CR signatures of Dipole-interacting Fermionic Dark Matter

Jae Ho HEO Theoretical High Energy group

jaeheo1@gmail.com

Yonsei University

2012 NRF Workshop @ Yonsei, June 8-9

Electromagnetic Interactions (effective dimension-5 dipole operators) Relic abundance (Strength of dipoles from present DM Relic abundance)

Cosmic ray signatures (positrons, antiprotons, photons)

Conclusion and Future work

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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

rrMG

rv

N1)( 2

2

2

α⇒=

World Composition

(mass-energy density)

Nobody knows these

• A spin ½ Dirac fermion with a mass roughly near the electroweak scale (10~1000 GeV) and its nonzero electro-magnetic dipole couplings.

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How dark is the dark matter??

P and T violations C and P violation unbroken U(1)Q

No discrete symmetry violatioins

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onAnnihilati DM from ,, γpe+

Antimattes: 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 creat other particles indirect detection

Effective Lagrangian

The effective Lagrangian with dimension-5 dipole couplings (larger than 10GeV)5 dipole

Rotate w.r.t Weinberg angle :

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EDM : CP violating interaction

MDM : no discrete symmetry

violations

photon) (shifted boson gauge ehyperchargfor strength field : B μν

ANNIHILATION PROCESS

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Annihilation rates

No suppression

Threshold suppression

by CP violating interaction

4

3

γ,Z-mediated s-channel processes.

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Fermionic annihilation products dominate. γ−Z interference plays important role for W-boson channel.

The contribution from ZH and neutrino channels is relatively small because of only Z-exachange

Annihilation fraction

CONSTRAINT FROM RELIC ABUNDANCE

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Relic density : Time evolution Boltzmann equation

Constant inverse freeze out temperature : xf~20 Constant annihilation rate : <σv> ~0.62pb

Thermal average for this annihilation

This implies the new physics will be O(Λ)∼10TeV

P.Gondolo NP B360, 124 (1991)

WMAP data : 0.0946 < ΩCDMh2<0.1286 (at 2σ)

WMAP Col. AJS 180, 330 (2009)

Source for Cosmic Ray Signals

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•Emissivity/energy at location x from the galactic center

Pair-annihilation

Injected particle spectra DM density at location x

(DM halo profile) : NFW, Moore, core isothermal, Einasto

Boost factor

•Fluxes

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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 : •Breit-Wigner resonance : In case that mediators have mass just below twice the DM mass annihilation rates can be enhanced

22 (x) (x) ><≥>< ρρ

⇒

Sommerfeld enhancement factor:

Same type of coupling as electric charge

presentat 10~ out-freezeat 0.3~

velocityDM :

3-

v

Cirelli et al., NPB 800, 204 (2008)

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Propagation of CRs

Diffusion equation:

Space diffusion Energy loss Convective wind

Scattering in IS (H, He atoms)

Positrons:

Antiprotons:

,0condition statesteady with thedensity number The =

∂∂

dTdn

tdTdn

model. zone- twoain conditionsboundary and

Casse, Lemoine, Pelleetier, PRD 65, 023002 (2002)

Three propagation models : MIN, MED, MAX Correspond to minimal(MIN), medium (MED), maximum(MAX) antiproton fluxes.

⇒ Deliahaye et al., PRD 77, 063527 (2008)

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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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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 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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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

γµ

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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/1205.1045 E. 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 −− −

CONCLUSION • The signals from spin ½ fermionic dark matters are

nicely fit the experimental measurements of the PAMELA, Fermi LAT with the enhancements of 30-50 factor.

• Simultaneously, no excess of antiproton over proton gives a severe restriction for this scenario. The MIN propagation model is viable, but likely ruled out for other propagation models, MED, MAX.

• The predicted signals from GH are within current unobservable experimental constraint.

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• The signals from regions close to GC as monoenergetic lines are under experimental exclusion limits of the Fermi LAT.

• The recent tentative analysis for the gamma ray excess can be accounted for, provided the subhalo boost factor of about 100.

• Our predicted signals from regions close to GC are in the potential probe at a planned experiment, AMS-02, with the better experimental method.

Thanks for the attention

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Future Work

Neutrino Telescopes : We need the magnetic profile of the SUN