Complementarity of Dark Matter Direct Detection Targets

Physical review D: Particles and fields (Impact Factor: 4.86). 12/2010; 83(8). DOI: 10.1103/PhysRevD.83.083505
Source: arXiv


We investigate the reconstruction capabilities of the dark matter mass and spin-independent cross section from future ton-scale direct detection experiments using germanium, xenon, or argon as targets. Adopting realistic values for the exposure, energy threshold, and resolution of dark matter experiments which will come online within 5 to 10 years, the degree of complementarity between different targets is quantified. We investigate how the uncertainty in the astrophysical parameters controlling the local dark matter density and velocity distribution affects the reconstruction. For a 50 GeV WIMP, astrophysical uncertainties degrade the accuracy in the mass reconstruction by up to a factor of ∼4 for xenon and germanium, compared to the case when astrophysical quantities are fixed. However, the combination of argon, germanium, and xenon data increases the constraining power by a factor of ∼2 compared to germanium or xenon alone. We show that future direct detection experiments can achieve self-calibration of some astrophysical parameters, and they will be able to constrain the WIMP mass with only very weak external astrophysical constraints.

© 2011 American Physical Society

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    • "We make the simplifying assumption of an energy-independent acceptance of data quality cuts, and adjust the acceptance-corrected exposure to accurately reproduce the exclusion limit in the (m ˜ χ 0 1 , σ SI χN ) plane reported in Ref. [33] in the mass range of interest. For the calculation of the number of expected signal recoil events we fix the astrophysical parameters that describe the density and velocity distribution of DM particles at the commonly adopted benchmark values: local CDM density ρ ,CDM = 0.4 GeV cm −3 , circular velocity v 0 = 235 km s −1 and escape velocity v esc = 550 km s −1 (see, e.g., [34] and references therein for a recent discussion of the astrophysical uncertainties on these quantities). For the contribution of the light quarks to the nucleon form factors for the spin-independent WIMP-nucleon cross section we have adopted the values f T u = 0.02698, f T d = 0.03906 and f T s = 0.36 [35] derived experimentally from measurements of the pionnucleon sigma term 2 . "
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    Journal of High Energy Physics 11/2013; 2014(12). DOI:10.1007/JHEP12(2014)114 · 6.11 Impact Factor
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    • "WIMPs are typically sought via three observational channels: direct WIMP-nucleon scattering (e.g. [5] [6] [7] [8] [9] [10] [11]), production at accelerators (e.g. [12] [13] [14] [15] [16] [17] [18]) and indirect detection of SM products of WIMP self-annihilation (e.g. "
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    Journal of Cosmology and Astroparticle Physics 11/2012; 2012. DOI:10.1088/1475-7516/2012/11/057 · 6.04 Impact Factor
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    • "As described in the experimental papers, the bound is obtained from the p-value of a likelihood function which includes the systematic and statistical error in signal and background, as well as the uncertainties on scintillation efficiency and escape velocity; see [11] for details. However, the experimental analysis does not consider the astrophysical uncertainties associated with the chosen velocity distribution and DM halo profile [31] [32] [33], nor the nuclear physics uncertainties associated with calculations of the π-nucleon sigma-term Σ πN [34], which are in fact dominant. Here and below we denote these theoretical uncertainties with τ . "
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