1 / 9

Challenges in Revealing Dark Matter from the High Energy Gamma-Ray Background (Continuum)

Challenges in Revealing Dark Matter from the High Energy Gamma-Ray Background (Continuum). Ranga-Ram Chary Spitzer Science Center, Caltech rchary@caltech.edu. The Different Galactic Components. GALACTIC PLANE l~0, b~0. GALACTIC ANTICENTER l~180, b~75. Isotropic Component.

quanda
Download Presentation

Challenges in Revealing Dark Matter from the High Energy Gamma-Ray Background (Continuum)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Challenges in Revealing Dark Matter from the High Energy Gamma-Ray Background (Continuum) Ranga-Ram Chary Spitzer Science Center, Caltech rchary@caltech.edu

  2. The Different Galactic Components GALACTIC PLANE l~0, b~0 GALACTIC ANTICENTER l~180, b~75 Isotropic Component p-p component EB component IC Component Gas Scale Height is smaller than Radiation Field Scale Height Hunter et al., Bertsch et al.

  3. Contribution of Dark Matter to the E~150 MeV Background Strong Dependence on Emissivity and Halo Core Radius

  4. Current Constraints on the Spectrum of the Residual Halo Emission: Looks more like γ-raypulsars Isotropic EBL ~ E-2.1 Anisotropic Halo Component ~ E-1.7

  5. Uncertainty I: Anisotropic IC

  6. The Radiation Field R=5 kpc, z=0 kpc R=5 kpc, z=1.5 kpc R=8.5 kpc, z=1.5 kpc The Radial Scale Length of the ISRF Energy Density is ~3 kpc The Scale Height is ~1.5 kpc In contrast, gas Scale Height is ~100 pc

  7. A Visual Approach Although the average intensity is the same, anisotropy is x10-100 greater on the right

  8. Uncertainty II: The Cosmic Ray Spectrum and Intensity - Strong Dependence on Distance from SNR R=5 kpc, z=0 kpc R=5 kpc, z=1.5 kpc R=8.5 kpc, z=1.5 kpc

  9. The Problem List For our galaxy: • CR propagation model (Can it be done ?) • Azimuthal angle dependent ISRF using more recent Sloan, Spitzer and 2MASS data To Pinpoint Dark Matter Consider: • Deep GLAST pointings at edge on galaxies – still need to remove the IC component • Of course, dwarf galaxies and clusters might remain the best place to identify dark matter • Angular power spectrum of CGRB is likely to be dominated by unresolved blazars

More Related