Snowden-Ifft, Freeman, and Price Reply:

Snowden-Ifft, D.P.; Freeman, E.; Price, P. B.

doi:10.1103/physrevlett.76.332

Cited by 48 publications

(101 citation statements)

References 4 publications

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“…Some detectors, however, can be made insensitive to these gammas [15]. So the use of lead as shielding and its thickness is decided for each particular experiment.…”

Section: Neutrons From Rockmentioning

confidence: 99%

Neutron background in large-scale xenon detectors for dark matter searches

CARSON¹

2004

Astroparticle Physics

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Simulations of the neutron background for future large-scale particle dark matter detectors are presented. Neutrons were generated in rock and detector elements via spontaneous fission and (α,n) reactions, and by cosmic-ray muons. The simulation techniques and results are discussed in the context of the expected sensitivity of a generic liquid xenon dark matter detector. Methods of neutron background suppression are investigated. A sensitivity of 10 −9 − 10 −10 pb to WIMP-nucleon interactions can be achieved by a tonne-scale detector.

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“…Some detectors, however, can be made insensitive to these gammas [15]. So the use of lead as shielding and its thickness is decided for each particular experiment.…”

Section: Neutrons From Rockmentioning

confidence: 99%

Neutron background in large-scale xenon detectors for dark matter searches

CARSON¹

2004

Astroparticle Physics

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“…Under the assumption that DRIFT-type detectors can be made insensitive to gammas [2,3,4], all nuclear recoils (even those accompanied by gammas, electrons or muons) are of potential danger to the detector sensitivity. Figure 8 shows the energy spectrum of nuclear recoils originated from muon-induced neutrons in a TPC filled with CS 2 .…”

Section: Muon-induced Neutronsmentioning

confidence: 99%

“…Other backgrounds that have the capability to generate false signals include sources of alphas and gammas. Simulations of these backgrounds, however, have been neglected in this study as any signals generated by alpha particles in the detector can be actively vetoed because they will be produced at the edge of the detector and have long tracks, and those due to gammas can be rejected by adjusting the energy threshold and applying appropriate cuts [2,3,4].…”

Section: Introductionmentioning

confidence: 99%

Simulations of neutron background in a time projection chamber relevant to dark matter searches

Carson

Davies

Daw

et al. 2005

Nuclear Instruments and Methods in Physics Research Section A:

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Presented here are results of simulations of neutron background performed for a time projection chamber acting as a particle dark matter detector in an underground laboratory. The investigated background includes neutrons from rock and detector components, generated via spontaneous fission and (α,n) reactions, as well as those due to cosmic-ray muons. Neutrons were propagated to the sensitive volume of the detector and the nuclear recoil spectra were calculated. Methods of neutron background suppression were also examined and limitations to the sensitivity of a gaseous dark matter detector are discussed. Results indicate that neutrons should not limit sensitivity to WIMP-nucleon interactions down to a level of (1 − 3) × 10 −8 pb in a 10 kg detector.

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“…Recoil tracks produced will preferentially be aligned with this wind vector [3]. A detector on Earth at a latitude ∼45 • , like Boulby, will thus see the WIMP wind vector oscillate over a sidereal day, from pointing south to pointing to the Earth's center, repeating each sidereal day and going rapidly out of phase with the terrestrial day.…”

Section: Drift Concept and Head-tail Experimentsmentioning

confidence: 99%

“…Annual modulation [2] provides one route towards a galactic signature based on the non-terrestrial nature of WIMPs but it is known that a more powerful galactic signal, impossible to mimic by terrestrial backgrounds, could come from a device capable of tracking the direction of WIMP-induced recoil ions, down to low (∼1 keV/amu) energies, event by event [3]. The only method established for observing these powerful but difficult to extract signatures, is to use a low density, large volume, target with sufficient spatial resolution to do the necessary tracking [4].…”

Section: Introductionmentioning

confidence: 99%

Techniques for Head-Tail directional recoil measurements in the DRIFT-II dark matter detector

Spooner¹

2009

Proceedings of Identification of Dark Matter 2008 — PoS(idm2008)

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We introduce the concepts and techniques relevant to determining evidence for the so-called Head-Tail asymmetry from neutron-induced nuclear recoil tracks in the DRIFT-II dark matter detector. The back-to-back dual TPC arrangement in DRIFT makes this detector ideal for Head-Tail tests, allowing systematic errors to be reduced. The detection of Head-Tail asymmetry can open a powerful new means of searching for a galactic signature from WIMPs. Identification of dark matter

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Snowden-Ifft, Freeman, and Price Reply:

Cited by 48 publications

References 4 publications

Neutron background in large-scale xenon detectors for dark matter searches

Neutron background in large-scale xenon detectors for dark matter searches

Simulations of neutron background in a time projection chamber relevant to dark matter searches

Techniques for Head-Tail directional recoil measurements in the DRIFT-II dark matter detector

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