{\cal W}_\alpha /\Lambda]_{\theta^2}$ is used to reproduce the observed SM gauge couplings (see Section \[subsec:gcu\]) and we naturally expect $F_\Sigma \sim O(\tilde{m} \Lambda)$ (see Eq. (\[eq:Sigma-VEVs\])), the last contribution gives typically the gaugino masses not much smaller than $\tilde{m}$. As we will see in the next subsection, however, the wino mass may have to be lowered to a TeV scale as a result of environmental selection associated with dark matter. This occurs through a cancellation of various contributions given above, which in turn could suppress the gluino and bino masses through GUT relations. Note that the cancellation of the wino mass requires a modest suppression of $F_\Sigma$ and/or the coefficient of $[\Sigma {\cal W}^\alpha {\cal W}_\alpha /\Lambda]_{\theta^2}$ to allow the cancellation of its contribution with the rest, which are one-loop suppressed. We thus expect that the gaugino masses are in the range $$M_\lambda \approx O(10^{-2}\mbox{--}1)\, \tilde{m},
\label{eq:gaugino}$$ except possibly for the wino, which may be at a TeV scale.

TeV-scale wino {#subsec:wino}
--------------

If $R$-parity is unbroken, the lightest supersymmetric particle (LSP) is stable and contributes to the dark matter once cosmologically produced.[^6] The abundance of the LSP in the universe may depend strongly on the reheating temperature $T_R$ after 