Compatibility of DAMA dark matter detection with other searches

By P. Gondolo, G. Gelmini. 2005

168 citations recorded by the source corpus.

We present two examples of velocity distributions for light dark matter particles that reconcile the annual modulation signal observed by DAMA with all other negative results from dark matter searches. They are: (1) a conventional Maxwellian distribution for particle masses around 5 to 9 GeV; (2) a dark matter stream coming from the general direction of galactic rotation (not the Sagittarius stream). Our idea is based on attributing the DAMA signal to scattering off Na, instead of I, and can be tested in the immediate future by detectors using light nuclei, such as CDMS-II (using Si) and CRESST-II (using O)

Subfields: Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6d9e7d346aeec9a4609e3115c69c0ebeb6dddfb8

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Nuclear and High Energy Physics

Citations in the corpus

Galactic Searches for Dark Matter (2012, result): “There have been numerous efforts to reconcile the observed DAMA signal with other null results, and windows have remained open for low-mass spin-independent interpretations (Gondolo and Gelmini, 2005) until the recent announcement of the recent XENON100 results.”
Spin-independent elastic WIMP scattering and the DAMA annual modulation signal (2008, background): “These results are very similar to the ones of [9] (if channeling is neglected, not shown in the figure) and [19] (including channeling), where only two data points for the modulation amplitude below and above 6 keVee have been used.”
Dark Matter Candidates from Particle Physics and Methods of Detection (2010, background): “The magenta shaded region is DAMA-favored given channeling and no streams (204), and the medium green shaded region is DAMA-favored at 3σ given streams and no channeling (81).”
Dark Matter: A Primer (2010, background): “Equation (18) can then be integrated from x = 0 to x0 = mχ/T0 to find Y0 (which will be needed in (19) for the relic density) [59].”
Dark matter direct detection with non-Maxwellian velocity structure (2009, methodology): “16 the allowed parameter space for the LDM scenario for the canonical MB model, for the (averaged) simulations VL2, GHALO and GHALO-scaled, as well as two sample spheres from the halos.”
Colloquium: Annual modulation of dark matter (2013, background): “…can reasonably reproduce the observed modulation amplitude spectrum: m 10 GeV (where sodium recoils dominate) and m 80 GeV (where iodine recoils dominate) (Bottino et al., 2003, 2004; Gondolo and Gelmini, 2005; Petriello and Zurek, 2008; Chang, Pierce, and Weiner, 2009; Savage et al., 2009b).”
Phase-space structure in the local dark matter distribution and its signature in direct detection experiments (2008, background): “…RAS Downloaded from https://academic.oup.com/mnras/article-abstract/395/2/797/1747020 by guest on 30 July 2018 which are in conflict with upper limits established by other experiments (see Savage, Gondolo & Freese 2004; Gondolo & Gelmini 2005; Gelmini 2006, for a discussion and possible solutions).”
Dark matter direct detection signals inferred from a cosmological N-body simulation with baryons (2009, background): “G(ER, σ(ER)) ) , (4) where is the e ciency of the detector and the nite energy resolution of the experiment is taken into account by convoluting the di erential rate with a Gaussian distribution with spread σ(ER).”