Conservative Constraints on Dark Matter Self Annihilation Rate

Conservative Constraints on Dark Matter Self Annihilation Rate Thomas Jacques 2009-07-13, TeVPA 2009

Indirect Detection Indirect detection often focuses on choosing a model, and comparing predicted flux to observed flux Great for testing a model, not so great for finding the nature of DM

Indirect Detection Indirect detection often focuses on choosing a model, and comparing predicted flux to observed flux Great for testing a model, not so great for finding the nature of DM So, what can we deduce about DM, in a model independent way, from it s annihilation flux? Great progress in recent years; A number of bounds on annihilation cross section/decay width We expand and strengthen these limits, focusing on two final states, γγ and e + e - We can be confident that these upper limits are robust

γγ χ χ γ γ Photon line Smoking Gun χ χ γ γ Common final state, even if small branching ratio Don t know branching ratio: We constrain this channel only from Mack, Jacques, Beacom, Bell, Yuksel; Phys.Rev.D78:063542 (2008)

Annihilation Flux Annihilation flux from a nearby source: dφ γ de = 1 2 σ Av Br(γγ) R 0 ρ(s) 2 4πm 2 χ dl dn γ de

Annihilation Flux Annihilation flux from a nearby source: dφ γ de = 1 2 σ Av Br(γγ) R 0 ρ(s) 2 4πm 2 χ dl dn γ de Flux in some direction depends on:

Annihilation Flux Annihilation flux from a nearby source: dφ γ de = 1 2 σ Av Br(γγ) R 0 ρ(s) 2 4πm 2 χ dl dn γ de Flux in some direction depends on: Cross section,

Annihilation Flux Annihilation flux from a nearby source: dφ γ de = 1 2 σ Av Br(γγ) R 0 ρ(s) 2 4πm 2 χ dl dn γ de Flux in some direction depends on: Cross section, Integral along the line of sight of the DM density squared,

Annihilation Flux Annihilation flux from a nearby source: dφ γ de = 1 2 σ Av Br(γγ) R 0 ρ(s) 2 4πm 2 χ dl dn γ de Flux in some direction depends on: Cross section, Integral along the line of sight of the DM density squared, The γ-ray spectrum per annihilation (Dirac delta)

Annihilation Flux Annihilation flux from a nearby source: dφ γ de = σ Av 2 γγ J Ω J 0 1 4πm 2 χ dn γ de

Density profiles Minimize uncertainty by looking at large angular regions Focus on conservative Kravtsov profile, but show results for other profiles 1 30

Observation Regions Galactic Center Our main flux source; lots of data M31 (Andromeda) Relatively weak upper limits on σav Analysis very similar to GC case Cosmic Annihilation Diffuse photon flux from extragalactic DM annihilation Analysis includes integral over redshift, photon attenuation, DM clumping factor Use data from INTEGRAL, COMPTEL, EGRET, HEGRA, CELESTE, HESS, SMM Cover broad range of energies: ~10-5 to ~10 4 GeV

Results 10-20 < " A v > ## [cm 3 s -1 ] 10-22 10-24 10-26 10-28 10-30 10-32 DIFFUSE PHOTON BACKGROUND INTEGRAL CGRO MW EGRET M31 CELESTE M31 HEGRA M31 HESS GC RIDGE 10-34 10-5 10-3 10-1 10 1 10 3 10 5 m! [GeV] Very conservative analysis Results more general than they appear: We integrate the signal over a large energy bin, so results are valid for an annihilation spectrum as wide as our analysis bin (0.4 in log 10 E) At worst, our limit would be increased by a factor of several for a broad annihilation spectrum (except for INTEGRAL/HEGRA)

Results 10-16 10-18 KKT Using Br(γγ) = 10-4, find a limit on the total cross section < " A v > total [cm 3 s -1 ] 10-20 10-22 10-24 10-26 Gamma Rays Br(##!=10-4 Natural Scale Unitarity Bound Neutrinos Br($$!=1 10-28 10-30 10-5 10-3 10-1 10 1 10 3 10 5 m! [GeV]

Positron Excess from N. Bell & T. Jacques; Phys.Rev.D79:043507 (2008)

Positron Excess Nearby Pulsars? Dark Matter Annihilation? No antiproton excess Large annihilation cross section from N. Bell & T. Jacques; Phys.Rev.D79:043507 (2008)

Positron Excess Nearby Pulsars? Dark Matter Annihilation? No antiproton excess Large annihilation cross section Want to constrain annihilation to e + e - Look for associated gamma-ray emission from N. Bell & T. Jacques; Phys.Rev.D79:043507 (2008)

Positron Excess Nearby Pulsars? Dark Matter Annihilation? No antiproton excess Large annihilation cross section Want to constrain annihilation to e + e - Look for associated gamma-ray emission Internal Bremsstrahlung No dependence on Magnetic field, ISRF, Diffusion Hard gamma rays near the endpoint, and background decreases with energy χ χ e e + from N. Bell & T. Jacques; Phys.Rev.D79:043507 (2008)

Internal Brem Spectrum Similar to analysis for gamma-gamma case Different spectrum dφ γ de = σ Av 2 dn γ de = 1 σ tot dσ IB de γ dσ IB de = σ tot α J Ω J 0 1 4πm 2 χ Eπ [ ln ( s m 2 e dn γ de 2 s=4mχ s =4mχ(mχ-E) ) 100 E 2 dn γ /de [GeV annihilation -1 ] 1 10 1 ][ 1+ ( s 100 1000 E [GeV] s ) 2 ] Beacom, Bell, Bertone, Phys.Rev.Lett.94:171301 (2005)

Constraints <σ A v> e + e - [cm 3 s -1 ] 10-20 10-21 10-22 10-23 10-24 10-25 10-26 10-27 COMPTEL EGRET Natural Scale CELESTE H.E.S.S. 10-28 10-3 10-2 10-1 10 0 10 1 10 2 10 3 10 4 10 5 m χ [GeV] Br(ii ) < σ A v > total [cm 3 s -1 ] 10-16 10-18 10-20 10-22 10-24 10-26 10-28 10-30 e + e - γγ KKT µ + µ - τ + τ - Unitarity Bound Natural Scale 10-32 10-3 10-2 10-1 10 0 10 1 10 2 10 3 10 4 10 5 m χ [GeV] νν Thomas Jacques - TeV PA 2009.07.13

<σ A v> e + e - [cm 3 s -1 ] 10-20 10-21 10-22 10-23 10-24 10-25 10-26 10-27 COMPTEL EGRET Constraints 10-20 Natural Scale CELESTE H.E.S.S. 10-28 10-3 10-2 10-1 10 0 10 1 10 2 10 3 10 4 10 5 m χ [GeV] Br(ii ) < σ A v > total [cm 3 s -1 ] 10-16 10-18 10-22 10-24 10-26 10-28 10-30 e + e - γγ KKT µ + µ - τ + τ - Unitarity Bound Natural Scale 10-32 10-3 10-2 10-1 10 0 10 1 10 2 10 3 10 4 10 5 m χ [GeV] νν Thomas Jacques - TeV PA 2009.07.13 Cirelli, Kadastik, Raidal & Strumia arxiv:0809.2409