Miami 2010 Probing Dark Matter With Neutrinos Ina Sarcevic

Miami 2010Probing Dark Matter with NeutrinosIna SarcevicErkoca, Gelmini, Reno and Sarcevic, Phys. Rev D81 (2010).Erkoca, Reno and Sarcevic, Phys. Rev. D 82 (2010).

Dark Matter Searches Direct searches:look for DM interactions with targetnuclei (XENON, CDMS, DAMA,CoGeNT)Indirect searches:DM annihilation producing electrons,positrons, gamma-rays (PAMELA, ATIC,FERMI/LAT, HESS ) and neutrinos(IceCube, KM3Net )

PAMELA Positron Fraction

FERMI Cosmic Ray Electron Spectrum

Neutrino Flux from DM Annihilationin the Galactic CenterErkoca, Gelmini, Reno and Sarcevic,Phys. Rev. D81, 096007 (2010) Model independent DM signals withneutrino-induced upward and containedmuons and cascades (showers) Predictions for IceCube and Km3Net

Neutrino Flux from Dark MatterNeutrino flux from DM annihilation/decay:here R for DM annihilation is:and for DM decay:

Defineas:distance from us in the direction of thecone-half angle from the GCdensity distribution of dark mater halosdistance of the solar system from the GClocal dark matter density near the solarsystem

Neutrino Flux () at the ProductionNeutrinos can be produced directly orthrough decays of leptons, quarks andgauge bosons:

Detection:neutrinos interactingbelow detector or in the detectorproducing muons Signals: upward and containedmuons and cascade/showers Upward muons lose energy beforereaching the detector

Energy loss of the muons over a distance dz :α : ionization energy loss α 10-3GeVcm2/g. β : bremsstrahlung, pair production andphotonuclear interactions β 10-6cm2/g. Relation between the initial and the finalmuon energy: Muon range:

Contained and Upward Muon FluxContained muon flux is given bydφµ dEµ EmaxdEνEµ dNdEν dσν (Eν )NA ρdEµUpward muon flux is given by Rµ (Eµi ,Eµ ) EmaxdφµdNβρz e dzdEνNA ρdEµdEνi0Eµdσν (Eν )i Psurv (Eµ , Eµ )dEµ

dφsh dEsh EmaxdEνEsh dφνdEν dσν (Eν , Eν Esh )NA ρdEsh

Neutrino Energy Distributionchannel :channels :

Muon Flux

Muon Flux for Different DMAnnihilation Modes

Muon Rates

Hadronic Shower Spectra withouttrack-like events

Probing the Nature of Dark Matterwith NeutrinosErkoca, Reno and Sarcevic, Phys. Rev. D82,113006 (2010)DM candidates: gravitino, Kaluza-Kleinparticle, a particle in leptophilic models. Dark matter signals: upward andcontained muon flux and cascades(showers) from neutrino interactions Experimental signatures that woulddistinguish between different DMcandidates

Contained Muon Flux

Contained Muon Flux

Contained muon flux

DM Detection with NeutrinoTelescopesIceCUBE : 1 km3 neutrino detector at South Pole detects Cherenkov radiation from the chargedparticles produced in neutrino interactions contained and upward muon events and showers contained muons from GC showers from GC with IceCUBE DeepCoreKM3Net : a future deep-sea neutrino telescope contained and upward muon events andshowers upward muons from GC

Summary Neutrinos could be used to detect darkmatter and to probe its physical origin Contained and upward muon flux issensitive to the DM annihilation mode andto the mass of dark matter particleCombined measurements of cascade eventsand muons with IceCube DeepCore andKM3Net look promising Neutrinos can probe DM candidates, suchas gravitino, Kaluza-Klein DM, and aparticle in leptophilic models

Erkoca, Gelmini, Reno and Sarcevic, Phys. Rev D81 (2010). Erkoca, Reno and Sarcevic, Phys. Rev. D 82 (2010). Ina Sarcevic Probing Dark Matter with Neutrinos Miami 2010 Direct searches: look for DM interactions with target .