Abstract
The CRESST experiment uses cryogenic detectors based on transition-edge sensors to search for dark matter interactions. Each detector module consists of a scintillating CaWO_4 crystal and a silicon-on-sapphire (SOS) light detector which operate in coincidence (phonon-light technique). The 40-mm-diameter SOS disks (2 g mass) used in the data taking campaign of CRESST-II Phase 2 (2014–2016) reached absolute baseline resolutions of sigma = 4–7 eV. This is the best performance reported for cryogenic light detectors of this size. Newly developed silicon beaker light detectors (4 cm height, 4 cm diameter, 6 g mass), which cover a large fraction of the target crystal surface, have achieved a baseline resolution of sigma = 5.8,eV. First results of further improved light detectors developed for the ongoing low-threshold CRESST-III experiment are presented.
Highlights
J Low Temp Phys (2018) 193:1160–1166 mass) used in the data taking campaign of cryogenic rare event search with superconducting thermometers (CRESST)-II Phase 2 (2014–2016) reached absolute baseline resolutions of σ = 4–7 eV
The cryogenic rare event search with superconducting thermometers (CRESST) experiment ([1,2] and references therein) uses tungsten thin-film TES for a highsensitivity measurement of phonons created in particle interactions in a CaWO4 target crystal at milli-Kelvin temperatures, and an SOS disk as a separate cryogenic detector to measure the scintillation light emitted from the target
The energy scale of the light channel established can be converted to a baseline resolution of the light channel using empty baseline samples. This indirect measure of light detector resolution is most relevant for dark matter search, as it directly relates to the energy range for which particle identification is possible
Summary
J Low Temp Phys (2018) 193:1160–1166 mass) used in the data taking campaign of CRESST-II Phase 2 (2014–2016) reached absolute baseline resolutions of σ = 4–7 eV This is the best performance reported for cryogenic light detectors of this size. As the fraction of the deposited energy emitted in scintillation light depends on the ionization density of the recoiling particle, this technique allows for event-byevent particle identification. This is a decisive advantage in dark matter searches, since radiogenic backgrounds typically result in electron-recoil events, whereas the searched-for dark matter signal is expected to produce nuclear recoils. The more massive recoiling nuclei cause a further reduced scintillation output with light yields of 11% (O), 6% (Ca), 2% (W) relative to electron-recoil events [3]
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