Detectors dark matter

Dark matter searches with detector arrays up to several tens of kilograms. 

In a cryogenic experiment, one or several detectors are used for a definite goal for which they have been optimized. For example, in CUORE experiment described in Section 16.5, the sensors are the Ge thermistors, i.e. thermometers used in a small temperature range (around 10 mK). One detector is a bolometer made up of an absorber and a Ge sensor. The experiment is the array of 1000 bolometers arranged in anticoincidence circuits for the detection of the neutrinoless double-beta decay. Note that the sensors, if calibrated, could be used, as well, as very low-temperature thermometers. Also the array of bolometers can be considered a single large detector and used for different purposes as the detection of solar axions or dark matter. 

LTD-1 Low Temperature Detectors for Neutrinos and Dark Matter Proceedings of a Workshop, Field at Ringberg Castle, Tegernsee, May 12-13, 1987, ed. by K. Pretzl, N. Schmitz, L. Stodolsky, Springer-Verlag, Berlin, Heidelberg (December 1987)... 

LTD-2 Low Temperature Detectors for Neutrinos and Dark Matter II Proceedings of the Second European Workshop on Low Temperature Devices for the Detection of Low Energy Neutrinos and Dark Matter, Annecy-le-Vieux, France, May 2-6, 1988, ed. by L. Gonzales-Mestres and D. Perret-Gallix, Gif-sur-Yvette, France, Editions Frontieres (1988)... 

LTD-4 Proc. 4th Int. Conf. of Low Temperature Dark Matter and Neutrino Detectors, Oxford 1991, ed. by N.E. Booth and G.L. Salmon, Editions Frontieres, Gif-sur-Yvette, France (1992)... 

We point out that the Heaviside component of radiation does, in fact, represent a dark and massive form of radiated EM energy that is physically always present, is missed by standard detectors, is arbitrarily excluded from the EM theory, and has been completely unaccounted for in astrophysics as well as elsewhere. Certainly the EM dark-energy radiation is gravitational, so one may hypothesize it as a candidate or major contributor to resolving the dark-matter problem. In short, the dark-matter problem may arise not because of missing matter, but because of unaccounted for, undetected, and theoretically discarded dark EM radiation of Heaviside form. 

The idea here is that neutralino dark matter is to be found not only in the halo of our galaxy and in our solar system, but also here on Earth and in the room we are in. Thus if we could set up a detector that records the passage of dark matter neutralinos, we could hope of detecting neutralino dark matter. 

Figure 16.9. Annual modulation of the total counting rate (background plus possible dark matter signal) in seven years of data with the DAMA-Nal detector. A constant counting rate has been subtracted to give the residuals. The significance of the modulation is 6cr and its period is 1 year. The interpretation of the yearly modulation as due to a WIMP signal is controversial. (Figure from Bernabei et al.(2003).)...

Ahlen, S. P, Avignone, F. T., Brodzinski, R. L., Drukier, A. K., Gelmini, G. Spergel, D. N. 1987. Limits On Cold Dark Matter Candidates From An Ultralow Background Germanium Spectrometer, Phys. Lett. B195, 603 Ahmad, Q. R., et al. [SNO Collaboration] 2002. Direct evidence for neutrino flavor transformation from neutral-current interactions in the Sudbury Neutrino Observatory, Phys. Rev. Lett.89, 011301 Ahrens, J., et al. [AMANDA Collaboration] 2002. Limits to the muon flux from WIMP annihilation in the center of the earth with the AMANDA detector, Phys. Rev. D66, 032006... 

Freese, K., Gondolo, P, Newberg, H., Lewis, M. 2003. The Effects of the Sagittarius Dwarf Tidal Stream on Dark Matter Detectors, Phys. Rev. Lett., to appear [Preprint astro-ph/0310334]... 

Gondolo, P. 2002c. Recoil momentum spectrum in directional dark matter detectors, Phys. Rev. D66, 103513... 

The forthcoming km3 neutrino telescopes are discovery detectors that could widen the knowledge of the Universe. These detectors have high potential to solve questions as the detection of UHECR sources, the investigation of hadronic processes in astrophysical environments or massive dark matter. Strong scientific motivations suggest the construction of two km3 scale detectors in the Northern and the Southern Hemisphere. 

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