1 / 5

IceCube Galactic Halo Analysis

IceCube Galactic Halo Analysis.

berke
Télécharger la présentation

IceCube Galactic Halo Analysis

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. IceCube Galactic Halo Analysis WIMPs could annihilate in the Galactic dark matter halo and produce observable neutrino signals. IceCube has looked for signals from the Galactic Center and halo and was able to constrain the WIMP self-annihilation cross section, <sAv>, as function of its mass, mc. Note this search is fundamentally different from indirect searches targeting the Sun, which probe the WIMP-Nucleon scattering cross section. • Galactic halo analysis searched for a neutrino anisotropy on the northern hemisphere in the 22-string sample (2007-2008) • Galactic Center, search for an excess in down-going events in direction of the GC • Observations in both analyses were consistent with background expectations • Results start to constrain WIMP models with large boost factors as motivated by PAMELA observations Distribution Constrain Measure SUSY Model “2 WIMPs per annihilation” Isotropic emission Abbasi et al (2011) arXiv:1101.3349v1 (accepted PRD)

  2. Backup slides

  3. 90° 60° 30° 0° -30° -60° -90° Galactic Halo Analysis • 5114 Eventsafter selectionfrom -5° to +85° declination • Nobserved in on and off source regions are consistent with each other. • No excess flux in the region, closer to the Galactic Center, proceed to set limits 1389 1367 Carsten Rott (CCAPP)

  4. Comparison of Limits – Galactic Halo cc  mm cc tt • Neutrino limits start to constrain dark matter models motivated by the lepton excess in PAMELA / Fermi • Using the partial instrumented (~25%) IceCube detector and one year of data we can set limits in the physical interesting parameter space arXiv:1101.3349v1 (accepted PRD) Carsten Rott (CCAPP)

  5. IceCube Galactic Center Analysis not to scale • Dark Matter profiles are peaked at the Galactic Center • Optimize the size of the on-source region • δ = 8ο • Compare the amount of events in the on- and off-source region • From off-source prediction 798919 events • On-source observed: 798842 events • Galactic Center is above the horizon events are down-going in IceCube • Use starting events to reduce atmospheric muon background veto region fiducial volume off source on source off source -d Zenith d GC DRA=-180o -20o -dd 20o 180o Carsten Rott (CCAPP)

More Related