Astrophysical uncertainties of dark matter direct detection experiments
By C. McCabe. 2010
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The effects of astrophysical uncertainties on the exclusion limits at dark matter direct detection experiments are investigated for three scenarios: elastic, momentum dependent, and inelastically scattering dark matter. We find that varying the dark matter galactic escape velocity and the Sun's circular velocity can lead to significant variations in the exclusion limits for light (≲ 10 GeV) elastic and inelastic scattering dark matter. We also calculate the limits using 100 velocity distributions extracted from the Via Lactea II and GHALO N-body simulations and find that a Maxwell-Boltzmann distribution with the same astrophysical parameters generally sets less constraining limits. The elastic and momentum dependent limits remain robust for masses ≳ 50 GeV under variations of the astrophysical parameters and the form of the velocity distribution.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/d7c1243a7a75fdabfb1748cc2a3803dd90041f41
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Citations in the corpus
- WIMP dark matter candidates and searches—current status and future prospects (2017, background): “1] and references therein). The dependence on the velocity distribution is typically weak [212], but can become more important, e.g., if the detector is sensitive only to the tail of the distribution [213]. Alternatively, the limits can be shown in a DM halo-independent way [214] (see also [215] and”
- Colloquium: Annual modulation of dark matter (2013, background): “(14) or (17), the mean inverse speed has an analytical form, presented in Appendix B and in Savage, Freese, and Gondolo (2006) and McCabe (2010).”
- Beyond effective field theory for dark matter searches at the LHC (2013, background): “These crosssections should be accurate within a factor of two or three (similar to the uncertainty from the local dark matter density [59]).”
- The Bar and Spiral Structure Legacy (BeSSeL) Survey: Mapping the Milky Way with VLBI Astrometry† (2011, background): “Corresponding author: e-mail: brunthal@mpifr-bonn.mpg.de ground (e.g. Loeb & Narayan 2008), and even on the interpretation of dark matter direct detection experiments (Foot 2010; McCabe 2010).”
- Characterising dark matter searches at colliders and direct detection experiments: vector mediators (2014, unknown): “nucleon scattering cross-section limit [89, 90].”
- Dark matter direct-detection experiments (2015, methodology): “val are robust against the uncertainties of astrophysical parameters. This parameter space has been used in the last couple of years to display results of direct detection experiments (see as examples[232][233][234][235]). 6. Detector calibration Results from dark matter detectors contain typically ”
- A taste of dark matter: flavour constraints on pseudoscalar mediators (2014, unknown): “on form factors FN;N 0 00 from [128], the Earth’s velocity from [129,130], assume the Standard Halo Model and use v 0 = 230 km=s, v esc = 550 km=s and ˆ = 0:3 GeV/cm3 for the astrophysical parameters [131]. 10The SIMPLE [122], PICASSO [123] and COUPP [124] experiments also give similar constraints. ”
- Search for dark matter with a 231-day exposure of liquid argon using DEAP-3600 at SNOLAB (2019, methodology): “5 × 10−44 cm(2)) for WIMPs with a mass of 100 GeV=c(2) ð1 TeV=c2Þ, assuming the standard halo dark matter model described in [49], with a Maxwell-Boltzmann velocity distribution below an escape velocity of 544 km=s and v0 1⁄4 220 km=s, and a local density of 0.”