overview of indirect dark matter detection jae ho heo theoretical high energy group...
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Overview of indirect dark matter detection
Jae Ho HEO Theoretical High Energy group
Yonsei University
2012 Jindo Workshop, Sep. 20-23
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Outlines
Jae Ho HEO 2
1. Introduction
2. Relic abundance
3. Indirect detections (positrons, antiprotons, photons)
4. Direct detections (annual modulation, iDM)
5. Triplet dark matter (no hypercharge Y=0, but weak charge SU(2) )
6. Future work
Heo, PRD 80, 033001 (2009)
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Jae Ho HEO 3
1930s Zwicky
L. Bergstrom Rept. Prog. Phys 63, 793 (2000)
Galactic Rotation Curves
• Newtonian prediction expect velocity to fall across the galactic disk as mass density falls.
• Observed rotational curves not consistent with visible distribution of matter.
• Supports the view that galaxies are immersed in a halo of so-called dark matter.
• Appears to make up ~83% of mass in the Universe
rv
r
rMG
r
vN
1)( 22
2
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World Composition(mass-energy density)
Nobody knows these
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Jae Ho HEO 5
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Jae Ho HEO 6
Targets
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Jae Ho HEO 7
Antimatters: rarely produced in astrophysical background.
Gamma rays: can transport freely long distance without energy loss or transmutations of the direction.
Dark matter particles can annihilate and create other particles relic abundance, indirect DM detection
Dark Matter Annihilation
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RELIC ABUNDANCE
Jae Ho HEO 8
Relic density : Time evolution Boltzmann equation
Constant inverse freeze out temperature : xF~20-25 for 10 GeV<M <1000 GeV 25-… for M>1000 GeV
Thermal average for this annihilationP. Gondolo NP B360, 124 (1991)
WMAP data : 0.1097 < WCDMh2<0.1165 (at 3s)
WMAP Col. AJS 180, 330 (2009)
From Boltzman distribution considered relativity
v~0.3 c
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Source for Cosmic Ray Signals
Jae Ho HEO 9
• Emissivity/energy at location x from GC Injected
particle spectra
DM density at location x(DM halo profile) : NFW, Moore, core Isothermal, Einasto
Boost factor
• Fluxes
Number of particles
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Jae Ho HEO 10
Boost factors
• Subhalo structure : less than 10 or 20 at GH, it can be very large ~100(000) around GC
• Sommerfeld nonperturbative effect : non-relativistic velocity and a long-range
attractive force For a singe Abelian massless vector with potential
• Breit-Wigner resonance : In case that mediators have mass just below twice the DM
mass annihilation rates can be enhanced
22 (x) (x)
Sommerfeld enhancement factor: presentat 10~
out-freezeat 0.3~
velocityDM :
3-
v
Cirelli et al., NPB 800, 204 (2008)
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Jae Ho HEO 11
Propagation of CRs
Particles, emitted by whatever process, must reach the detector (Earth) travelling through a medium with structure (the galaxy): interstellar gas, magnetic field
We have a standard diffusion model (Galprop) which assumes the galaxy is a flat cylinder with free scape at the boundaries
Space diffusion Energy loss Convective wind
Scattering in IS (H, He atoms)
Casse, Lemoine, Pelleetier, PRD 65, 023002 (2002)
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Jae Ho HEO 12
Two-Zone model
Positrons:
Antiprotons:
,0condition statesteady with thedensity number The
dT
dn
tdT
dn
model. zone- twoain conditionsboundary and
Three propagation models : MIN, MED, MAX Correspond to minimal(MIN), medium (MED), maximum(MAX) antiproton fluxes.
Deliahaye et al., PRD 77, 063527 (2008)
L=3-20 kpc
h=0.1 kpc
R=20 kpc
8.5 kpc
SUNH, He
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Jae Ho HEO 13
A model with magnetic dipoleHeo, Kim, arXiv:1207.1341
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Jae Ho HEO 14
Positrons
• Predicted signals have almost no difference in halo profiles or diffusion models.
• Predicted fractions exhibit rather sharp distribution at E~M, since our candidate can directly annihilate into electron-positron pair.
• Predicted signals with the boost factor, 30-80 nicely fit measurements of the PAMELA, Fermi LAT, etc
• We predict that an enhancement of 16 factor comes from Sommerfeld effect, and the rest 2-5 enhancements from the subhalo structure (dark clumps).
Solar modulation at low energies (<10 GeV)
Gleeson et al., Astropart. Phys. 154, 1011 (1968)
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Jae Ho HEO 15
Gamma-Rays from GH
• Almost no difference in the halo profiles
• Slightly touch EGRET anomaly
The predicted signals are within the current unobservable experimental constraint.
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Jae Ho HEO 16
Antiprotons
• No difference in halo profiles
• Sensitive to the propagation models
• Viable in MIN propagation model
• Likely rule out for other propagation Models, MED and MAX
• The MED propagation parameters are in uncertainty of one order of magnitude.
• The MED propagation model might be viable, if we consider uncertainty of Propagation parameters.
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Jae Ho HEO 17
Gamma-Rays from around GC
Most complex regions in galaxy due to many possible sources : difficult to model the diffuse emission, and discriminate the DM annihilation signals from background.
Smoking-gun signatures : monochromatic gamma-ray lines
state final Zfor angle rgby Weingben suppressio Additional
dipole magneticby Suppressed 4
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Jae Ho HEO
18
Signals from around GC
• Predictions are under experimental exclusion limits
100)(~t enhancemen subhalo a
with explained becan
GeV 130 around mass DMat
excess s/cm 103-1
analysis, tativerecent ten The327-
• The predicted signals are in the potential probe at the AMS-02 with the better experimental method (energy resolution 1.5-2%, Fermi LAT 11-13%).
C. Weniger, hep-ph/1205.2797E. Tempel, A. Hektor, M. Raidal,hep-ph/1205.1045
A. Kounine, astro-ph/1009.5349; http://ams.cern.ch.
Fermi. Col., astro-ph/1205.12739
s/cm 1010~ 32930
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Jae Ho HEO 19
Direct dark matter detection
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Jae Ho HEO 20
Normal dark matter (elastic scat-tering)
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Jae Ho HEO 21
Inelastic dark matter
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Jae Ho HEO 22
M=50 GeV M=100 GeV
M=300 GeV
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Jae Ho HEO 23
Triplet Dark Matter
• Extend the SM with an exotic lepton triplet E per family
• Anomaly constraints provide gauge charge of E
Heo, PRD 80, 033001 (2009)
Fermion gauge charges
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Jae Ho HEO 24
• There are no photon and Z boson couplings : This avoids direct detection constraint.
• Neutral and charged Es have mass splitting by radia-tive correction (~165 MeV)
:induce inelastic scattering for direct detection, but splitting is large -> also avoid direct detection con-straint.
I need consider indirect detection of this model
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Thanks for the atten-tion
Jae Ho HEO 25
Future Work
• Fermion triplet dark matter• Scalar triplet dark matter
• Neutrino Telescopes : We need the magnetic profile of the SUN