Simultaneous measurement of phonons and scintillation light for active background rejection in the CRESST experiment

Bravin, M.; Bruckmayer, M.; Frank, T.; Giordano, Stefano; Loidl, M.; Meier, Oliver; Meunier, P.; Pergolesi, Daniele; Pröbst, F.; Seidel, W.; Sisti, M.; Stéfano, P. Di; Stodolsky, L.; Uchaikin, S.; Zerle, L.

doi:10.1016/s0168-9002(99)01371-6

Cited by 15 publications

(6 citation statements)

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“…Therefore, CPSDs play an important role in experiments searching for rare events, so as interactions with weakly interacting massive particles ͑WIMP͒, possibly constituting the galactic dark matter. 10,11 A clear demonstration of this technique's effectiveness derives from a recent upper limit for the scalar cross section of WIMP-nucleon elastic scattering, obtained in a search for dark matter. 12 A further advantage of the CPSD technique is the possibility of using different target materials, which allows ex-ploiting the material signature for the confirmation of a WIMP signal.…”

Section: Introductionmentioning

confidence: 99%

Thermal properties ofCaMoO4: Lattice dynamics and synchrotron powder diffraction studies

et al. 2006

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The structure of calcium molybdate was studied by means of synchrotron based high-resolution powder diffraction methods in the temperature range 12-300 K. The scheelite structure type was confirmed for CaMoO 4 in the temperature region investigated and no structural anomalies were observed. Thermal expansion coefficients extracted from the thermal dependencies of the cell sizes are found to be in good agreement with the predictions from our lattice dynamics calculations that form the background for microscopic interpretation of the experimental data. From the analyses of experimental results and the calculated thermal expansion coefficients, elastic constants, phonon density of states, heat capacities, entropy, and Grüneisen parameters it is concluded that a quasiharmonic lattice dynamics approach provides a good description of these properties for CaMoO 4 at temperatures below 800 K.

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Section: Introductionmentioning

confidence: 99%

Thermal properties ofCaMoO4: Lattice dynamics and synchrotron powder diffraction studies

et al. 2006

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“…More recently, however, the extreme level of radiopurity and the expertise achieved in low background techniques, as in the case of IGEX [6,7,8], has reduced the raw background to levels where the neutron contribution can be of great importance. These facts, together with the recent development of discrimination techniques to disentangle nuclear recoils produced by particle dark matter interactions from electron recoils generated by the typical gamma or beta background [9,10,11,12] have made the neutrons to remain as the real worrisome background for WIMPs [13,14,15,16]. They can produce nuclear recoils (< 100 keV) in the detector target nuclei which would mimic WIMP interactions.…”

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confidence: 99%

Neutron background at the Canfranc underground laboratory and its contribution to the IGEX-DM dark matter experiment

Carmona

Cebrián

Garcı́a

et al. 2004

Astroparticle Physics

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A quantitative study of the neutron environment in the Canfranc Underground Laboratory has been performed. The analysis is based on a complete set of simulations and, particularly, it is focused on the IGEX-DM dark matter experiment. The simulations are compared to the IGEX-DM low energy data obtained with different shielding conditions. The results of the study allow us to conclude, with respect to the IGEX-DM background, that the main neutron population, coming from radioactivity from the surrounding rock, is practically eliminated after the implementation of a suitable neutron shielding. The remaining neutron background (muon-induced neutrons in the shielding and in the rock) is substantially below the present background level thanks to the muon veto system. In addition, the present analysis gives us a further insight on the effect of neutrons in other current and future experiments at the Canfranc Underground Laboratory. The comparison of simulations with the body of data available has allowed to set the flux of neutrons from radioactivity of the Canfranc rock, (3.82 ± 0.44) × 10 −6 cm −2 s −1 , as well as the flux of muon-induced neutrons in the rock, (1.73 ± 0.22(stat) ± 0.69(syst)) × 10 −9 cm −2 s −1 , or the rate of neutron production by muons in the lead shielding, (4.8 ± 0.6(stat) ± 1.9(syst)) × 10 −9 cm −3 s −1 .Key words: Underground muons, dark matter, muon flux, neutron background PACS: 28.20. Gd, 96.40.Tv, 25.30.Mr, 95.35.+d The search for dark matter is one of the biggest challenges of modern cosmology. Last observational data [1,2,3] are compatible with a flat accelerating * Deceased. Preprint submitted to Elsevier Science 11 April 2018Universe with a matter content of around 30%, where about 25% is dark matter, mostly in the form of non-baryonic cold dark matter. Even though the Standard Model (SM) of particle physics does not offer a proper candidate satisfying all the needed requirements, its supersymetric extensions open a new world of particles. Experiments looking for cold, non-baryonic, weakly interacting, massive neutral particles beyond the SM -generically called WIMPssupposedly forming this missing matter of the Universe are obviously of most relevance for particle physics and cosmology and so the number of such attempts -with a large variety of techniques, detectors and targets-is quite numerous [4].In experiments intended for WIMP direct detection, such as IGEX Dark Matter (IGEX-DM), galactic WIMPs could be detected by means of the nuclear recoil they would produce when scattered off target nuclei of suitable detectors.

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“…The current generation of CRESST detectors use 300 g CaW O 4 crystals as absorbers, instrumented with superconducting W thermometers. The scintillation light is absorbed by a sapphire wafer, instrumented with a superconducting W thermometer, adjacent to the CaW O 4 crystal[31]. The CRESST detectors are sensitive to spin dependent WIMP interactions, and are located in the same underground laboratory as DAMA.EDELWEISSOf the various Dark Matter direct detection experiments, the EDELWEISS (Expérience pour Detecter Les WIMPs en Site Souterrain) experiment resembles CDMS the most.…”

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confidence: 99%

Search for weakly interacting massive particles with the Cryogenic Dark Matter Search experiment

Saab

2002

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From individual galaxies, to clusters of galaxies, to in between the cushions of your sofa, Dark Matter appears to be pervasive on every scale. With increasing accuracy, recent astrophysical measurements, from a variety of experiments, are arriving at the following cosmological model : a flat cosmology (Ω k = 0) with matter and energy densities contributing roughly 1/3 and 2/3 (Ω m = 0.35, Ω Λ = 0.65). Of the matter contribution, it appears that only ∼ 10% (Ω b ∼ 0.04) is attributable to baryons. Astrophysical measurements constrain the remaining matter to be non-realtivistic, interacting primarily gravitationally. Various theoretical models for such Dark Matter exist. A leading candidate for the non-baryonic matter are Weakly Interacting Massive Particles (dubbed WIMPS). These particles, and their relic density may be naturally explained within the framework of Super-Symmetry theories. Super-Symmetry also offers predictions as to the scattering rates of WIMPs with baryonic matter allowing for the design and tailoring of experiments that search specifically for the WIMPs. The Cryogenic Dark Matter Search experiment is searching for evidence of WIMP interactions in crystals of Ge and Si. Using cryogenic detector technology to measure both the phonon and ionization response to a particle recoil the CDMS detectors are able to discriminate between electron and nuclear recoils, thus reducing the large rates of electron recoil backgrounds to levels with which a Dark Matter search is not only feasible, but far-reaching. This thesis will describe in some detail the physical principles behind the CDMS detector technology, highlighting the final step in the evolution of the detector design and characterization techniques. In iv addition, data from a 100 day long exposure of the current run at the Stanford Underground Facility will be presented, with focus given to detector performance as well as to the implications on allowable WIMP mass-cross-section parameter space. v It is almost impossible to express, within the scope of one or two pages, the immense debts of gratitude I owe to the numerous people who have, directly and indirectly, made this possible. By this I refer not just to the dissertation itself, but the entire Ph.D. process that began when I arrived at Stanford five years ago. Let me begin by thanking Marcia Keating, Dawn Hyde, and Kathleen Guan who were extremely patient and helpful whenever I ran into their offices with the latest emergency regarding the progress of my degree or status of my student visa or (most important of all) my paycheck. Along with the rest of the physics department administerial staff; Rosenna Yau, Cindy Mendel, and Jennifer Conan-Tice, they made it possible for me to concentrate on my work here at Stanford rather than the logistics of my student status. Of course, none of the research that I did would have been possible without the help and support of the Cabrera group. The groups administrative assistant, Linda Hubly, was instrumental in the acquisition of various experimental equipm...

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Simultaneous measurement of phonons and scintillation light for active background rejection in the CRESST experiment

Cited by 15 publications

References 6 publications

Thermal properties ofCaMoO4: Lattice dynamics and synchrotron powder diffraction studies

Thermal properties ofCaMoO4: Lattice dynamics and synchrotron powder diffraction studies

Neutron background at the Canfranc underground laboratory and its contribution to the IGEX-DM dark matter experiment

Search for weakly interacting massive particles with the Cryogenic Dark Matter Search experiment

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