Limits on WIMP dark matter using sapphire cryogenic detectors

Angloher, G.; Bruckmayer, M.; Bucci, C.; Bühler, M.; Cooper, S.; Cozzini, C.; DiStefano, P.; Feilitzsch, F. von; Frank, T.; Hauff, D.; Jagemann, T.; Jochum, J.; Jörgens, V.; Keeling, R.; Kraus, H.; Loidl, M.; Marchese, José Abramo; Meier, Oliver; Nagel, U.; Pröbst, F.; Ramachers, Y.; Rulofs, A.; Schnagl, J.; Seidel, W.; Sergeyev, Ivan V.; Sisti, M.; Stark, M.; Uchaikin, S.; Stodolsky, L.; Wulandari, H.; Zerle, L.

doi:10.1016/s0927-6505(02)00111-1

Cited by 180 publications

(81 citation statements)

References 30 publications

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“…In each scattering the DM particle loses energy according to (2), and we assume isotropic scattering in the c.m. frame.…”

Section: Xqc Experimentsmentioning

confidence: 99%

“…This corresponds to the electron response threshold divided by the quenching factor of the target. [2] Al2O3 1400 m 600 eV 0.8 (1.1) GeV DAMA, [3] NaI 1400 m 6 keV 3.5 (5) GeV ELEGANT, [6] NaI 442 m 10 keV 5 (8) GeV COSME I, [5] Ge 263 m 6.5 keV 5.5 (8) GeV CDMS, [31] Si, Ge 10.6 m 25 keV 9.8 (16) GeV…”

Section: Underground Detectionmentioning

confidence: 99%

“…In the region where the window is located, i.e. masses below 2 GeV, we perform the analysis based on the fit method used by the CRESST group, [2]. The measured spectrum is fit with an empirical function called B.…”

Section: Experiments Target Depthmentioning

confidence: 99%

“…When σ 0 is such that the simulated signal S is below the measured signal B 0 , B ′ adds to the signal S, completing it to B 0 and the likelihood is unchanged. With increasing σ 0 , when S starts to exceed the function B 0 , B ′ becomes zero, and we calculate the likelihood using S alone in such bins, leading to a new likelihood L. Following the CRESST collaboration prescription, σ 0 excluded at 90% CL is taken to be the value of σ 0 giving ln L−ln L 0 = −1.28 2 /2 [2], since 10% of the area of a normalized Gaussian distribution of width σ is 1.28σ above than the peak. We show the window obtained this way in Figure 2 and for the low mass range, in Figure 1.…”

Section: Experiments Target Depthmentioning

confidence: 99%

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Window in the dark matter exclusion limits

2005

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We consider the cross section limits for light dark matter candidates (m = 0.4 to 10 GeV). We calculate the interaction of dark matter in the crust above underground dark matter detectors and find that in the intermediate cross section range, the energy loss of dark matter is sufficient to fall below the energy threshold of current underground experiments. This implies the existence of a window in the dark matter exclusion limits in the micro-barn range.

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“…In each scattering the DM particle loses energy according to (2), and we assume isotropic scattering in the c.m. frame.…”

Section: Xqc Experimentsmentioning

confidence: 99%

Section: Underground Detectionmentioning

confidence: 99%

Section: Experiments Target Depthmentioning

confidence: 99%

Section: Experiments Target Depthmentioning

confidence: 99%

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Window in the dark matter exclusion limits

2005

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“…Notice that the most important limits on the elastic cross section for light dark matter candidates are given by the Xenon10 Collaboration [29]. However, when the dark matter mass is below 10 GeV the best bounds are coming from CRESST-1 [30] and they are very weak.…”

Section: Relic Density Direct Detection and Higgs Decaysmentioning

confidence: 99%

Baryon asymmetry and dark matter through the vector-like portal

Pérez

Wise

2013

J. High Energ. Phys.

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A possible connection between the cosmological baryon asymmetry, dark matter and vectorlike fermions is investigated. In this scenario an asymmetry generated through baryogenesis or leptogenesis (in the vector-like matter sector) connects the baryon asymmetry to the dark matter density. We present explicit renormalizable models where this connection occurs. These models have asymmetric dark matter and a significant invisible Higgs decay width to dark matter particles is possible. We refer to this type of scenario as the vector-like portal. In some asymmetric dark matter models there are potential naturalness issues for the low energy effective theory. We address that issue in the models we consider by starting with a Lagrangian that is the most general renormalizable one consistent with the gauge (and discrete) symmetries and showing the low energy effective theory automatically has the required form as a consequence of the symmetries of the full theory. We show that the mass of the dark matter candidate is predicted in these scenarios.

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Applications of Superconductivity

Buckel

Kleiner

2004

Superconductivity

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Limits on WIMP dark matter using sapphire cryogenic detectors

Cited by 180 publications

References 30 publications

Window in the dark matter exclusion limits

Window in the dark matter exclusion limits

Baryon asymmetry and dark matter through the vector-like portal

Applications of Superconductivity

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