Neutralino Dark Matter as the Source of the WMAP Haze

Transcription

1 Neutralino Dark Matter as the Source of the WMAP Haze Gabriel Caceres Penn State University & Fermilab Based on work with Dan Hooper INT Summer School 2009

2 Dark Matter: The Evidence

3 The Search Direct Detection Indirect Detection Signal from the Sun Neutrinos Signal from Galactic Center/Halo Gamma-rays Neutrinos Positrons/Antiprotons Synchrotron Radiation

4 The Search Direct Detection Indirect Detection Signal from the Sun Neutrinos Signal from Galactic Center/Halo Gamma-rays Neutrinos Positrons/Antiprotons Synchrotron Radiation

5 Synchrotron Radiation χ... e-, e+ χ Electrons/positrons produced in dark matter annihilations propagate through the galactic magnetic field. For electroweak scale dark matter the emitted synchrotron radiation falls within range of WMAP frequency bands.

6 WMAP Haze WMAP: CMB & Galactic Foregrounds... WMAP

7 WMAP Haze WMAP: CMB & Galactic Foregrounds... Free free CMB Synchrotron T & S Dust WMAP

8 WMAP Haze 22 GHz =

9 WMAP Haze 22 22GHz GHz = After known foregrounds are subtracted, an excess appears in the residual maps within the inner ~20 around the Galactic Center

10 WMAP Haze Doug Finkbeiner suggested in 2004 that the excess emission could be synchrotron radiation due to dark matter annihilation products. (astro-ph/ ) Similar morphology observed in all WMAP frequency bands D. Hooper, G. Dobler and D. Finkbeiner, PRD, arxiv:

11 WMAP Haze Determine dark matter distribution required to explain the Haze ραr -1.2 ρ(r) α r ρ(r) α r -1 D. Hooper, G. Dobler and D. Finkbeiner, PRD, arxiv: (NFW) -1.2 Although the fit depends on the diffusion parameters, the range of slopes -1.1 to -1.3 is fairly robust

12 WMAP Haze Determine dark matter distribution required to explain the Haze ( ) ρ α r -1 ραr NFW -1.2 ρ(r) α r ρ(r) α r -1 D. Hooper, G. Dobler and D. Finkbeiner, PRD, arxiv: (NFW) ( ) ρ α r -1.5 Moore et al -1.2 Although the fit depends on the diffusion parameters, the range of slopes -1.1 to -1.3 is fairly robust

13 WMAP Haze Using the astrophysical data, the particle properties required to explain the Haze can be determined DM annihilation cross section bb WW ZZ ττ Spectrum bb WW ZZ µµ ee ee ττ µµ D. Hooper, G. Dobler and D. Finkbeiner, PRD, arxiv:

14 Supersymmetry Symmetry between Fermions and Bosons New particles introduced Neutralino LSP, Dark Matter candidate >100 free parameters

15 CMSSM Constrained Minimal Supersymmetric Standard Model (CMSSM) reduces free parameters through theoretically oriented assumptions at the GUT scale

16 CMSSM Constrained Minimal Supersymmetry Standard Model (CMSSM) reduces free parameters through theoretically oriented assumptions at the GUT scale Through 5 parameters, the entire particle spectrum can be calculated (here using the DarkSUSY package): Universal gaugino mass: m½ Universal scalar mass: m0 Universal tri-linear scalar coupling: A0 Ratio of v.e.v. of the two Higgs doublets: tan β Sign of the Higgsino mass parameter: μ

17 CMSSM (Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50) GC and D. Hooper, PRD, arxiv:

18 CMSSM Coannihilation (Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50) GC and D. Hooper, PRD, arxiv:

19 CMSSM Bulk Coannihilation (Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50) GC and D. Hooper, PRD, arxiv:

20 CMSSM A-funnel Bulk Coannihilation (Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50) GC and D. Hooper, PRD, arxiv:

21 CMSSM Focus Point Bulk Coannihilation A-funnel (Done for μ>0, tanβ 3,10,35,50 and μ<0, tanβ 35,50) GC and D. Hooper, PRD, arxiv:

22 Focus Point Cross Section Annihilation Modes GC and D. Hooper, PRD, arxiv:

23 WMAP Haze Dark Matter requirements to produce the Haze for relevant supersymmetric annihilation channels: DM annihilation cross section Spectrum

24 CMSSM Comparison Compare with Haze requirements

25 Detection Prospects Direct Detection Neutrino Detection

26 Detection Prospects Direct Detection Neutrino Detection GC and D. Hooper, PRD, arxiv:

27 Summary The excess emission observed by WMAP, known as the WMAP Haze, could be explained by WIMPs annihilating in the Galactic Center. Much of the CMSSM parameter space provides us with a Neutralino which is capable of producing the WMAP Haze In particular: Most of the Focus Point and A-funnel provide a viable candidate Part of the Bulk (high tanβ) can accomodate the desired properties The Stau coannihilation does not satisfy the requirements of the Haze Very positive detection prospects for models in the Focus Point region