Overview of indirect dark matter detection

Jae Ho HEO Theoretical High Energy group

jaeheo1@gmail.comYonsei University

2012 Jindo Workshop, Sep. 20-23

Outlines

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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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1930s ZwickyL. 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

rrMG

rv

N1)( 2

2

2

World Composition(mass-energy density)

Nobody knows these

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Targets

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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

RELIC ABUNDANCE

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Relic density : Time evolution Boltzmann equation

Constant inverse freeze out temperature : xF~20-25 for 10 GeV<M <1000 GeV 25-… for M>1000 GeVThermal 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 relativityv~0.3 c

Source for Cosmic Ray Signals

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• 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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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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Propagation of CRs

Particles, emitted by whatever process, must reach the detector (Earth) travelling through a medium with structure (the galaxy): interstellar gas, magnetic fieldWe 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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Two-Zone model

Positrons:

Antiprotons:

,0condition statesteady with thedensity number The

dTdn

tdTdn

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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A model with magnetic dipoleHeo, Kim, arXiv:1207.1341

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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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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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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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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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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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Direct dark matter detection

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Normal dark matter (elastic scat-tering)

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Inelastic dark matter

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M=50 GeV M=100 GeV

M=300 GeV

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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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• 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

Thanks for the atten-tion

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Future Work

• Fermion triplet dark matter• Scalar triplet dark matter

• Neutrino Telescopes : We need the magnetic profile of the SUN