Dark matter results from 225 live days of XENON100 data.

By E. Aprile, M. Alfonsi, K. Arisaka, F. Arneodo, C. Balan, L. Baudis, B. Bauermeister, A. Behrens, P. Beltrame, K. Bokeloh and 66 more. Physical Review Letters, 2012

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We report on a search for particle dark matter with the XENON100 experiment, operated at the Laboratori Nazionali del Gran Sasso for 13 months during 2011 and 2012. XENON100 features an ultralow electromagnetic background of (5.3 ± 0.6) × 10(-3) events/(keV(ee) × kg × day) in the energy region of interest. A blind analysis of 224.6 live days × 34 kg exposure has yielded no evidence for dark matter interactions. The two candidate events observed in the predefined nuclear recoil energy range of 6.6-30.5 keV(nr) are consistent with the background expectation of (1.0 ± 0.2) events. A profile likelihood analysis using a 6.6-43.3 keV(nr) energy range sets the most stringent limit on the spin-independent elastic weakly interacting massive particle-nucleon scattering cross section for weakly interacting massive particle masses above 8 GeV/c(2), with a minimum of 2 × 10(-45) cm(2) at 55 GeV/c(2) and 90% confidence level.

Subfields: Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a8cd9dff47648a13f0d9297c306f2189f577ca4b

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Citations in the corpus

Lectures on Dark Matter Physics (2016, methodology): “If the DM scatters off a nucleus with mass mN , then the nuclear recoil energy is ER = q2 2mN ' 50 keV ( mχ 100 GeV )2 (100 GeV mN ) , (3.1) 18 where q ∼ mχv is the momentum transfer in the collision and v ∼ 10−3 is the (non-relativistic) speed of the incoming DM.7 Let us take as an example the LUX ”
Galaxy UV-luminosity function and reionization constraints on axion dark matter (2014, background): “…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; Abbasi c© 0000 RAS ar X iv…”
DARWIN: towards the ultimate dark matter detector (2016, background): “The XENON100 experiment [23, 24], a TPC with a 62 kg active target, has reached its sensitivity goal and excluded spin-independent WIMP-nucleon cross sections above 2× 10 cm(2) at a WIMP mass of 55GeV/c(2) [25].”
Liquid noble gas detectors for low energy particle physics (2012, methodology): “d liquid argon experiments (red); in order of publication: DAMA/LXe [375], ZEPLIN-I [44], ZEPLIN-II [49], WARP 2.3-l [55], XENON10 [377, 126] (low energy analysis [210]), ZEPLIN-III [56] and XENON100 [215]. The parameter space favored by Constrained MSSM after 1 fb 1 of LHC data is shown in green [4”