Dark matter spin-dependent limits for WIMP interactions on 19F by PICASSO

Archambault, S.; Aubin, F.; Auger, M.; Behnke, E.; Beltrán, B.; Clark, K.; Dai, Xiongxin; Davour, Anna; Farine, J.; Faust, Rachel; Genest, M. H.; Giroux, G.; Gornea, R.; Krauss, C. B.; Kumaratunga, S.; Lawson, I.; Leroy, C.; Lessard, L.; Lévy, C.; Levine, I.; MacDonald, R.; Martin, J. P.; Nadeau, P.; Noble, A. J.; Piro, M.‐C.; Pospı́šil, S.; Shepherd, T.; Starinski, N.; Štekl, I.; Storey, Caroline; Wichoski, U.; Zacek, V.

doi:10.1016/j.physletb.2009.11.019

Cited by 143 publications

(153 citation statements)

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“…Together with the Fermi line search data, we have shown the best limits from direct detection experiments [50] and the Tevatron limits [19]. For M6, the Fermi line search is currently the best available limits for the masses to which they apply, with the Tevatron limits comparable and taking over at low WIMP masses.…”

Section: Discussionmentioning

confidence: 77%

“…If the LAT were to observe a gamma ray line signal in the near future, this would (for example) exclude these combinations of WIMP masses and couplings as being responsible. In Figure 3, we show the parameter space for a Dirac WIMP scattering through a spin-dependent interaction along with some of the relevant direct detection experiments [50]. We see that, as was also true for colliders, the line searches are stronger for some operators than near future prospects for spin-dependent scattering.…”

Section: Discussionmentioning

confidence: 82%

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Gamma ray line constraints on effective theories of dark matter

et al. 2011

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A monochromatic gamma ray line results when dark matter particles in the galactic halo annihilate to produce a two body final state which includes a photon. Such a signal is very distinctive from astrophysical backgrounds, and thus represents an incisive probe of theories of dark matter.We compare the recent null results of searches for gamma ray lines in the galactic center and other regions of the sky with the predictions of effective theories describing the interactions of dark matter particles with the Standard Model. We find that the null results of these searches provide constraints on the nature of dark matter interactions with ordinary matter which are complementary to constraints from other observables, and stronger than collider constraints in some cases.

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Section: Discussionmentioning

confidence: 77%

Section: Discussionmentioning

confidence: 82%

Gamma ray line constraints on effective theories of dark matter

et al. 2011

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“…We estimate the prospects for Super-K, finding sensitivity to σ SD χP in a range competitive to that of other, rather different, experiments. Importantly, our results are nearly insensitive to the annihilation final states and the details of the astrophysical inputs (in standard scenarios [27]); non- [28][29][30] and high-energy neutrino searches are shown [31,32], along with the possible DAMA/LIBRA signal region [33,34].…”

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confidence: 99%

New sensitivity to solar WIMP annihilation using low-energy neutrinos

2013

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Dark matter particles captured by the Sun through scattering may annihilate and produce neutrinos, which escape. Current searches are for the few high-energy neutrinos produced in the prompt decays of some final states. We show that interactions in the solar medium lead to a large number of pions for nearly all final states. Positive pions and muons decay at rest, producing low-energy neutrinos with known spectra, includingνe through neutrino mixing. We demonstrate that SuperKamiokande can thereby provide a new probe of the spin-dependent WIMP-proton cross section. Compared to other methods, the sensitivity is competitive and the uncertainties are complementary.PACS numbers: 95.35.+d, 95.85.Ry Introduction.-If dark matter is a thermal relic of the early universe, then its self-annihilation cross section is revealed by its present mass density. To match observations, the required cross section, averaged over relative velocities, is σ A v = (5.2−2.2)×10 −26 cm 3 /s, as a function of increasing mass, m χ [1]. This indicates a weakly interacting massive particle (WIMP; denoted χ) [2][3][4].The total annihilation cross section, including all final states, is well defined, but the partial annihilation, scattering, and production cross sections with any specific standard model (SM) particles are model-dependent. Measurement of any of these cross sections would dramatically constrain WIMP models and eliminate more exotic possibilities. There are limits from straightforward searches for astrophysical fluxes of annihilation products, direct nuclear scatterings in underground experiments, and collider events with missing energy.Searches for high-energy neutrinos from the Sun give strong limits on WIMP-nucleon scattering. WIMPs passing through the Sun may rarely scatter with nuclei and become gravitationally bound. Scattering can occur by coherent spin-independent (SI) or valence spindependent (SD) interactions. Further scatterings thermalize WIMPs in the solar core, where they annihilate. Only neutrinos can escape and potentially be detected. When the capture rate, Γ C , regulates the annihilation rate, Γ A , as expected, an upper limit on the neutrino flux sets an upper limit on the WIMP-nucleon scattering cross section.The most interesting limits using searches for highenergy neutrinos from the Sun are on SD WIMP-proton scattering, σ SD χp . Though the searches are based on the annihilation process, these limits are independent of σ A v , except for assumptions about the annihilation final states, which govern the detectability of the neutrinos. High-energy neutrinos come from the few annihilation products that decay promptly, before losing energy in the solar medium, giving continuum spectra up to E ν ∼ m χ (direct annihilation to neutrino pairs, helicitysuppressed in many models, produces a line at E ν = m χ ). Strong limits on the SD WIMP-proton scattering cross section have been derived for large m χ and certain final states, such as W + W − , τ + τ − , and bb.Generalizing to other final states and a broader range...

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“…Standard tools in particle physics for decades, the bubble chamber has been repurposed for dark matter search by the COUPP [62], PICASSO [63], and SIMPLE [64] experiments. A liquid target is superheated and compressed, and when sufficient energy density is deposited in the target, a bubble is nucleated.…”

Section: Bubble Chambersmentioning

confidence: 99%

Detector Simulation and WIMP Search Analysis for the Cryogenic Dark Matter Search Experiment

McCarthy¹

2013

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Astrophysical and cosmological measurements on the scales of galaxies, galaxy clusters, and the universe indicate that ∼85% of the matter in the universe is composed of dark matter, made up of non-baryonic particles that interact with cross-sections on the weak scale or lower. Hypothetical Weakly Interacting Massive Particles, or WIMPs, represent a potential solution to the dark matter problem, and naturally arise in certain Standard Model extensions.The Cryogenic Dark Matter Search (CDMS) collaboration aims to detect the scattering of WIMP particles from nuclei in terrestrial detectors. Germanium and silicon particle detectors are deployed in the Soudan Underground Laboratory in Minnesota. These detectors are instrumented with phonon and ionization sensors, which allows for discrimination against electromagnetic backgrounds, which strike the detector at rates orders of magnitude higher than the expected WIMP signal.This dissertation presents the development of numerical models of the physics of the CDMS detectors, implemented in a computational package collectively known as the CDMS Detector Monte Carlo (DMC). After substantial validation of the models against data, the DMC is used to investigate potential backgrounds to the next iteration of the CDMS experiment, known as SuperCDMS. Finally, an investigation of using the DMC in a reverse Monte Carlo analysis of WIMP search data is presented.140.23 kg-days of WIMP search data from the silicon detectors in the CDMSII experiment is also analyzed. The resulting upper limits on the WIMP-nucleon crosssection are higher than those published by other experiments at all WIMP masses, and the lowest limit on the WIMP-nucleon cross-section is 1.07*10 −42 cm 2 at a mass 3 of 60 GeV/c 2 . These results do provide new and interesting constraints at WIMP masses ≤40 GeV/c 2 and cross sections from 10 −42 -10 −39 cm 2 , a region in which some WIMP search experiments have claimed evidence for a WIMP signal, which other experiments claim to have ruled out.

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Dark matter spin-dependent limits for WIMP interactions on 19F by PICASSO

Cited by 143 publications

References 29 publications

Gamma ray line constraints on effective theories of dark matter

Gamma ray line constraints on effective theories of dark matter

New sensitivity to solar WIMP annihilation using low-energy neutrinos

Detector Simulation and WIMP Search Analysis for the Cryogenic Dark Matter Search Experiment

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