Results on low mass WIMPs using an upgraded CRESST-II detector
By G. Angloher, A. Bento, C. Bucci, L. Canonica, A. Erb, F. Feilitzsch, N. Iachellini, P. Gorla, A. Gütlein, D. Hauff and 34 more. The European Physical Journal C, 2014
221 citations recorded by the source corpus.
The CRESST-II cryogenic dark matter search aims for the detection of WIMPs via elastic scattering off nuclei in CaWO4\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$_4$$\end{document} crystals. We present results from a low-threshold analysis of a single upgraded detector module. This module efficiently vetoes low energy backgrounds induced by α\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\alpha $$\end{document}-decays on inner surfaces of the detector. With an exposure of 29.35 kg live days collected in 2013 we set a limit on spin-independent WIMP-nucleon scattering which probes a new region of parameter space for WIMP masses below 3 GeV/c2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$^2$$\end{document}, previously not covered in direct detection searches. A possible excess over background discussed for the previous CRESST-II phase 1 (from 2009 to 2011) is not confirmed.
Subfields: Artificial Intelligence, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/545efd7dbbc0bfde5aa3f262178514d18e61b76b
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Citations in the corpus
- Dark matter direct-detection experiments (2015, methodology): “egion was observed[187]. With the same detector technology and exposure a dedicated low mass analysis was performed excluding WIMP interactions for a mass of 3GeV/c2 at a cross-section of 8 210 40 cm [217]. Using the detector module with the lowest energy threshold of 307eV and an increased exposure”
- History of dark matter (2018, unknown): “…2011a, 2011b), CRESST (Angloher et al., 2012), and CDMS (Agnese et al., 2013) experiments were briefly interpreted as possible dark matter signals, they now appear to be the consequences of poorly understood backgrounds (Angloher et al., 2014; Kelso et al., 2014) and/or statistical fluctuations.”
- WIMP dark matter candidates and searches—current status and future prospects (2017, background): “d in two mass ranges around 10GeV and 25GeV with the signicance at the level of 4:2˙and 4:7˙, respectively. However, as it was pointed out in [195] and conrmed in a later study by the collaboration [196], the excess was mainly due to a missing contribution to the background (see also [92] and [175] ”
- Characterising dark matter searches at colliders and direct detection experiments: vector mediators (2014, unknown): “See also [111–114] and [115–117] for additional non-DM explanations of the CoGeNT, CRESST-II and DAMA/LIBRA excesses.”
- Galaxy UV-luminosity function and reionization constraints on axion dark matter (2014, background): “Many experimental efforts are underway to detect and constrain these DM candidates via their direct (e.g. Aalseth et al. 2011; Agnese et al. 2014; Angloher et al. 2014; Aprile et al. 2012; Akerib et al. 2014; Asztalos et al. 2010; Budker et al. 2014) or indirect (e.g Ackermann et al. 2011;…”