wim de boer, karlsruhe seminar beijing, august 15, 2007 1 dark matter visible by hard gamma rays?...
Post on 21-Dec-2015
215 views
TRANSCRIPT
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 1
Dark matter visible by hard gamma
rays?
Big Bang
Particle physics
Astroparticle physicsAstronomy
Cosmology13.7 billion years
1 ps
10-34 s
95% of energy in universe of unknown nature
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 2
Center of the Coma Cluster by Hubble space telescope ©Dubinski
Discovery of DM in 1933Zwicky, Fritz (1898-1974
Zwicky notes in 1933 that outlying galaxies in Coma cluster moving much faster than mass calculated for the visible galaxies would indicate
DM attractsgalaxies withmore force->higher speed.But still bound!
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 3
Do we have Dark Matter in our Galaxy?
RotationcurveSolarsystem
rotation curveMilky Way
1/r
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 4
Estimate of DM density
DM density falls off like 1/r2 for v=const.
Averaged DM density “1 WIMP/coffee cup” (for 100 GeV WIMP)
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 5
• 95% of the energy of the Universe is non-baryonic 23% in the form of Cold Dark Matter
• Dark Matter enhanced in Galaxies and Clusters of Galaxies but DM widely distributed in halo-> DM must consist of weakly interacting and massive particles -> WIMP’s
• Annihilation with <σv>=2.10-26 cm3/s, if thermal relic
From CMB + SN1a + surveys
DM halo profile of galaxycluster from weak lensing
If it is not darkIt does not matter
What is known about Dark Matter?
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 6
Expansion rate of universe determines WIMP annihilation cross section
Thermal equilibrium abundance
Actual abundance
T=M/22Co
mo
vin
g n
um
ber
d
ensi
ty
x=m/TGary Steigmann (
WMAP -> h2=0.1130.009 -> <v>=2.10-26 cm3/s
DM increases in Galaxies:1 WIMP/coffee cup 105 <ρ>. DMA (ρ2) restarts again..
T>>M: f+f->M+M; M+M->f+fT<M: M+M->f+fT=M/22: M decoupled, stable density(wenn Annihilationrate Expansions- rate, i.e. =<v>n(xfr) H(xfr) !)
Annihilation into lighter particles, likequarks and leptons -> 0’s -> Gammas!Only assumption in this analysis:WIMP = THERMAL RELIC!
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 7
IF DM particles are thermal relics from early universethey can annihilate with cross section as large as <v>=2.10-26 cm3/s which implies an enormous rate of gamma raysfrom π0 decays (produced in quark fragmentation) (Galaxy=1040 higher rate than any accelerator)
Expect large fraction of energetic Galactic gamma rays to come from DMA in this case.Remaining ones from pCR+pGAS-> π0+X , π0->2γ
(+some IC+brems)This means: Galactic gamma rays have 2 componentswith a shape KNOWN from the 2 BEST studied reactionsin accelerators: background known from fixed target exp. DMA known from e+e- annihilation (LEP)
Conclusion sofar
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 8
Example of DM annihilation (SUSY)
Dominant + A b bbar quark pairSum of diagrams should yield<σv>=2.10-26 cm3/s to getcorrect relic density
Quark fragmentation known!Hence spectra of positrons,gammas and antiprotons known!Relative amount of ,p,e+ known as well.
f
f
f
f
f
f
Z
Z
W
W 0
f~
A Z
≈37 gammas
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 9
R
Sundisc
Basic principle for indirect dark matter searches
R
Sun
bulge
disc
From rotation curve:
Forces: mv2/r=GmM/r2
or M/r=const.for v=cons.and(M/r)/r2
1/r2
for flat rotation curve
Expect highest DM densityIN CENTRE OF GALAXY
Divergent for r=0?NFW profile1/rIsotherm profile const.
IF FLUX AND SHAPE MEASURED INONE DIRECTION, THEN FLUX ANDSHAPE FIXED IN ALL (=180) SKY DIRECTIONS!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!!
R1
THIS IS AN INCREDIBLE CONSTRAINT, LIKE SAYING I VERIFYTHE EXCESS AND WIMP MASS WITH 180 INDEPENDENT MEAS.
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 10
Instrumental parameters:
Energy range: 0.02-30 GeVEnergy resolution: ~20%Effective area: 1500 cm2
Angular resol.: <0.50
Data taking: 1991-1994
Main results: Catalogue of point sourcesExcess in diffuse gamma rays
EGRET on CGRO (Compton Gamma Ray Observ.)
Data publicly available from NASA archive
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 11
Two results from EGRET paper
Enhancement in ringlike structure at 13-16 kpc
Called “Cosmic enhancement
Factor”Excess
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 12
Galactic coordinates: longitude l and latitude b
( l,b)=(0,0)=Galactic Center
( l,b)=(0,90)=North Galactic Pole
-900 < latitude b < 900
00 < longitude l < 3600
Galactocentric coordinates(left-handed to be
corotating!)Mathematics usually right-
handed!
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 13
Background + signal describe EGRET data!
Blue: background uncertainty
Background + DMA signal describe EGRET data!
Blue: WI MP mass uncertainty
50 GeV
70
I CI C
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 14
No SM
Electrons
No SM
Protons
Quarks fromWIMPS
Quarks in protons
What about background shape?
Background from nuclear interactions (mainly p+p-> π0 + X -> + X inverse Compton scattering (e-+ -> e- + ) Bremsstrahlung (e- + N -> e- + + N)Shape of background KNOWN if Cosmic Ray spectra of p and e- known
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 15
PYTHIA processes: 11 f+f' -> f+f' (QCD) 2370 12 f+fbar -> f'+fbar' 0 13 f+fbar -> g + g 0 28 f+g -> f + g 213068 g+g -> g + g 151053 g+g -> f + fbar 20 92 Single diffractive (XB) 1670 93 Single diffractive (AX) 1600 94 Double diffractive 70095 Low-pT scattering 0Prompt photon production:14 f+fbar -> g+γ 018 f+fbar -> γ +γ 029 f+g -> f +γ 1115 g+g -> g + γ 0114 g+g -> γ + γ 0
Contribution from various hadronic processes
2 GeV4
816
3264
diff.
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 16
Energy loss times of electrons and nuclei
Protons diffuse much faster than energy loss time, so expect SAME shape everywhere. Indeed observed: outer Galaxy can be fitted with same shape as inner Galaxy.
-1 = 1/E dE/dt
univ
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 17
Analysis of EGRET Data in 6 sky directions
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: inner Galaxy B: outer disc C: outer Galaxy
D: low latitude E: intermediate lat. F: galactic poles
Total 2 for all regions :28/36 Prob.= 0.8 Excess above background > 10σ.
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 18
Fits for 180 instead of 6 regions180 regions:80 in longitude 45 bins4 bins in latitude 00<|b|<50
50<|b|<100
100<|b|<200
200<|b|<900 4x45=180 bins >1400 data points. Reduced 2≈1 with 7% errorsBUT NEEDED IN ADDITION to 1/r2 profile, substructurein the form of 2 doughnut-likerings in the Galactic disc!
ONE RING COINCIDES WITHORBIT FROM CANIS MAJORDWARF GALAXY which losesmass along orbit by tidal forces
OTHER RING coincides with H2 ring
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 19
Background scaling factors agree withexpectations of gas- and CR densities
Background scaling factor = Data between 0.1 and 0.5 GeV/GALPROPGALPROP = computer code simulating our galaxy (Moskalenko, Strong)
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 20
x y
z
2002,Newberg et al. Ibata et al, Crane et al. Yanny et al.
1/r2 profile and ringsdetermined from inde-pendent directions
xy
xz
Expected Profile
v2M/r=cons.and
(M/r)/r2
1/r2
for const.rotation
curveDivergent for
r=0?NFW1/r
Isotherm const.
Dark Matter distribution
Halo profile
Observed Profile
xy
xz
Outer Ring
Inner Ring
bulge
tota
lDM
1/r2 halodisk
Rotation Curve
Normalize to solar velocity of 220 km/s
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 21
How does DM substructure formfrom tidal disruption of dwarf
galaxies?
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 23
The Milky Way and its 13 satellite galaxies
Canis Major
Tidal force ΔFG 1/r3
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 24
Tidal streams of dark matter from CM and Sgt
CM
Sgt
Sun
From David Law, Caltech
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 25
Artistic view of Canis Major Dwarf just below Galactic disc
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 26
Canis Major Dwarf orbits from N-body simulationsto fit visible ring of stars at 13 and 18 kpc
Canis Major leaves at 13 kpc tidal stream of gas(106 M☉ from 21 cm line), stars (108 M☉ ,visible), dark matter (1010 M☉, EGRET)
Movie from Nicolas Martin, Rodrigo Ibatahttp://astro.u-strasbg.fr/images_ri/canm-e.html
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 27
N-body simulation from Canis-Major dwarf galaxy
prograde retrograde
Ob
serv
ed
sta
rsR=13 kpc,φ=-200,ε=0.8
Canis Major (b=-150)
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 28
Gas flaring in the Milky Way
no ring
with ring
P M W Kalberla, L Dedes, J Kerp and U Haud, http://arxiv.org/abs/0704.3925
Gas flaring needs EGRET ring with mass of 2.1010M☉!
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 29
Enhancement of inner (outer) ring over 1/r2 profile 6 (8).Mass in rings 0.3 (3)% of total DM
Inner Ring coincides with ring of dust and H2 -> gravitational potential well!
H2
4 kpc coincides with ring ofneutral hydrogen molecules!H+H->H2 in presence of dust->grav. potential well at 4-5 kpc.
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 30
Bergstrom et al. astro-ph/0603632, Abstract:
we investigate the viability of the model using the DarkSUSY package to compute the gamma-ray and antiproton fluxes. We are able to show that their (=WdB et al) model is excluded by a wide margin from the measured flux of antiprotons.
Problem with DarkSUSY (DS):1) Flux of antiprotons/gamma in DarkSUSY: O(1) from DMA. However, O(10-2) from LEP data Reason: DS has diffusion box with isotropic diffusion -> DMA fills up box with high density of antiprotons2) Priors of DARKSUSY.(and other propagation models as well): a) static galactic magnetic fields are negligible b) gas is smoothly distributed c) propagation in halo and disk are the sameALL priors likely wrong and can change predictions for DM seaches by ORDER OF MAGNITUDE (and still ok with all observations!)
Do antiproton data exclude interpretation of EGRET data?
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 31
it is shown that Galactic cosmic rays can be effectively confined throughmagnetic reflection by molecular clouds,
Another propagation model including static magnetic fields and gas clouds and anisotropic diffusion
Integral excess of positrons in bulge because positrons are trapped in magnetic mirrors between gas clouds?
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 32
The van Allen belts are trapped cosmicrays in magnetic mirrors of earth
Radiation in inner belt: 25 Sv/yr inside space shipLethal dose for human: 3 Sv/hSatellites switch of electronics, wennentering dense radiation areas.
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 33
Escape time of cosmic rays andgrammage (distance x density)
10Be (t1/2 = 1.51 Myr) is cosmicClock: lifetime of cosmics 107 yrs.
In GALPROP by large haloIn CHANDRAN: by long trapping.
B/C=secondary/prim.determines grammage. In GALPROP by large haloIn Chandran: by reflectingmagnetic mirrors.
B/C determines grammage
10Be/9Be determines escape time
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 34
CHANDRAN model GALPROP model
Preliminary results from GALPROP with isotropic and anisotropic propagation
Summary: with anisotropic propagation you can send charged particleswhereever you want and still be consistent with B/C and 10Be/9Be
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 35
511 keV1809 keV (26Al)
Comparing radioactive isotopes with positron distribution (Knödlseder et al.)
Problem: expect most low energy positrons to originate from radioactive nuclei with β+ decay.But these are distributed in bulge AND disk.Positrons mostly in bulge. Why???
Unknown positron source only in bulge?? Light DM?Or simply: relativistic positrons escape indisk and annihilate in bulge?
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 36
astro-ph/0509298
NO annihilation in molecularclouds (MC), although 75% ofmass in MC. Why?Either volume of MC too smallOR MC are magnetic mirrorsas postulated by Chandran!
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 37
What aboutSupersymmetry?
Assume mSUGRA5 parameters: m0, m1/2, tanb, A, sign μ
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 38
EGRET excess interpreted as DM consistent with WMAP, Supergravity and electroweak constraints
Bulk
Too largeboostfactorfor EGRETdata
StauLSP
h<114
LSP largely Bino DM may be supersymmetric partner of CMB
Charginos, neutralinos and gluinos light
WMAP
EGRET
Stau coannihilation
mA resonance
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 39
Gauge unification perfect with SUSY spectrum from EGRET
With SUSY spectrum from EGRET + WMAP data and start values of couplings from final LEP data perfect gauge coupling unification!
Up
date
fro
m A
mald
i,
dB
, F
ürs
ten
au
, P
LB
260
1991
SM SUSY
Also b->s and g-2 in agreement with SUSY spectrum from EGRET
NO FREEparameter
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 40
Grand Unified Theories
Possible evolution of Universe
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 41
Celestial bodies collect DM in their cores by their high density.Annihilation can result in flux of HIGH energy neutrinos from sun (from b-decays or from Z-decays).
Neutrinos can be detected by large detectors,like Super-Kamiokande, Amanda, Ice-Cube, Baksanby the charged current interactions with nuclei,which yields muons in the detectors.
Indirect DM detection from solar neutrinos
EG
RET
SUN
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 42
WIMPs elastically scatter off nuclei => nuclear recoilsMeasure recoil energy spectrum in target
Direct Detection of WIMPs
0
0
H,Z
EGRET?CDMS
XENON10
If SUSY particle spectrumknown, elastic scattering X-section can be calculated
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 43Movie from M. Steinmetz, Potsdam
Clustering enhances flux from DMA by factor 20-200 (Dokuchaev et al.)
Galaxy formation starting from quantum fluctuations
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 44
Clustering of DM
An artist picture of what we should see if oureyes were sensitive to 3 GeV gamma rays and wewere flying with 220 km/s through the DM halo
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 45
8 physics questions answered SIMULTANEOUSLY if WIMP = thermal relic
• Astrophysicists: What is the origin of “GeV excess” of diffuse
Galactic Gamma Rays?• Astronomers: Why a change of slope in the galactic rotation
curve at R0 ≈ 11 kpc? Why ring of stars at 13 kpc? Why ring of molecular hydrogen at 4 kpc? Why S-shape in gas flaring? • Cosmologists: How is DM annihilating?A: into
quark pairs
How is Cold Dark Matter distributed?• Particle physicists: Is DM annihilating as expected in
Supersymmetry?
A: DM substructure
A: DM annihilation
A: standard profile + substructure
A: Cross sections perfectly consistent with mSUGRA for light gauginos, heavy squarks/sleptons
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 46
Summary
>>10σ EGRET excess shows intriguing hint that:
WIMP is thermal relic with expected annihilation into quark pairs
SPATIAL DISTRIBUTION of annihilation signal is signature for DMAwhich clearly shows that EGRET excess is tracer of DM by fact thatone can construct rotation curve and tidal streams from gamma rays.
DM becomes visible by gamma rays from fragmentation(30-40 gamma rays of few GeV pro annihilation from π0 decays)
Results rather model independent, since only KNOWN spectral shapes of signal and background used, NO model dependent calculations of abs.fluxes.Different shapes or unknown experimental problems may change the gamma ray flux and/or WIMP mass, BUT NOT the distribution in the sky.
DM interpretation strongly supported independently by gas flaring
DM interpretation perfectly consistent with Supersymmetry
Wim de Boer, Karlsruhe
Seminar Beijing, August 15, 2007 47
Summary on WIMP searches
Indirect detection: (SPACE EXPERIMENTS)
intriguing hint for signals from DMA for 60 GeV WIMP from gamma rays
Direct detection: (UNDERGROUND OBSERVATORIES) expected to observe signal in near future
IF we are not in VOID of clumpy DM halo
Direct production:(ACCELERATORS (LHC 2008-2018)): cannot produce WIMPs directly (too small cross section), BUT IF WIMPs are Lightest Supersymmetric Particle (LSP) THEN WIMPs observable in DECAY of SUSY particles
IF EVERY METHOD measures SAME WIMP mass, then PERFECT.In this case Dark Matter is the supersymmetric partner of the CMB!