Neutrino constraints on the dark matter total annihilation cross section

Yüksel, Hasan; Horiuchi, Shunsaku; Beacom, J. F.; Ando, Shinʼichiro

doi:10.1103/physrevd.76.123506

Cited by 162 publications

(217 citation statements)

References 70 publications

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“…The overall normalization of the flux is affected by the value of J avg,k , scaling as ρ k . For instance, for different profiles [218][219][220], astrophysical uncertainties can induce up to a factor of ∼100 (∼6) for annihilations [216,217] (decays [214]). For concreteness, in what follows we present results using the Navarro, Frenk and White (NFW) profile [219], with J avg,1 = 2 [214] and J avg,2 = 5 [216].…”

Section: Searching Neutrinos From Mev Dmmentioning

confidence: 99%

“…In this section, and following and reviewing the approach of [214][215][216][217], we consider this case and evaluate the potential neutrino flux from DM annihilation (decay) in the whole Milky Way, which we compare with the relevant backgrounds for detection. In such a way, we obtain an estimate of the sensitivity on the DM annihilation cross section (lifetime) by LENA.…”

Section: Introductionmentioning

confidence: 99%

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The next-generation liquid-scintillator neutrino observatory LENA

Wurm

Beacom

Bezrukov

et al. 2012

Astroparticle Physics

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2As part of the European LAGUNA design study on a next-generation neutrino detector, we propose the liquid-scintillator detector LENA (Low Energy Neutrino Astronomy) as a multipurpose neutrino observatory. The outstanding successes of the Borexino and KamLAND experiments demonstrate the large potential of liquid-scintillator detectors in low-energy neutrino physics. Low energy threshold, good energy resolution and efficient background discrimination are inherent to the liquidscintillator technique. A target mass of 50 kt will offer a substantial increase in detection sensitivity.At low energies, the variety of detection channels available in liquid scintillator will allow for an energy-and flavor-resolved analysis of the neutrino burst emitted by a galactic Supernova. Due to target mass and background conditions, LENA will also be sensitive to the faint signal of the Diffuse Supernova Neutrino Background. Solar metallicity, time-variation in the solar neutrino flux and deviations from MSW-LMA survival probabilities can be investigated based on unprecedented statistics. Low background conditions allow to search for dark matter by observing rare annihilation neutrinos. The large number of events expected for geoneutrinos will give valuable information on the abundances of Uranium and Thorium and their relative ratio in the Earth's crust and mantle. Reactor neutrinos enable a high-precision measurement of solar mixing parameters. A strong radioactive or pion decay-at-rest neutrino source can be placed close to the detector to investigate neutrino oscillations for short distances and sub-MeV to MeV energies.At high energies, LENA will provide a new lifetime limit for the SUSY-favored proton decay mode into kaon and antineutrino, surpassing current experimental limits by about one order of magnitude. Recent studies have demonstrated that a reconstruction of momentum and energy of GeV particles is well feasible in liquid scintillator. Monte Carlo studies on the reconstruction of the complex event topologies found for neutrino interactions at multi-GeV energies have shown promising results. If this is confirmed, LENA might serve as far detector in a long-baseline neutrino oscillation experiment currently investigated in LAGUNA-LBNO.3

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Section: Searching Neutrinos From Mev Dmmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The next-generation liquid-scintillator neutrino observatory LENA

Wurm

Beacom

Bezrukov

et al. 2012

Astroparticle Physics

Self Cite

212

200

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“…[32]) can differ considerably in the inner part of the galaxy. However, this has only a relatively mild effect on the neutrino flux if a large field of view is considered [27]. Assuming DM annihilates into neutrino-antineutrino pairs, we can compute the neutrino flux coming from these annihilations in the halo (see, e.g.…”

Section: Neutrino Fluxes From Dark Matter Self-annihilationsmentioning

confidence: 99%

“…The same approach, but for higher masses, was followed in Refs. [26,27]. We evaluate the expected signal from DM annihilations in the entire Milky Way in large neutrino detectors with low energy threshold, such as the existing Super-Kamiokande (SK) and the proposed liquid scintillator detector LENA [28].…”

Section: Introductionmentioning

confidence: 99%

Testing MeV dark matter with neutrino detectors

2008

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MeV particles have been advocated as Dark Matter (DM) candidates in different contexts. This hypothesis can be tested indirectly by searching for the Standard Model (SM) products of DM self-annihilations. As the signal from DM self-annihilations depends on the square of the DM density, we might expect a sizable flux of annihilation products from our galaxy. Neutrinos are the least detectable particles in the SM and a null signal in this channel would allow to set the most conservative bound on the total annihilation cross section. Here, we show that neutrino detectors with good energy resolution and low energy thresholds can not only set bounds on the annihilation cross section but actually test the hypothesis of the possible existence of MeV DM, i.e. test the values of the cross section required to explain the observed DM density. At present, the data in the (positron) energy interval MeV of the Super-Kamiokande experiment is already able to put a very stringent bound on the annihilation cross section for masses between ∼15-130 MeV. Future large experiments, like megaton water-Čerenkov or large scintillator detectors, will improve the present limits and, if MeV DM exists, would be able to detect it.PACS numbers: 14.60. St, 95.35.+d, 95.55.Vj

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“…While neutrinos from WIMP annihilations in the halo of our galaxy have been studied previously [40], there are new implications for this detection channel in light of the high annihilation or decay rate and preference for leptonic modes required to explain the PAMELA and other anomalous cosmic ray signals. Furthermore, decays or annihilations directly into e þ e À final states are disfavored by the observed spectra, requiring instead muon or tau final states.…”

Section: Introductionmentioning

confidence: 99%

High-energy neutrino signatures of dark matter

et al. 2010

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It has been suggested that the excesses of high-energy cosmic ray electrons and positrons seen by PAMELA and the Fermi Gamma Ray Space Telescope are evidence of dark matter annihilation or decay in the Galactic halo. To accommodate these signals however, the final states must be predominantly muons or taus. These leptonic final states will produce neutrinos, which are potentially detectable with the IceCube neutrino observatory. We find that with five years of data, IceCube (supplemented by DeepCore) can significantly constrain the relevant parameter space for both annihilating or decaying dark matter, and may be capable of discovering leptophilic dark matter in the halo of the Milky Way.

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Neutrino constraints on the dark matter total annihilation cross section

Cited by 162 publications

References 70 publications

The next-generation liquid-scintillator neutrino observatory LENA

The next-generation liquid-scintillator neutrino observatory LENA

Testing MeV dark matter with neutrino detectors

High-energy neutrino signatures of dark matter

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