Sensitivity of the IceCube neutrino detector to dark matter annihilating in dwarf galaxies (original) (raw)
Related papers
IceCube search for dark matter annihilation in nearby galaxies and galaxy clusters
Physical Review D, 2013
We present the results of a first search for self-annihilating dark matter in nearby galaxies and galaxy clusters using a sample of high energy neutrinos acquired in 339.8 days of livetime during 2009/10 with the IceCube neutrino observatory in its 59-string configuration. The targets of interest include the Virgo and Coma galaxy clusters, the Andromeda galaxy and several dwarf galaxies. We obtain upper limits on the cross section as function of the WIMP mass between 300 GeV and 100 TeV for the annihilation into bb , W + W − , τ + τ − , µ + µ − and νν. A limit derived for the Virgo cluster, when assuming a large effect from subhalos, challenges the WIMP interpretation of a recently observed GeV positron excess in cosmic rays.
Neutrino telescopes’ sensitivity to dark matter
Physical Review D, 2002
The nature of the dark matter of the Universe is yet unknown and most likely is connected with new physics. The search for its composition is under way through direct and indirect detection.
Astrophysical neutrinos, PeV events at IceCube, and the Direct Detection of Dark Matter
We study the possibility of detecting dark matter directly via a small but energetic component that is allowed within present-day constraints. Drawing closely upon the fact that neutral current neutrino nucleon interactions are indistinguishable from DMnucleon interactions at low energies, we extend this feature to high energies for a small, non-thermal but highly energetic population of DM particle χ, created via the decay of a significantly more massive and long-lived non-thermal relic φ, which forms the bulk of DM. If χ interacts with nucleons, its cross-section, like the neutrino-nucleus coherent cross-section, can rise sharply with energy leading to deep inelastic scattering, similar to neutral current neutrino-nucleon interactions at high energies. Thus, its direct detection may be possible via cascades in very large neutrino detectors. As a specific example, we apply this notion to the recently reported three ultra-high energy PeV cascade events clustered around 1 − 2 PeV at IceCube (IC). We discuss the features which may help discriminate this scenario from one in which only astrophysical neutrinos constitute the event sample in detectors like IC.
The IceCube Neutrino Observatory Part IV: Searches for Dark Matter and Exotic Particles
The cubic-kilometer sized IceCube neutrino observatory, constructed in the glacial ice at the South Pole, offers new opportunities for neutrino physics with its in-fill array "DeepCore". In particular, the use of the outer layers of the IceCube detector as a veto allows low-energy neutrino searches to be performed in the southern sky. This makes the Galactic Center, an important target in searches for self-annihilating dark matter, reachable for IceCube. In this contribution we present the results of the first Galactic Center analysis using more than 10 months of data taken with the 79-string configuration of IceCube-DeepCore, with a special focus on low WIMP masses reaching a sensitivity as low as 30 GeV. We also present the status of an analysis extending the sensitivity to WIMP masses up to the TeV scale.
Search for Dark Matter from the Galactic Halo with the IceCube Neutrino Observatory
2011
Self-annihilating or decaying dark matter in the Galactic halo might produce high energy neutrinos detectable with neutrino telescopes. We have conducted a search for such a signal using 276 days of data from the IceCube 22-string configuration detector acquired during 2007 and 2008. The effect of halo model choice in the extracted limit is reduced by performing a search that considers the outer halo region and not the Galactic Center. We constrain any large scale neutrino anisotropy and are able to set a limit on the dark matter self-annihilation cross section of σAv ≃ 10 −22 cm 3 s −1 for WIMP masses above 1 TeV, assuming a monochromatic neutrino line spectrum. PACS numbers: 95.35.+d,98.35.Gi,95.85.Ry
Search for dark matter from the Galactic halo with the IceCube Neutrino Telescope
2011
There is compelling observational evidence for the existence of dark matter. Although knowledge of its underlying nature remains elusive, a variety of theories provide candidate particles [1]. Among those are supersymmetry [2] and universal extra dimensions [3], both of which predict new physics at the electro-weak scale and, in most scenarios, introduce a light, and stable (or long lived) particle that exhibits the properties of a weakly interacting massive particle (WIMP)[4].
Monthly Notices of …, 2011
Due to their large dynamical mass-to-light ratios, dwarf spheroidal galaxies (dSphs) are promising targets for the indirect detection of dark matter (DM) in γ-rays. We examine their detectability by present and future γ-ray observatories. The key innovative features of our analysis are: (i) We take into account the angular size of the dSphs; while nearby objects have higher γ ray flux, their larger angular extent can make them less attractive targets for background-dominated instruments. (ii) We derive DM profiles and the astrophysical J-factor (which parameterises the expected γ-ray flux, independently of the choice of DM particle model) for the classical dSphs directly from photometric and kinematic data. We assume very little about the DM profile, modelling this as a smooth split-power law distribution, with and without sub-clumps. (iii) We use a Markov Chain Monte Carlo (MCMC) technique to marginalise over unknown parameters and determine the sensitivity of our derived J-factors to both model and measurement uncertainties. (iv) We use simulated DM profiles to demonstrate that our J-factor determinations recover the correct solution within our quoted uncertainties.