Limits on WIMP dark matter using sapphire cryogenic detectors
By G. Angloher, M. Bruckmayer, C. Bucci, M. Bühler, S. Cooper, C. Cozzini, P. Distefano, F. Feilitzsch, T. Frank, D. Hauff and 21 more. 2002
174 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/a814dd2755b4c2cccfc7ae00e85dfe0b04c170a2
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In Astronomy and Astrophysics
- P. Graham
- Romain Teyssier
- F. Ling
- Jonathan L. Feng
- E. Nezri
- S. Rajendran
- Matthew T. Walters
- D. Kaplan
In Atomic and Molecular Physics, and Optics
- P. Graham
- S. Rajendran
- D. Kaplan
- Jonathan L. Feng
- Romain Teyssier
- Matthew T. Walters
- E. Athanassoula
- J. Redondo
In Nuclear and High Energy Physics
- P. Graham
- S. Rajendran
- D. Kaplan
- F. Ling
- Jonathan L. Feng
- Romain Teyssier
- E. Nezri
- Matthew T. Walters
Citations in the corpus
- Dark Matter Candidates from Particle Physics and Methods of Detection (2010, methodology): “The light yellow shaded region is excluded by the direct detection experiments CRESST (205), CDMS (206), XENON10 (60), TEXONO (207), and CoGeNT (208), as indicated.”
- Dark matter direct detection signals inferred from a cosmological N-body simulation with baryons (2009, methodology): “For the second commissioned run of 2007 (CRESST-II) [122, 40], the target is changed to CaWO4.”
- Semiconductor Probes of Light Dark Matter (2012, methodology): “This is caused by our BBN/SN Astro CRESST Xe Ge Si 1 10 100 1000 104 10-8 10-7 10-6 10-5 10-4 Dark Matter Mass HMeVL Λ HH ea vy L BBN/SN Astro CRESST CDMS XENON10Xe Ge Si 1 10 100 1000 104 10-15 10-14 10-13 10-12 10-11 10-10 10-9 Dark Matter Mass HMeVL Λ HL ig ht L (a) mA = 10 MeV and (b) mA = 1 meV”