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Dark Matter Interpretations of the WMAP Haze

Dark Matter Interpretations of the WMAP Haze. Daniel Cumberbatch CERCA Case Western Reserve University. Wilkinson Microwave Anisotropy Probe. Temperature anisotropies. Cosmic Microwave Background (CMB). Polarization anisotropies. Cosmological parameter estimation. Galactic Foregrounds.

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Dark Matter Interpretations of the WMAP Haze

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  1. Dark Matter Interpretations of the WMAP Haze Daniel Cumberbatch CERCA Case Western Reserve University CERCA Dark Matter Workshop March 2009

  2. Wilkinson Microwave Anisotropy Probe • Temperature anisotropies • Cosmic Microwave Background (CMB) • Polarization anisotropies • Cosmological parameter estimation • Galactic Foregrounds • Requires estimation before CMB signal extraction • Multiple sources • Dominant foregrounds: • Free-Free (Thermal Bremsstrahlung) • Thermal Dust • Synchrotron • Minimized in WMAP range (23 <  < 94 GHz) CERCA Dark Matter Workshop March 2009

  3. 23 GHz WMAP Haze • Residual microwave emission surrounding Galactic Centre • Radial symmetry, hard spectrum (I -0.25) CERCA Dark Matter Workshop March 2009

  4. WMAP Haze (2) • Gas thermally unstable • Insufficient gas abundance at 104 K (recombination lines) or 106 K (X-rays) • Excess Free-Free emission from hot gas (104 K <T<106 K) • Other Astrophysical Sources of synchrotronemission • Ultra-relativistic electrons from supernovae • Population of accretion-powered x-ray binaries (Bandyopadhyay et al. 0810.3674) • Dark Matter • WIMPs • Exciting Dark Matter (XDM) • Compact Composite Objects (CCO’s) CERCA Dark Matter Workshop March 2009

  5. WIMP Dark Matter • DM annihilation Rate(r)2hence increases towards GC • WIMP DM candidates annihilate to e+/- +…other SM particles e+/-propagate ISM e+/-interact with galactic magnetic field e+/-radiate via synchrotron (i.e. Haze) • Ingredients for DM contribution: • e+/- injection spectrum for WIMPs (i.e. per annihilation) • steady-statee+/- distribution in the galactic halo • fractional power of sync. rad. thate+/- of a given E contributes to a given frequency • total flux radiated by e+/- along a given line of sight CERCA Dark Matter Workshop March 2009

  6. e-e+,-  +,-+, ,W+W-, ZZ WIMP Dark Matter (2) Hooper, Finkbeiner & Dobler (PRD 76, 083012, (2007) ) Simple Case: • M=100 GeV, B(e-e+)=1 K-band (22 GHz) • NFW ((r)r -1 ) and(r)r -1.2 • Canonical diffusion parameters: B=10G, E~1016s, K~1028 0.33 cm s-1, L=2-3 kpc Parameter Scan: • Mvs. Boost Factor (BF)=<>/ <>can. • Hard Haze Spectrum reproduced • No significant boost factors required • In particular,  in areas of the focus point, A-funnel and bulk regions of the CMSSM possess the characteristics to reproduce the Haze (Careces & Hooper PRD 78, 123512 (2008) ) CERCA Dark Matter Workshop March 2009

  7. Canonical • diffusion • parameters: WIMP Dark Matter (3) Cumberbatch, Zuntz, Eriksen & Silk (arXiv:0902.0039) • Statistically significant WMAP Haze using Gibbs/ILC CMB estimators (<50°) • Significant Boost Factors required to fit haze (366<BF<1701) • Significant reduction (~50% @ 23GHz (<50°) ) in Haze when invoking slight spatial dependence in spectral index of soft synchrotron emission. CERCA Dark Matter Workshop March 2009

  8. m=100 GeV, B( )=1 WIMP Dark Matter (4) • Includes substructure enhancement: Mmin=10-6Msol., Msub./Mhalo~50%, NFW profiles aswell as host halo Borriello, Cuocu & Miele (arXiv:0809.2990) • Tinyakov&Tkachev / Uniform B-fields • Diffusion of e+e- neglected • <>~10-23 cm3 s-1 using TT model • <>~10-25 cm3s-1 for 10G B-field (including effects from DM substructure) • Similar/more stringent constraints from low frequency radio observations (~0.1-1 GHz) • LOFAR/SKA CERCA Dark Matter Workshop March 2009

  9. Einasto profile: K()~4x1028 0.33 cm s-1, L=4 kpc WIMP Dark Matter (5) Cholis et al. arXiv:0811.3641 • Boost factors ranging from 50 to 6000 • BF primarily due to non-cuspy profile and exponential decreasing B-field • Canonical diffusion parameters: • Consistency with PAMELA and ATIC CERCA Dark Matter Workshop March 2009

  10. Exciting Dark Matter (XDM) • Coupling to SM particles via scalar  (via Higgs mixing) • Majorana Fermion with excited state * (E>2me) • S-wave annihilations (CP=-1) (arXiv:0802.2922 Cholis, Goodenough & Weiner ) • For 2me< m< 2me+e- and  + - dominate • m >> me hence annihilation products are highly boosted  larger synchrotron fluxes (  2 ) CERCA Dark Matter Workshop March 2009

  11. Muon Channel m=100 GeV Direct Channel m=100 GeV Exciting Dark Matter (XDM) (2) • Good fit to WMAP Haze without significant boost factors (arXiv:0802.2922 Cholis, Goodenough & Weiner ) • High energy e+ provide good simultaneous fits to PAMELA data • (Cholis et al. arXiv:0810.5344) • Low energy e+e- also provide natural explanation to DAMA/LIBRA and • INTEGRAL observations (Finkbeiner et al. arXiv:0903.1037) CERCA Dark Matter Workshop March 2009

  12. (to be reconciled with Chandra) CCO Dark Matter • Formed from Axion domain wall collapse during QCD phase transition • B~1033 , R~O(10)m, M~1 ton (Zhitnitsky, JCAP 10, 010 2003) • Electrosphere of e+ surrounding CCO’s interacts with e- and p • from ISM, similar to quark stars (Alcock et al., ApJ 310, 261, 1986) • Assemblies of colour superconducting pairs of and  Proclaimed to be able to account for INTEGRAL, COMPTEL, Chandra and EGRET observations (Forbes&Zhitnitsky 0802.3830) • Fraction ‘1-g’ of energy from p annihilations radiated thermally: •  Therm. emitted in +∆. Hence for WMAP (i.e. /223-100 GHz): • Therm. Brem. Emission spectrum for T~104 K consistent with original • interpretation of WMAP haze as emission from gas with104K<T<106K • (Finkbeiner ApJ 614, 186, 2004) CERCA Dark Matter Workshop March 2009

  13. The “PLANCK Haze” • LFI 30-70 GHz (WMAP 23 - 94 GHz) • Re-confirmation of the WMAP haze • Predictions for a “Planck haze” at higher frequencies using HFI (100-857 GHz) • Fractional Synchrotron Power:  Cut-off in haze provides m constraint CERCA Dark Matter Workshop March 2009

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