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IoPIoP/RAS Meeting 2007/RAS Meeting 2007 Nov. 26, 2007

Multi-frequency analysis ofDark Matter signals

Multi-frequency analysis ofDark Matter signals

Sergio Sergio ColafrancescoColafrancescoASI ASI -- ASDC ASDC INAF INAF -- Osservatorio Astronomico di RomaOsservatorio Astronomico di RomaEmailEmail: Sergio.Colafrancesco@mporzio.astro.it

Colafrancesco@asdc.asi.it

mailto:Sergio.Colafrancesco@mporzio.astro.itmailto:Colafrancesco@asdc.asi.it

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INFERENCE

Virial Theorem

Hydro Equilibrium

Gravitational lensing

+

PHYSICAL

+

,...,,0 pXX ±→+ π

ieXX ντµ ,,,±±±→+

Annihilation Decay

γ+→ ixX

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Astrophysical search for DM

• Cosmology• DM candidatesDM and LSS

• Signals• Targets• Detectability

Search for DM

• Dark galaxies (dwarfs)• DM–baryon offset clusters

Optimal laboratories

Coma - 1ES0657-556 • Constraints• Experimental outlineMW Dwarf Sph. galaxies

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Viable DM candidatesLight (MeV) DMNeutralinos Sterile ν’s

Unstable

Radiative decay: line

νs → να + γνs → να + γ

WMAP (95%)

Exc

lude

dby

BB

N

Bremsstrahlung

in-flight annihilation

SNe

e- anomalous magnetic moment

Exc

lude

dby

BB

NNo

Cos

mol

ogica

l DM

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DM candidates: signalsLight (MeV) DMNeutralinos

Annihilating MeV DM• Continuum: HXR/γ-rays• Line: e± annihilation

Radiative decay: line

νs → να + γνs → να + γ

511 keVMs

Mχ

Inverse Compton scatteringBremsstrahlung

Synchr.

Bremsstrahlung

π0

Sterile ν’s

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SUSY neutralino DM

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Gamma raysbremsstrahlung

ICS

χ

χπ±

π0 γ+γ

Gamma rays(π0 decay)

p

e±

SZ effectICS

Radio emissionSynchrotron

B

e± e±γCMB

p

e±γCMB

X-raysbremsstrahlung

ICS

High frequencyHigh frequency

Hadronic

Hadronic

processes

processes

Low frequencyLow frequency

Leptonic

Leptonicprocesses

processes

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Covering the whole e.m. spectrum

Synch

rotron

SZ E

ffect

ICS

Brem.+ICS+π 0

Brem.+ICS

ICS

χχannihilation

products

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DM signals: multi-ν Best Labs.

[Colafrancesco 2005, 2007]

ClustersClusters

dSphdSph GalaxyGalaxy

gas

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Neutralino DM: γ-rays

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The γ-ray DM sky

[Kuhlen et al. arXiv:0704.0944]

http://babbage.sissa.it/abs/0704.0944

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The GLAST skySC2 simulation (55 days) Angular power spectrum

Blazars

DM

multipole1 10 102

l(l+1

)Cl/2

π

103

Variability

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DM halos: multi−ν messengers

−+WW_bb

Mχ=40 GeV_bb

Dwarf galaxies DRACO

[Colafrancesco, Profumo & Ullio 2006, 2007]

Galaxy clustersCOMA

GLAST

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DM signals: multi-frequency

π0 → γγ ~ 10-11 10 2 ~ 6

ICS ~ 10-13 10 6 ≥ 10 3

Synchrotron ~ 10-14 1016 ≥ 104

F (erg/s cm2) counts S/N

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Neutralino DM: low-ν

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Leptons: e± equilibrium spectrum

[ ] [ ] ),(),()(),()(),( rEQrEnEbE

rEnEDt

rEneeee

e =∂∂

−∇∇−∂

∂

ProductionProduction EquilibriumEquilibrium

),( rEQe ),( rEne

DiffusionDiffusion E lossesE lossesγγ −= BEDED 0)( bremCoulsyncICe bbbbEb +++=)(

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Solution: qualitative[ ]

lossD

D

diffusionsource

sourcelossee VV

VrEQrEnττ

ττ+

⋅+

⋅= ),(),(

VD

Vs

VD

Vs

τ loss « τ D τ loss » τ D

[ ]lossee rEQrEn τ),(),( = [ ]loss

D

diffusion

sourcelossee V

VrEQrEnτττ ⋅⋅= ),(),(

Galaxies (∼kpc)Galaxy clusters (∼Mpc)

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DM halos: multi−ν messengers

−+WW_bb

Mχ=40 GeV_bb

Dwarf galaxies DRACO

[Colafrancesco, Profumo & Ullio 2006, 2007]

Galaxy clustersCOMA

SimbolX SimbolX

GLAST

EGRETMAGICSTACEE

CTACTA

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Dwarf Galaxies at multi-ν: a DM survey

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F1.4 < 3.5 mJy S=13 pho; bkg=11 pho

F4.9 < 2 mJy S=1 pho; bkg=1 pho

F1.4 < 3.5 mJy S=4 pho: bkg=2 phoF2keV <

SED

SED

F2keV <

F2keV

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F5 < 15.2 mJy F2keV <

F1.4 < 3.5 mJy S=2 pho; bkg=3 pho

No NVSS coverage

F2keV <

F0.1-10=2.9° 14erg/scm2

SED

Scl.

UMa O

Carina

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F1.4 = 0.54 mJy (HI line) F2keV <

F2-38 < 4 mJy S=2 pho; bkg=3 pho

F1.4 < 3.5 mJy S=2 pho; bkg=3 pho

F2keV <

F2keV <

Fornax

O

LeoII

LeoI

O

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Neutralino DM: radio emission

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DM halos: Synchrotron radio emission

[Colafrancesco, Profumo & Ullio 2006, 2007]

Dwarf galaxies DRACOGalaxy clustersCOMA

Diffusionirrelevant

Diffusiondominant

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Clusters of galaxies: χ propertiesRadio halo• brightness distribution (@ 1.4 GHz) • integrated spectrum (30 MHz-5 GHz)

[Colafrancesco, Profumo & Ullio 2006]

sub-halos

sub-halos

ComaComa

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Dwarf galaxies: avoiding the B-trapVD

VS

vrEnDBS eee σνν ),,()(2⊗⊗∝

vrEnDBI eee σνν ),,()(2⊗⊗∝

γ)/(0 BEDD ee =

Spectrum BrightnessB

[Colafrancesco 2007, Colafrancesco & Pieri 2007]

χ

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Neutralino DM: ICS of CMB (SZE)

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SZE: probe of leptonic atmospheres[Colafrancesco 2007, New Astr.Rev., 51, 394][Colafrancesco 2007, New Astr.Rev., 51, 394]

I0(x) I(x)

Irel(x)

thermal NR e-

2

34γ

νν

≈∆

24 cmkT

e

e≈∆νν

relativistic e-

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SZE: general derivation [Colafrancesco & al. 2003, A&A, 397, 27][Colafrancesco & al. 2003, A&A, 397, 27]

Intensity changeIntensity change

ThermalPressurePressure

Relativistic

Spectral shapeSpectral shape

∫∞

=0

);()()( psPpdpfsP seRedistribution functionRedistribution function

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SZE in DM halos [Colafrancesco 2007, New Astr.Rev., 51, 394][Colafrancesco 2007, New Astr.Rev., 51, 394]

SZthSZth

SZrelSZrel

SZDMSZDM

SZkinSZkinSZwarmSZwarm

A structure with:

• Hot gas• Warm gas• Rel. Plasma• DM• Vr > 0

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SZE in DM halos

SZthSZth

SZwarmSZwarm

SZrelSZrel

SZDMSZDM

A structure with:

• Hot gas• Warm gas• Rel. Plasma• DM• (Vr ≈ 0)

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SZE in DM halos

SZthSZth

SZwarmSZwarm

SZDMSZDM

A structure with:

• Hot gas• Warm gas•• DM• (Vr ≈ 0)

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SZE in DM halos [Colafrancesco 2004, A&A, 422, L23][Colafrancesco 2004, A&A, 422, L23]

SZDMSZDM

A structure with:

•••• DM• (Vr ≈ 0)

Pure DM haloPure DM halo

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Draco dSph.

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SZDM in Draco Diffusion effects

[ ]lossD

D

diffusionsource

sourcelossee VV

VrEQrEnττ

ττ+

⋅+

⋅= ),(),(

VD

τ loss » τ D

Vs

[ ]loss

D

diffusion

sourcelossee V

VrEQrEnτττ ⋅⋅= ),(),(

Iν

r

[Culverhouse, Evans & Colafrancesco 2006][Culverhouse, Evans & Colafrancesco 2006]

[Colafrancesco, Profumo & Ullio 2007][Colafrancesco, Profumo & Ullio 2007]

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The cluster 1ES0657-556

DM clump A)M = 1015 MDM clump A)M = 1015 M

Gas clump A)T = 14 keVGas clump A)T = 14 keV

Gas clump B)T = 6 keVGas clump B)T = 6 keV

DM clump B)M = 6 1013 MDM clump B)M = 6 1013 M

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SZE in 1ES0657-556: avoiding the θ-trap

gas SZE

DM SZE

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Isolating SZDM at ∼223 GHz [Colafrancesco et al. 2007][Colafrancesco et al. 2007]

Neu

tral

ino

mas

s (

ν=22

3 G

Hz)

Freq

uenc

y(M

χ=20

GeV

)

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1ES0657-556 @ various frequencies

SymbolXSymbolXSKA SKA

[Colafrancesco & Ullio 2006]

GLAST GLAST

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Sterile neutrino DM

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Sterile neutrino DM: lineHot gasDark Matter

νs → να + γνs → να + γ

expectationexpectation

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Sterile neutrinos: limits

[Watson et al. 2006 (astro-ph/0605424)]

Exclu

ded

Exclu

ded

[Colafrancesco 2007]

Bullet cluster

Excl

ude

dby

Ly-α

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Coma constraints from20-80 keV emission

[Yuksel et al. 2007][Colafrancesco 2007]

Simbol-XNEXTnuStar

GRI

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DM search thru the e.m. spectrum

Synch

rotron

SZ E

ffect

ICS

Brem.+ICS+π 0

Brem.+ICS

ICS

χχannihilation

products

SKASKALOFARLOFAR

PLANCKPLANCKOLIMPOOLIMPO

Simbol-XSimbol-XNEXTNEXT

GLASTGLASTHESSHESS

ALMAALMA

SZ exp.SZ exp. GRIGRI CTACTA

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THANKS

for your attention !

IoP/RAS Meeting 2007 Nov. 26, 2007Astrophysical search for DMViable DM candidatesDM candidates: signalsSUSY neutralino DMCovering the whole e.m. spectrumDM signals: multi-n Best Labs.Neutralino DM: g-raysThe g-ray DM skyThe GLAST skyDM halos: multi-n messengersDM signals: multi-frequencyNeutralino DM: low-nLeptons: e equilibrium spectrumSolution: qualitativeDM halos: multi-n messengersDwarf Galaxies at multi-n: a DM surveyNeutralino DM: radio emissionDM halos: Synchrotron radio emissionClusters of galaxies: c propertiesDwarf galaxies: avoiding the B-trapNeutralino DM: ICS of CMB (SZE)SZE: probe of leptonic atmospheresSZE: general derivationSZE in DM halosSZE in DM halosSZE in DM halosSZE in DM halosDraco dSph.SZDM in DracoThe cluster 1ES0657-556SZE in 1ES0657-556: avoiding the q-trapIsolating SZDM at 223 GHz1ES0657-556 @ various frequenciesSterile neutrino DMSterile neutrino DM: lineSterile neutrinos: limitsDM search thru the e.m. spectrum