march. 7, 2005 moriond electroweak, 2005, w. de boer, univ. karlsruhe1 wim de boer, christian...
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March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 1
Wim de Boer, Christian Sander, Valery ZhukovUniv. Karlsruhe
Dmitri Kazakov, Alex GladyshevDubna
Outline (see astro-ph/0408272)
• EGRET Data on diffuse Gamma Rays show excess in all sky directions with the SAME energy spectrum from monoenergetic quarks
• WIMP mass between 50 and 100 GeV from spectrum of EGRET excess
• Halo distribution from sky map
• Data consistent with Supersymmetry
EGRET excess of diffuse Galactic Gamma Rays interpreted as Dark Matter Annihilation
From CMB + SN1a + structure formation
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 2
DM annihilation in Supersymmetry
Dominant diagram for WMAPcross section in MSSM: + A b bbar quark pair
B-fragmentation well studied at LEP!Yield and spectra of positrons,gammas and antiprotons well known!
f
f
f
f
f
f
Z
Z
W
W 0
f~
A Z
Galaxy = SUPER-B-factory with luminosity some 40 orders of magnitude above man-made B-factories
≈ 37 gammas
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 3
Basics from cosmology:Hubble const. determines WIMP annihilation x-section
Thermal equilibrium abundance
Actual abundance
T=M/22Co
mo
vin
g n
um
ber
d
ensi
ty
x=m/T
T>>M: f+f->M+M; M+M->f+fT<M: M+M->f+fT=M/22: M decoupled, stable density(wenn annihilation rate expansion rate, i.e. =<v>n(xfr) H(xfr) !)
Jung
man
n,K
amio
nko
wsk
i, G
riest
, P
R 1
995
Present WMAP h2=0.1130.009requires <v> 2.10-26 cm3/s
H-Term takes care of decrease in density by expansion. Right-hand side:annihilation and production.
More precisely by solving Boltzmann eq.
h2 = mn/c 2.10-27 [cm3/s]/<v>
(<v> independ. of m!)
DM density increases locally after galaxy formation. In this room: 1 WIMP/coffee cup 105 averaged density.
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 4
RED=flux fromDM AnnihilationYellow = backgr.Blue = BG uncert.
Bremsstr.
Extragal.
ICWIM
PS 0
Blue: uncertainty from background shape
Blue: uncertainty from WIMP mass
Basics of background and signal shapes
WIMP MASS50 - 100 GeV
65100
Bremsstr.
Extragal.
ICWIM
PS
0
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 5
No SM
Electrons
No SM
Protons
Quarks fromWIMPS
Quarks in protons
Basics of background and signal shapes
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 6
Energy loss times of electrons and nuclei
Protons diffuse for long times without loosing energy!
-1 = 1/E dE/dt
univ
If centre would have harder spectrum, then hard to explain why excessin outer galaxy has SAME shape (can be fitted with same WIMP mass!)
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 7
EGRET on CGRO (Compton Gamma Ray Observ.)
9 yrs of data taken (1991-2000)
Main purpose: sky map of pointsources above diffuse BG.
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 8
Gamma Ray Flux from WIMP annihilation in given direction ψ:
Similar expressions for:
pp->0+x->+x, ( given by gas density, highest in disc) e->e, eN->eN, ( given by electron/gamma density, highest in disc)Extragalactic Background (isotropic)DM annihilation ( 1/r2 for flat rotation curve)All have very different, but known energy spectra.Cross sections known. Densities not well known, so keep absolutenormalization free for each process.
Basics of astro-particle physics
Fit shape of various contributions with free normalization, but normalizationlimited by experimental overall normalization error, which is 15% for EGRET data. Point-to-point errors 7% (yields good 2).
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 9
x y
z
2003, Ibata et al, Yanny et al.
v2M/r=cons.and
M/r3
1/r2
for const.rotation
curveDivergent for
r=0?NFW1/r
Isotherm const.
Executive Summary for fits in 360 sky directions
xy
xz
Expected Profile
Halo profile
Outer Ring
Inner Ring
bulge
tota
lDM
1/r2 halodisk
Rotation Curve
Observed Profile
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 10
Excess of Diffuse Gamma Rays above 1 GeV(first publications by Hunter et al, Sreekumar et al. (1997)
Str
on
g,
Moskale
nko,
Reim
er,
AP
J.613,
astr
o-p
h/0
406254
2004
A: inner Galaxy (l=±300, |b|<50)B: Galactic plane avoiding AC: Outer Galaxy
D: low latitude (10-200)
E: intermediate lat. (20-600)F: Galactic poles (60-900)
A B C
D E F
0
Bre
msstra
hlu
ng
Inv. Compton
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 11
Excess of Diffuse Gamma Rays has same spectrum in all directions compatible with WIMP mass of 50-100 GeV
Important: if experiment measures gamma rays down to 0.1 GeV, then normalizations of DM annihilation and background can both be left free, so one is not sensitive to abso- lute background estimates, BUT ONLY TO THE SHAPE, which is much better known.
Egret Excess aboveextrapolated backgroundfrom data below 0.5 GeV
Excess same shape in all regions implying same source everywhere
Statistical errors only
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 12
Diffuse Gamma Rays for different sky regions Good Fits for WIMP masses between 50 and 100 GeV
3 components: galactic background + extragalactic bg + DM annihilation fittedsimultaneously with same WIMP mass and DM normalization in all directions.Boost factor around 70 in all directions and statistical significance > 10 !
A: inner Galaxy B: outer disc C: outer Galaxy
D: low latitude E: intermediate lat. F: galactic poles
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 13
Optimized Model from Strong et al. astro-ph/0406254 Change spectral shape of electrons AND protons
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 14
Optimized Model from Strong et al. astro-ph/0406254 Change spectral shape of electrons AND protons
Nucleon and electron spectratuned to fit gamma ray data.
Apart from the difficulty tohave inhomogeneous nuclei spectra(SMALL energy losses!) the modeldoes NOT describe the spectrumIN ALL DIRECTIONS!
Electrons Protons
B/C
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 15
Optimized Model from Strong et al. astro-ph/0406254 Change spectral shape of electrons AND protons
100 MeV 150 MeV 300 MeV
500 MeV 1000 MeV
2000 MeV
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 16
Optimized Model from Strong et al. astro-ph/0406254 Change spectral shape of electrons AND protons
Probability of optimized modelif 2 measuredin 360 sky directionsand integrate data with E>0.5 GeV:
2= 962.3/324 for Optimized Model without DM +correl. errors: Prob = < 10-10
2= 306.5/323 for Optimized Model +DM +correl. errors: Prob = 0.736Boostfactor=25 for OM vs 70 for CM
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 17
Determining halo profile
DM Gamma Ray Flux:
1/r2
=2
2 Gaussian ovals
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 18
Enhancement of rings over 1/r2
profile 2 and 7, respectively.Mass in rings1.6 and 0.3%of total DM
14 kpc coincides with ringof stars at 14-18 kpc due to infall of dwarf galaxy(Yanny, Ibata, …..)
4 kpc coincides with ring ofneutral hydrogen molecules!
Fit results of halo parameters
(<v> from WMAP)Parameter values:
H2
H
R [kpc]4
Boostfactor 20-200 Dokuchaev et al: 10<B<200, IDM2004
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 19
Halo density on scale of 300 kpc
Sideview Topview
Cored isothermal profile with scale 4 kpc Total mass: 3.1012 solar masses
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 20
Halo density on scale of 30 kpc
Sideview Topview
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 21
Longitude fits for 1/r2 profile with/w.o. rings
Halo parameters from fit to 180 sky directions: 4 long. profiles forlatitudes <50, 50<b<100, 100<b<200, 200<b<900 (=4x45=180 directions)
WITHOUT rings
DISC
50<b<100
100<b<200
200<b<900
WITH 2 rings
DISC
50<b<100 200<b<900
100<b<200
E > 0.5 GeV
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 22
Longitude on linear scale
ABOVE 0.5 GeVBELOW 0.5 GeV
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 23
Do other galaxies have bumps in rotation curves?
Sofue & Honma
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 24From Eric Hayashi
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 25
Normalizationof background:
Compare with GALPROP,which gives absolute
prediction of backgroundfrom gas distributions etc.
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 26
Background scaling factors
Background scaling factor = Data between 0.1 and 0.5 GeV/GALPROPGALPROP = computer code simulating our galaxy (Moskalenko, Strong)
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 27
Normalizationof DMA ->
“Boost factor”(= enhancement of DMA
by clustering of DM)
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 28
Clustering of DM -> boosts annih. rate
Clumps with Mmin give the dominant contribution to DM annihilation ->many in a given direction -> similar boost factor in all directions
Annihilation DM density squared!
Clustersize: 1014 cm =10x solar systemMmin 10-8 -10-6 MּסCluster density 25 pc-3
Halo mass fraction in clumps: 0.002From Berezinsky, Dokuchaev, EroshenkoBoost factor <2>/<>2 20-200
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 29
What aboutSupersymmetry?
Assume mSUGRA5 parameters: m0, m1/2, tanb, A, sign μ
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 30
Annihilation cross sectionsin m0-m1/2 plane (μ > 0, A0=0)
tan=5 tan=50bb t t
WW
bb t t
WW
For WMAP x-section of <v>2.10-26 cm3/s one needs large tanβ
10-2410-27
EGRETWMAP
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 31
Coannihilations vs selfannihilation of DM
If it happens that other SUSY particles are around atthe freeze-out time, they may coannihilate with DM.E.g. Stau + Neutralino -> tau Chargino + Neutralino -> W
However, this requires extreme fine tuning of masses,since number density drops exponentially with mass.
But more serious: coannihilaition will cause excessive boostfactorsSince anni = coanni + selfanni must yield <v>=1026 cm3/s.This means if coannihilation dominates, selfannihilation 0In present universe only selfannihilation can happen, sinceonly lightest neutralino stable, other SUSY particles decayed,so no coannihilation. If selfannihilation x-section 0, no indirectdetection. CONCLUSION: EGRET data excludes largely coannih.
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 32
EGRET excess interpreted as DM consistent with WMAP, Supergravity and electroweak constraints
MSUGRA can fulfillall constraints from WMAP,LEP, b->s, g-2 and EGRET simultaneously, if DM is neutralino with massin range 50-100 GeV and squarks and sleptons are O(1 TeV)
WMAP
EGRET
Stau coannihilation
mA resonance
Bulk
Incomp. withEGRET data
StauLSP
No EWSB
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 33
SUSY Mass spectra in mSUGRA compatible with WMAP AND EGRET
LSP largely Bino DM is supersymmetric partner of CMB
Charginos, neutralinos and gluinos light
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 34
Unification of gauge couplings
With SUSY spectrum from EGRET data and start values of couplings from final LEP data perfect gauge coupling unification possible
Up
date
fro
m A
mald
i,
dB
, F
ürs
ten
au
, P
LB
260
1991
SM SUSY
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 35
Predictions from EGRET data assuming Supersymmetry
Comparison with direct DM Searches
DAMA
CDMS
ZEPLIN
Edelweiss
Projections
Spin-independent Spin-dependent
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 36
Positron fraction and antiprotons from present balloon exp.
SAME Halo and WIMP parameters as for GAMMA RAYS but fluxes dependent on propagation! DMA can be used to tune models:at present no convection, nor anisotropic diffusion in spiral arms.
Positrons AntiprotonsAntiprotonsPositrons
SignalBackground
SignalBackground
March. 7, 2005 Moriond Electroweak, 2005, W. de Boer, Univ. Karlsruhe 37
Summary
EGRET excess shows all key features from DM annihilation:
These combined features provide FIRST (>10) EVIDENCE that DM is not so dark and follow ALL DMA expectations imagined so far.
Excess has same shape in all sky directions: everywhere it is perfectly (only?) explainable with superposition of background AND mono-energetic quarks of 50-100 GeV Results and x-sect. in agreement with SUPERSYMMETRY
Excess connected to MASS, since it can explain peculiar shape of rotation curve
Excess follows expectations from galaxy formation: 1/r2 profile with substructure, visible matter/DM0.02
Conventional models CANNOT explain above points SIMULTANEOUSLY,especially spectrum of gamma rays in all directions, DM density profile,shape of rotation curve, stability of ring of stars at 14 kpc,..