Results of a Search for Sub-GeV Dark Matter Using 2013 LUX Data

Akerib, D. S.; Alsum, S.; Araújo, H. M.; Bai, X.; Balajthy, J.; Beltrame, P.; Bernard, E. P.; Bernstein, Adam; Biesiadzinski, T. P.; Boulton, E. M.; Boxer, B.; Brás, P.; Burdin, S.; Byram, D.; Carmona-Benitez, M. C.; Chan, C.; Cutter, J. E.; Davison, T. J. R.; Druszkiewicz, E.; Fallon, S. R.; Fan, A.; Fiorucci, S.; Gaitskell, R. J.; Genovesi, J.; Ghag, C.; Gilchriese, M.; Gwilliam, C. B.; Hall, C.; Haselschwardt, S. J.; Hertel, S. A.; Hogan, D. P.; Horn, M.; Huang, Di; Ignarra, C. M.; Jacobsen, R. G.; Jahangir, O.; Ji, W.; Kamdin, K.; Kazkaz, K.; Khaitan, D.; Knoche, R.; Korolkova, E. V.; Kravitz, S.; Kudryavtsev, V. A.; Lenardo, B. G.; Lesko, K. T.; Liao, J.; Lin, J.; Lindote, A.; Lopes, I.; Manalaysay, A.; Mannino, R. L.; Marangou, N.; Marzioni, M. F.; McKinsey, D. N.; Mei, Dongming; Moongweluwan, M.; Morad, J. A.; Murphy, A. St. J.; Naylor, Andrew; Nehrkorn, C.; Nelson, H. N.; Neves, F.; Oliver-Mallory, K. C.; Palladino, K. J.; Pease, E. K.; Riffard, Q.; Rischbieter, G. R. C.; Rhyne, C.; Rossiter, P.; Shaw, S.; Shutt, T.; Silva, C.; Solmaz, M.; Solovov, V.; Sørensen, P.; Sumner, T. J.; Szydagis, M.; Taylor, D. J.; Taylor, WC; Tennyson, B. P.; Terman, P. A.; Tiedt, D. R.; To, W. H.; Tripathi, M.; Tvrznikova, L.; Utku, U.; Uvarov, S.; Velan, V.; Webb, R.; White, J. T.; Whitis, T. J.; Witherell, M. S.; Wolfs, F. L. H.; Woodward, David I.; Xu, J.; Yazdani, K.; Zhang, C.

doi:10.1103/physrevlett.122.131301

Cited by 168 publications

(139 citation statements)

References 34 publications

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“…The numerical solutions to Eqs. (2) show that by a scale factor of 3a RH , enough of the scalar has decayed away that it is a negligible source of radiation and the radiation energy density begins to evolve as in the usual radiation-dominated era from a temperature T (3a RH ) ≃ 0.34T RH onward. Expressed in terms of the variable µ, the physical free-streaming length calculated from the contribution from both the radiation-and matter-dominated eras is λ phys fs,0 = 4.66 × 10 5 Mpc µ   ln 2…”

Section: A Free-streaming Lengthmentioning

confidence: 92%

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Constraining nonthermal dark matter’s impact on the matter power spectrum

2019

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The inclusion of a period of (effective) matter domination following inflation and prior to the onset of radiation domination has interesting and observable consequences for structure growth. During this early matter-dominated era (EMDE), the Universe was dominated by massive particles, or an oscillating scalar field, that decayed into Standard Model particles, thus reheating the Universe. This decay process could also be the primary source of dark matter. In the absence of fine-tuning between the masses of the parent and daughter particles, both dark matter particles and Standard Model particles would be produced with relativistic velocities. We investigate the effects of the nonthermal production of dark matter particles with relativistic velocities on the matter power spectrum by determining the resulting velocity distribution function for the dark matter. We find that the vast majority of dark matter particles produced during the EMDE are still relativistic at reheating, so their free streaming erases the perturbations that grow during the EMDE. The free streaming of the dark matter particles can also prevent the formation of satellite galaxies around the Milky Way and the structures observed in the Lyman-α forest. For a given reheat temperature, these observations put an upper limit on the velocity of the dark matter particles at their creation. For example, for a reheat temperature of 10 MeV, dark matter must be produced with a Lorentz factor γ 550.

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Section: A Free-streaming Lengthmentioning

confidence: 92%

“…The required annihilation cross-section is "miraculously" of the electroweak scale [1]. However, as we continually place more stringent bounds on dark matter properties, while failing to receive signals from any direct [2][3][4] or indirect [5][6][7][8][9][10] searches, interest in alternatives to this commonly considered scenario grows.…”

Section: Introductionmentioning

confidence: 99%

Constraining nonthermal dark matter’s impact on the matter power spectrum

2019

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“…Detailed discussions for other experimental results obtained so far are given in Refs. [28][29][30][31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47].…”

Section: Limit On the Cross Section Between A Wimp And A Nucleonmentioning

confidence: 99%

Dark matter signals on a laser interferometer

et al. 2020

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WIMPs are promising dark matter candidates. A WIMP occasionally collides with a mirror equipped with interferometric gravitational wave detectors such as LIGO, Virgo, KAGRA and Einstein Telescope (ET). When WIMPs collide with a mirror of an interferometer, we expect that characteristic motions of the pendulum and mirror are excited, and those signals could be extracted by highly sophisticated sensors developed for gravitational wave detection. We analyze the motions of the pendulum and mirror, and estimate the detectability of these motions. For the "Thin-ET" detector, the signal to noise ratio may be 1.7 m DM 100 GeV , where mDM is the mass of a WIMP. We may set a more strict upper limit on the cross section between a WIMP and a nucleon than the limits obtained by other experiments so far when mDM is approximately lower than 0.2 GeV. We find an order of magnitude improvement in the upper limit around mDM = 0.2 GeV.

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“…More recently, there is growing interest in considering particle physics realizations of SIDM with multiple states. For example, to avoid strong bounds from direct detection experiments [24][25][26][27], Refs. [28,29] propose an inelastic SIDM model, where there are two dark states and they differ by a small mass splitting [30,31].…”

Section: Introductionmentioning

confidence: 99%

Astrophysical probes of inelastic dark matter with a light mediator

Álvarez

2020

Phys. Rev. D

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We consider an inelastic dark matter model, where a fermion is charged under a broken U(1) gauge symmetry, and introduce a tiny Majorana mass term to split the fermion into two states with the light one being a dark matter candidate. If the gauge boson is light, it can mediate both elastic and inelastic dark matter self-interactions in dark halos, leading to observational consequences. Using a numerical technique based on partial wave analysis, we accurately calculate the elastic and inelastic self-scattering cross sections. We assume a thermal freeze-out scenario and fix the gauge coupling constant using the relic density constraint. Then, we focus on six benchmark masses of dark matter, covering a wide range from 10 MeV to 160 GeV and map parameter regions where the elastic scattering cross section per unit mass is within 1 cm 2 /g-5 cm 2 /g, favored to solve small-scale issues of cold dark matter. If the heavy state can decay to the light state and a massless species, the inelastic up-scattering process can cool the halo and lead to core collapse. Taking galaxies with evidence of dark matter density cores, we further derive constraints on the parameter space. For dark matter masses below 10 GeV, the mass splitting must be large enough to forbid up scattering in the dwarf halo for evading the core-collapse constraint; while for higher masses, the up-scattering process can still be allowed. Our results show astrophysical observations can provide powerful tests for dark matter models with large elastic and inelastic self-interactions.

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Results of a Search for Sub-GeV Dark Matter Using 2013 LUX Data

Cited by 168 publications

References 34 publications

Constraining nonthermal dark matter’s impact on the matter power spectrum

Constraining nonthermal dark matter’s impact on the matter power spectrum

Dark matter signals on a laser interferometer

Astrophysical probes of inelastic dark matter with a light mediator

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