&NPWorking Group

The search for milky way halo substructure WIMP annihilations using the GLAST LAT

Dark matter

calculation with

semi-analytic

method of Taylor

& Babul 2004,

2005Background

estimate using

EGRET above 1GeV

(source

subtracted)

M=100GeV

<σ v> = 2.3x10-26cm3s-1

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

G.Bertone et al. astro-ph/0612387

Cosmological Wimp annihiliation spectrum

spectral fits of simulated DM point sources

Supersymmetry introduces free parameters:

In the MSSM, with Grand Unification assumptions, the masses and couplings of the SUSY 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

• 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

• tan = v2 / v1 = <H2> / <H1> the ratio between the two vacuum expectation

values of the Higgs fields

GLAST limits

no electroweaksymmetry breaking

WMAP 3 allowed region (95% C.L)

tg()=55, sign()=+1

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

mSUGRA

Sensitivity plot for 5 years observation of mSUGRA for GLAST for tan()=55.

GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile

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

equi neutralino mass curves

GLAST limits


WMAP 3 allowed region (95% C.L)

m=400 GeV

m=200 GeV

m=300 GeV

mSUGRA

Sensitivity plot for 5 years observation of mSUGRA for GLAST for tan()=55.

GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile

LHC limits 100 fb-1

LC500

GLAST limits

LC1000 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 SearchmSUGRA

Sensitivity plot for 5 years observation of mSUGRA for GLAST for tg(b)=55and for other experiments. GLAST 3σ sensitivity is shown at the blue line and below for truncated NFW halo profile



LHC limits

LC1000 limits

LCC2

mh0 < 114.3 GeVWMAP 3 3 allowed region

GLAST limits

tg()=10, sign()=+1

LC500

Sensitivity plot for observation of mSUGRA for a number of accelerator experiments and GLAST for tan()=10. GLAST 5σ sensitivity is shown at the

blue line and below a for truncated Navarro Frank and White (NFW) halo profile

LCC2 from E.Baltz et al. hep-ph/0602187

mSUGRA


tg()=60, sign()=+1

WMAP 3 5 allowed region

GLAST 5 limits

5 years of data

5σ Sensitivity plot for for GLAST for a truncated NFW halo profile mSUGRA

Sensitivity plot for observation of mSUGRA for GLAST for tan()=60. GLAST 5σ sensitivity is shown at the blue line and below a for truncated NFW halo profile

the end

Aldo Morselli, INFN & Università di Roma Tor Vergata, [email protected] 4120 x 20 field IBIS/ISGRI 20–40 keV1 pixel ~ 5 arcmin

Point source location for GLAST~ 5 arcmin

20 x 20 field EGRET, E > 1GeV



you need a factor ~ 10- 50 with respect to the “ standard” mSugra scenario

Conclusion:

GLAST limitsfor clumpiness factor 10

Documents

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