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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: [email protected]
2
3
INFERENCE
Virial Theorem
Hydro Equilibrium
Gravitational lensing
+
PHYSICAL
+
,...,,0 pXX ±→+ π
ieXX ντµ ,,,±±±→+
Annihilation Decay
γ+→ ixX
4
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
5
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
6
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
7
SUSY neutralino DM
8
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
9
Covering the whole e.m. spectrum
Synch
rotron
SZ E
ffect
ICS
Brem.+ICS+π 0
Brem.+ICS
ICS
χχannihilation
products
10
DM signals: multi-ν Best Labs.
[Colafrancesco 2005, 2007]
ClustersClusters
dSphdSph GalaxyGalaxy
gas
11
Neutralino DM: γ-rays
12
The γ-ray DM sky
[Kuhlen et al. arXiv:0704.0944]
http://babbage.sissa.it/abs/0704.0944
13
The GLAST skySC2 simulation (55 days) Angular power spectrum
Blazars
DM
multipole1 10 102
l(l+1
)Cl/2
π
103
Variability
14
DM halos: multi−ν messengers
−+WW_bb
Mχ=40 GeV_bb
Dwarf galaxies DRACO
[Colafrancesco, Profumo & Ullio 2006, 2007]
Galaxy clustersCOMA
GLAST
15
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
16
Neutralino DM: low-ν
17
Leptons: e± equilibrium spectrum
[ ] [ ] ),(),()(),()(),( rEQrEnEbE
rEnEDt
rEneeee
e =∂∂
−∇∇−∂
∂
ProductionProduction EquilibriumEquilibrium
),( rEQe ),( rEne
DiffusionDiffusion E lossesE lossesγγ −= BEDED 0)( bremCoulsyncICe bbbbEb +++=)(
18
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)
19
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
20
Dwarf Galaxies at multi-ν: a DM survey
21
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
22
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
23
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
24
Neutralino DM: radio emission
25
DM halos: Synchrotron radio emission
[Colafrancesco, Profumo & Ullio 2006, 2007]
Dwarf galaxies DRACOGalaxy clustersCOMA
Diffusionirrelevant
Diffusiondominant
26
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
27
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
28
Neutralino DM: ICS of CMB (SZE)
29
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-
30
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
31
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
32
SZE in DM halos
SZthSZth
SZwarmSZwarm
SZrelSZrel
SZDMSZDM
A structure with:
• Hot gas• Warm gas• Rel. Plasma• DM• (Vr ≈ 0)
33
SZE in DM halos
SZthSZth
SZwarmSZwarm
SZDMSZDM
A structure with:
• Hot gas• Warm gas•• DM• (Vr ≈ 0)
34
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
35
Draco dSph.
36
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]
37
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
38
SZE in 1ES0657-556: avoiding the θ-trap
gas SZE
DM SZE
39
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
)
40
1ES0657-556 @ various frequencies
SymbolXSymbolXSKA SKA
[Colafrancesco & Ullio 2006]
GLAST GLAST
41
Sterile neutrino DM
42
Sterile neutrino DM: lineHot gasDark Matter
νs → να + γνs → να + γ
expectationexpectation
43
Sterile neutrinos: limits
[Watson et al. 2006 (astro-ph/0605424)]
Exclu
ded
Exclu
ded
[Colafrancesco 2007]
Bullet cluster
Excl
ude
dby
Ly-α
44
Coma constraints from20-80 keV emission
[Yuksel et al. 2007][Colafrancesco 2007]
Simbol-XNEXTnuStar
GRI
45
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
46
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