Galactic models and Indirect Dark Matter search

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Galactic models and Indirect Dark Matter search
V.Zhukov W. de Boer, C. Sander, A. Nordt
Thanks to I.MoskalenkoA.Strong V.DokuchaevD.Ka
zakovA.Pukhov
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(No Transcript)
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Ingredients
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Galaxy
Leaky box r 20kpc z/- 4-6kpc
Vconv
Va
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Propagation
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Energy losses and cross sections
tunivers
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Galactic composition Gas
MW galaxy 7 1011 Mo
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Galactic compositionInterstellar Radiation
Field and B field
Energy density eV/cm3
CMB
Stars
Dust
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Cosmic particles
From gamma
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Tune to experimental data
AMS, Pamela, GLAST etc. will contribute
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Conventional model (CM)
protons
1 GeV
0.1 GeV

100 GeV
10 GeV
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Problems with Conventional model
?0
bremss
IC
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x ,kpc
y,kpc
sun
Galactic centre
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GalProp and DarkSusy
antiprotons 1GeV from DM
Positrons 1GeV
CM reacc. Bremss IC synchrotron
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Supersymmetric Dark Matter
SUSY MSSM mSUGRA CMSSM
DM candidate stable lightest unsymmetrical
particle (LSP) can be neutralino
Large tanb is preferable
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Annihilation cross section

Dominant for most of models


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Cross sections
Averaged cross section ?? v??
depends upon m21/2 , tan2b , mo

bbar is dominant. fragmentation is well known
from LEP
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Cross sections at decoupling
Decoupling of DM from Hubble at ltsvgtn c H
where nx
decoupling Tmc/22
At DM decoupling Pdecmc/20 3-5 GeV (now
10-4eV) For low m1/2 Z channel (depending on
p) can be dominant at decoupling -gt nowadays
smaller cross sections.
same ltsngt nowadays dominant by A exchange
now
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At different tanb funnel channel is dominant ??
v? m -2A , only at low tanb -gt bulk
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Uncertainties in relic density
??h2 m mA
For large tanb gt30 ltsngt is unstable since
m2Am21m22 Dcorr at EW scale depends
on as(0.115-0.122) mb(4.0-4.4) mt(174-182)
...
as 0.115 0.122
mA is fixed by ??h2 200-500 GeV
mb 4.0 4.4
tanb20
mA is defined
by m1
tanb51
both m1 and m2
goes down and
mAgt0 due to
corrections
mt 174 182
Fix ??h2 by tuning mA and m
GUT
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Dark matter halo
?(r)?? bulk profile is estimated from N
body simulation . Very big spread from very
cusped to the cored profiles. Can be normalized
by rotation curves to the local density
??(8.5kpc)(0.2-0.8 Gev/cm3)
B(r) - Boost factor due to DM clumps since
inside the clump Icl?cl2(r). Number density of
relic clumps depends on spectrum of primary
fluctuation Peq(k)k np (Harrison-Zeldovich)
np defines hierarchy of structure
formations. if npgt1 small structures are created
first (down-top scenario). Nowadays only 0.1
of DM mass can be in clumps . The relic
clumps are denser because created earlier.
?(r)clump r -1.8-2 N(m) m -2 mmin
10-6-8 Mo Most of signal is coming from the
smallest clumps.
Defined by inflation
Top down scenario- almost no clumps?
From WMAP np0.9770.03
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Bulk profile
Ap.J.462(1999)

Profile can have triaxial shape (elt0.5) and
probably co-rotate with the galaxy.
a,b,g slopes ????at rgta, ? at rlta 2, 2, 0
- isothermal 1, 3, 1 NFW 1.5, 0, 1.5 -Moore
profiles
Cusp in the centre
Interaction with the baryionic matter and
possible coupling of baryionic and DM -dynamical
friction (arms) -adiabatic compression can change
shape
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Boost factor
Boost factor B1Ic/ Ibulk , Ibulk -signal
from the bulk component IclNcl - from clumps ,
if Ncl rbulk(r) B 11/rbulk(r)
For isothermal B(r) r2 at large r
Depends on clumps profile and spectrum of
primary fluctuations np
At large np clumps are created earlier -gt denser
Nclumps in the galactic center for different mc
V.Berezinsky V.Dokuchaev Y.Eroshenko
astro-ph/0301551
If Boos factor gt1 Itot IbulkB r(r) not
r(r)2 ! The visible profile can be different from
the mass profile. The only cross check is the
rotation curves
Small clumps are dying first
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With Conventional Galprop Model same excess in
different sky regions
Fix the neutralino mass from the spectrum
DM ?
From DM electrons and positrons
EGRET
astro-ph/0408272
Galactic coordinates
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Define the DM Halo Profile from the angular
distributions.
Cusped NFW(1,3,1) profile is excluded
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Charged components
Conventional model EGRET DM halo profile
antiprotons
CR densities of positrons and antiprotons from
annihilation after propagation in CM.
positrons
antiprotons
1 GeV
positrons
80 GeV
In the galactic center the DM electrons and
antiprotons are dominant (even for isothm.)
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Implementations
Dark Matter finder
Susy mass spectrum
IsaSusy
Annihilation yields
DarkSusy v.4.0 suspect interface 3loop
corrections for mb
Suspect
GalProp v.42.2 DM profile annihilation components
(p,pb,e,ep,gamma) anisotropic diffusion,etc.
feynhiggs
hadronisation tables
Pythia
Halofitter minimization of expdata-model
Plotting and analysis of signal and bkg.
Check relic density
DataAnalysis interface to the exp.data, galprop,
future exp. acceptances
micrOmega
Verification of the halo profile
Rotation curves Surface density
Experimental data
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Summary
GalProp is extended for DM annihilation Gamma
and charged products are included.
More tunning of GalProp to existing experimental
data are needed. The minuit version of GalProp
is under way. The heliosphere propagation is
missing.
Annihilation cross sections are obtained from
the constrained mSUGRA model for nowadays DM and
the relic density.to More work is needed to
understand uncertainties in RGE propagation in
different codes.
The DM halo profile can have sub
structures. Clumps have distribution and at large
boos factors can define the observed profiles.
We will find it ......