Working Group Report: WIMP Dark Matter Direct Detection

By P. Cushman, T. Empl, R. Schnee, A. Ryd, C. Galbiati, B. Sadoulet, S. Golwala, B. Cabrera, S. Luitz, M. Kelsey and 39 more. 2013

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Cosmological Moduli and the Post-Inflationary Universe: A Critical Review (2015, background): “(8) For m3/2 ∼ 10− 100 TeV, as one would expect in models that at least partially address the electroweak hierarchy problem, we see that mσ falls within the mass range where a non-thermal history results.”
Dark matter direct-detection experiments (2015, methodology): “The SuperCDMS [391] and the EURECA [322] experiments aim to operate few hundreds of kg of target material to cover a significant part of the parameter space at low WIMP masses.”
Di-photon excess illuminates dark matter (2015, background): “ future direct detection experiments should reach a sensitivity of approximately 10 46 cm2 for spin independent cross section assuming a dark matter mass of around 300 GeV (see e.g. XENON1T prospects [48]), which is in the ballpark of the predictions for our benchmark points (see Table 2). In fact, ”
The Simons Observatory: science goals and forecasts (2018, background): “…down to 1 keV (Gluscevic and Boddy 2018; Boddy and Gluscevic 2018; Slatyer and Wu 2018; Xu et al. 2018) – far beyond the reach of current nuclear-recoil based experiments that are optimized to detect weakly interacting massive particles (WIMPs) much heavier than the proton (Cushman et al. 2013).”