that m$_{χ}$ < 200 GeV (see Fig. 2). Hence, the assumption of a thermal history is necessary to conclude that the neutralino is a Bino-Higgsino admixture, rather than Wino-Higgsino. In the next three subsections we will attempt to elucidate the difficulties one encounters when trying to suppress SI and/or SD. This will allow us to argue that large SI and SD DD signals are the generic prediction for a well-tempered MSSM neutralino, since suppression of either SI or SD or both requires doing some gymnastics. While future data may force these contortions upon us, we conjecture that if the DM is a well-tempered neutralino, it is likely to be discovered in the next generation of DD experiments. There are two ways to suppress both SI and SD. The first is to make | Z$_{H}$$_{u}$ | = | Z$_{H}$$_{d}$ | = 0, which is equivalent to the µ → ∞ limit. This limit leads to fine-tuning of the electroweak scale. To achieve the proper thermal relic abundance in this case requires a Bino-Wino mix. Note that the Bino and Wino only mix indirectly through the Higgsino. Therefore, two insertions of the mixing factor are required, and the resulting mixing is of size ( m$_{Z}$/µ ) $^{2}$. One can see the effects of this limit by inspecting the red crosses in Figs. 3, 4 and 5. The upper bound in Figs. 3 and 4 are from points which are either Bino/Higgsino or fully mixed states while the points with the smallest values for SI are due to either Wino/Bino neutralinos or the cancellations discussed in Sec. VI D. The second option is to take M$_{1}$$_{,}$$_{2}$ ≫ µ . This will imply that Z$_{B,W}$ = 0, thereby suppressing SI DD, and | Z$_{H}$$_{u}$ | = | Z$_{H}$$_{d}$ | so that SD DD is also zero. Reproducing the measured relic density then requires µ ≈ 1 TeV. When one does impose the thermal relic density as a prior, Fig. 2 shows that for DM masses of O (TeV), i.e. the region of dominantly Higgsino DM, the SD cross section ranges from O (10 − $^{5}$pb) to 0. Fig. 5 shows the corresponding SI cross sections for this range. The trend of SI and SD going to zero in this plot is due to the limit M$_{1}$$_{,}$$_{2}$ → ∞ . Thermal dark matter in either of these two limits ( µ or M$_{1}$$_{,}$$_{2}$ → ∞ ) will have a finely-tuned electroweak scale. Note that for either pure Wino or pure Higgsino DM there is a 1-loop diagram which leads to an SI DD cross section of O (10 − $^{11}$pb) or O (10 − $^{12}$pb) and an SD DD cross section of O (10 − $^{9}$pb) or O (10 − $^{10}$pb) for the Wino or Higgsino case respectively [61]. We neglect this tiny contribution in our numerical scans. 21 B. Small SI and Small SD