Underground searches for dark matter involve a complicated interplay of particle physics , nuclear physics , atomic physics and astrophysics .
We attempt to remove the uncertainties associated with astrophysics by developing the means to map the observed signal in one experiment directly into a predicted rate at another .
We argue that it is possible to make experimental comparisons that are completely free of astrophysical uncertainties by focusing on integral quantities , such as g ( v _ { min } ) = \int _ { v _ { min } } dv f ( v ) / v and \int _ { v _ { thresh } } dv vg ( v ) .
Direct comparisons are possible when the v _ { min } space probed by different experiments overlap .
As examples , we consider the possible dark matter signals at CoGeNT , DAMA and CRESST-Oxygen .
We find that expected rate from CoGeNT in the XENON10 experiment is higher than observed , unless scintillation light output is low .
Moreover , we determine that S2-only analyses are constraining , unless the charge yield Q _ { y } < 2.4 { electrons / keV } .
For DAMA to be consistent with XENON10 , we find for q _ { Na } = 0.3 that the modulation rate must be extremely high ( \raise 1.29 pt \hbox { $ > $ \kern - 7.5 pt \lower 4.3 pt \hbox { $ \sim$ } } 70 \% for m _ { \chi } = 7 { GeV } ) , while for higher quenching factors , it makes an explicit prediction ( 0.8 - 0.9 cpd/kg ) for the modulation to be observed at CoGeNT .
Finally , we find CDMS-Si , even with a 10 keV threshold , as well as XENON10 , even with low scintillation , would have seen significant rates if the excess events at CRESST arise from elastic WIMP scattering , making it very unlikely to be the explanation of this anomaly .