The DRIFT Directional Dark Matter Experiments

Daw, E. J.; Dorofeev, A.; Fox, J.; Gauvreau, J.-L.; Ghag, C.; Harmon, L. J.; Harton, J. L.; Gold, M.; Lee, E.R.; Loomba, D.; Miller, E. H.; Murphy, A. St. J.; Paling, S. M.; Landers, J. M.; Phan, N.; Pipe, M.; Pushkin, K.; Robinson, M.; Sadler, S. W.; Snowden‐Ifft, D.; Spooner, N. J. C.; Walker, D.; Warner, D.

doi:10.1051/eas/1253002

Cited by 28 publications

(27 citation statements)

References 10 publications

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“…Gaseous time projection chambers (such as DRIFT [64], DMTPC [65], D 3 [66], MIMAC [67] and NEWAGE [68]) using hydrocarbon targets may be well-suited for this type of search.…”

Section: Discussionmentioning

confidence: 99%

Tools for studying low-mass dark matter at neutrino detectors

et al. 2012

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We determine the neutrino spectra arising from low-mass (4 − 10 GeV) dark matter annihilating in the sun. We also determine the low-mass dark matter capture rates (element by element in the sun), assuming dark matter interacts either through elastic contact interactions, elastic long-range interactions, or inelastic contact interactions. These are the non-detector-specific data needed for determining the sensitivity of a neutrino detector to dark matter annihilating in the sun. As an application, we estimate the sensitivity of a one kiloton liquid scintillation neutrino detector (such as KamLAND) and LBNE (LAr-based) to low-mass dark matter with long-range interactions and compare this to the expected CDMS sensitivity. It is found that KamLAND's sensitivity can exceed that obtainable from the current CDMS data set by up to two orders of magnitude.

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“…Gaseous time projection chambers (such as DRIFT [64], DMTPC [65], D 3 [66], MIMAC [67] and NEWAGE [68]) using hydrocarbon targets may be well-suited for this type of search.…”

Section: Discussionmentioning

confidence: 99%

Tools for studying low-mass dark matter at neutrino detectors

et al. 2012

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“…We focus on the latter technique here since low-pressure gas time projection chambers (TPCs) have seen many more years of consistent progress in their experimental realisation, see e.g., Refs. [186][187][188][189][190][191][192][193][194]). Most recently the design for a tonne-scale network of directional gas-TPCs named Cygnus [195] has been put for-ward.…”

Section: B Directional Signalsmentioning

confidence: 99%

Velocity substructure from Gaia and direct searches for dark matter

et al. 2020

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Data from the Gaia satellite show that the solar neighbourhood of the Milky Way's stellar halo is imprinted with substructure from several accretion events. Evidence of these events is found in "the Shards", stars clustering with high significance in both action space and metallicity. Stars in the Shards share a common origin, likely as ancient satellite galaxies of the Milky Way, so will be embedded in dark matter (DM) counterparts. These "Dark Shards" contain two substantial streams (S1 and S2), as well as several retrograde, prograde and lower energy objects. The retrograde stream S1 has a very high Earth-frame speed of ∼ 550 km s −1 while S2 moves on a prograde, but highly polar orbit and enhances peak of the speed distribution at around 300 km s −1 . The presence of the Dark Shards locally leads to modifications of many to the fundamental properties of experimental DM signals. The S2 stream in particular gives rise to an array of effects in searches for axions and in the time dependence of nuclear recoils: shifting the peak day, inducing non-sinusoidal distortions, and increasing the importance of the gravitational focusing of DM by the Sun. Dark Shards additionally bring new features for directional signals, while also enhancing the DM flux towards Cygnus.

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“…The three-dimensional reconstruction of the recoil track then allows the full energy and direction dependence of the WIMP recoil spectrum to be measured and, in principle, the WIMP velocity distribution can be inferred [16]. The detectors currently in the prototype phase include DMTPC [17], DRIFT [18], MIMAC [19], and NEWAGE [20]. Directional detection offers several theoretical advantages over its nondirectional counterpart.…”

Section: Introductionmentioning

confidence: 99%

Directional detection of dark matter streams

O’Hare

Green

2014

Phys. Rev. D

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Directional detection of WIMPs, in which the energies and directions of the recoiling nuclei are measured, currently presents the only prospect for probing the local velocity distribution of Galactic dark matter. We investigate the extent to which future directional detectors would be capable of probing dark matter substructure in the form of streams. We analyse the signal expected from a Sagittarius-like stream and also explore the full parameter space of stream speed, direction, dispersion and density. Using a combination of non-parametric directional statistics, a profile likelihood ratio test and Bayesian parameter inference we find that within acceptable exposure times (O(10) kg yr for cross sections just below the current exclusion limits) future directional detectors will be sensitive to a wide range of stream velocities and densities. We also examine and discuss the importance of the energy window of the detector.Comment: 18 pages, 12 figures, 1st revision, submitted to Phys. Rev.

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The DRIFT Directional Dark Matter Experiments

Cited by 28 publications

References 10 publications

Tools for studying low-mass dark matter at neutrino detectors

Tools for studying low-mass dark matter at neutrino detectors

Velocity substructure from Gaia and direct searches for dark matter

Directional detection of dark matter streams

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