Search for dark matter with a 231-day exposure of liquid argon using DEAP-3600 at SNOLAB

Ajaj, Rahaf; Amaudruz, P.; Araujo, G. R.; Baldwin, Martin; Batygov, M.; Beltrán, B.; Bina, C. E.; Bonatt, J.; Boulay, M. G.; Broerman, B.; Bueno, J. F.; Burghardt, P. M.; Butcher, A.; Cai, B.; Cavuoti, S.; Chen, M.; Chen, Y.; Cleveland, B. T.; Cranshaw, D. J.; Dering, K.; DiGioseffo, J.; Doria, L.; Duncan, F. A.; Dunford, M.; Erlandson, A.; Fatemighomi, N.; Fiorillo, G.; Schepers, Florian; Flower, A.; Ford, R.; Gagnon, R.; Gallacher, D.; Garcés, E. A.; Garg, Sakshi; Giampa, P.; Goeldi, D.; Golovko, V. V.; Gorel, P.; Graham, K.; Grant, D.; Hallin, A. L.; Hamstra, M.; Harvey, P. J.; Hearns, C.; Joy, A.; Jillings, C.; Kamaev, O.; Kaur, G.; Kemp, A.; Kochanek, I.; Kuźniak, M.; Langrock, S.; Zia, F. La; Lehnert, B.; Li, X.; Lidgard, J.; Lindner, T.; Litvinov, O.; Lock, James A.; Longo, Giuseppe; Majewski, P.; McDonald, A. B.; McElroy, Thomas; McGinn, T.; McLaughlin, J.; Mehdiyev, R.; Mielnichuk, C.; Monroe, J.; Nadeau, P.; Nantais, C.; Ng, C.; Noble, A. J.; O’Dwyer, E.; Ouellet, C.; Pasuthip, P.; Peeters, S. J. M.; Piro, M.‐C.; Pollmann, T. R.; Rand, E. T.; Rethmeier, C.; Retière, F.; Seeburn, N.; Singhrao, Kamal; Skensved, P.; Smith, B. C.; Smith, N. J. T.; Sonley, T. J.; Soukup, J.; Stainforth, R.; Stone, Connor; Strickland, V.; Sur, B.; Tang, J.; Vázquez‐Jáuregui, E.; Veloce, L. M.; Viel, S.; Walding, J.; Waqar, Moaz; Ward, M.; Westerdale, S.; Willis, J. L.; Zuñiga-Reyes, A.

doi:10.1103/physrevd.100.022004

Cited by 159 publications

(198 citation statements)

References 46 publications

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“…To begin with, let us illustrate the latest results from DEAP-3600 and how they compare against other experiments under the standard assumption, f n /f p = 1 -see figure 3. This figure is quite similar to that shown by the DEAP collaboration in their recent publication [13]. It displays the current limits on the dark matter-nucleon spin-independent cross section from different experiments: DS-50 (dotted line), DEAP-3600 (solid line), LUX (short-dashed line), PandaX-II (dash-dotted line) and XENON1T (dashed line).…”

Section: Resultssupporting

confidence: 81%

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New constraints on xenonphobic dark matter from DEAP-3600

Yaguna

2019

J. Cosmol. Astropart. Phys.

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The first-year results from DEAP-3600, a single-phase liquid argon direct-detection dark matter experiment, were recently reported. At first sight, they seem to provide no new constraints, as the limit lies well within the region already excluded by three different xenon experiments: LUX, PandaX-II, and XENON1T. We point out, however, that this conclusion is not necessarily true, for it is based on the untested assumption that the dark matter particle couples equally to protons and neutrons. For the more general case of isosping-violating dark matter, we find that there are regions in the parameter space where DEAP-3600 actually provides the most stringent limits on the dark matter-proton spin-independent cross section. Such regions correspond to the so-called Xenonphobic dark matter scenario, for which the neutron-to-proton coupling ratio is close to −0.7. Our results seem to signal the beginning of a new era in which the complementarity among different direct detection targets will play a crucial role in the determination of the fundamental properties of the dark matter particle.

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Section: Resultssupporting

confidence: 81%

“…Recently, the DEAP collaboration reported the results of a dark matter search, based on 231-live days of data taken during the first year of operation, with the DEAP-3600 experiment [13]. DEAP-3600 is a direct-detection dark matter experiment that uses 3279 kg of liquid argon as target and is located 2km underground at SNOLAB.…”

Section: Introductionmentioning

confidence: 99%

New constraints on xenonphobic dark matter from DEAP-3600

Yaguna

2019

J. Cosmol. Astropart. Phys.

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“…3. Further, the densest part of the outer crust is 1 − 2 orders of magnitude less dense than the inner crust on average, while of comparable thickness; therefore its optical depth (and hence cross section sensitivity in Figure 4 directly compares our net crust sensitivity to constraints from underground experiments searching for dark matter in nuclear recoils, for both spin-independent and spin-dependent scattering [85][86][87][88][89]. We also show the xenon neutrino floor, which denotes the cross section sensitivity below which irreducible neutrino backgrounds are expected to confound direct detection searches.…”

Section: E Results and Discussionmentioning

confidence: 89%

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Acevedo

Bramante

Leane

et al. 2020

J. Cosmol. Astropart. Phys.

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Neutron stars serve as excellent next-generation thermal detectors of dark matter, heated by the scattering and annihilation of dark matter accelerated to relativistic speeds in their deep gravitational wells. However, the dynamics of neutron star cores are uncertain, making it difficult at present to unequivocally compute dark matter scattering in this region. On the other hand, the physics of an outer layer of the neutron star, the crust, is more robustly understood. We show that dark matter scattering solely with the low-density crust still kinetically heats neutron stars to infrared temperatures detectable by forthcoming telescopes. We find that for both spin-independent and spin-dependent scattering on nucleons, the crust-only cross section sensitivity is 10 −43 − 10 −41 cm 2 for dark matter masses of 100 MeV − 1 PeV, with the best sensitivity arising from dark matter scattering with a crust constituent called nuclear pasta (including gnocchi, spaghetti, and lasagna phases). For dark matter masses from 10 eV to 1 MeV, the sensitivity is 10 −39 − 10 −34 cm 2 , arising from exciting collective phonon modes in a neutron superfluid in the inner crust. Furthermore, for any s-wave or p-wave annihilating dark matter, we show that dark matter will efficiently annihilate by thermalizing just with the neutron star crust, regardless of whether the dark matter ever scatters with the neutron star core. This implies efficient annihilation in neutron stars for any electroweakly interacting dark matter with inelastic mass splittings of up to 200 MeV, including Higgsinos. We conclude that neutron star crusts play a key role in dark matter scattering and annihilation in neutron stars. *

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“…Many underground experiments have searched for DM that scatters with nucleons through either predominantly spin-dependent or spin-independent interactions, including DEAP [2], PICO [3,4], LUX [5], PandaX [6], and XENON1T [7]. These experiments place detectors deep underground to reduce backgrounds and gain in sensitivity to weakly interacting DM.…”

Section: Introductionmentioning

confidence: 99%

Terrestrial and martian heat flow limits on dark matter

et al. 2020

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If dark matter is efficiently captured by a planet, energy released in its annihilation can exceed that planet's total heat output. Building on prior work, we treat Earth's composition and dark matter capture in detail and present improved limits on dark matter-nucleon scattering cross sections for dark matter masses ranging from 0.1 to 10 10 GeV. We also extend Earth limits by applying the same treatment to Mars. The scope of dark matter models considered is expanded to include spin-dependent nuclear interactions including isospin-independent, proton only, and neutron only interactions. We find that Earth and Mars heating bounds are alleviated for dark matter s-wave self-annihilation cross sections 10 −37 cm 2 .

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Search for dark matter with a 231-day exposure of liquid argon using DEAP-3600 at SNOLAB

Cited by 159 publications

References 46 publications

New constraints on xenonphobic dark matter from DEAP-3600

New constraints on xenonphobic dark matter from DEAP-3600

Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Terrestrial and martian heat flow limits on dark matter

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