then roughly given by $$\Omega^{\rm dec} h^2 \sim 10^{20}\, B_\phi 
    \left( \frac{T_R}{m_\phi} \right) 
    \left( \frac{m_{\rm LSP}}{10^{12}~{\rm GeV}} \right),
\label{eq:Omega-dec}$$ where $B_\phi$ is the branching fraction of the inflaton decay to the LSP. We thus find that unless $T_R \lesssim 10^{-3}\, m_{\rm LSP}$ [*and*]{} $B_\phi$ is essentially zero, the LSP with $m_{\rm LSP} \sim 
O(\tilde{m})$ will overclose the universe.

The mass of the LSP, however, may be environmentally selected: it may be reduced to the TeV region due to a cancellation of various contributions [@Hall:2011jd]. This occurs if there are environmental constraints that strongly disfavor observers in universes with much more dark matter than our own, as argued, e.g., in Ref. [@Tegmark:2005dy]. Here and below, we assume that the LSP is the wino, $\tilde{W}$. In this case, if the wino mass is smaller than about $3~{\rm TeV}$, $\Omega^{\rm th} h^2 < 0.1$ [@Hisano:2006nn]. In general, the selection effects for dark matter act on any candidate, no matter the production mechanism, so dark matter may be multi-component; in particular, axions may comprise a part of the dark matter. This consideration, therefore, gives the only upper bound on the wino mass:  $M_{\tilde{W}} \lesssim 3~{\rm TeV}$.

An important signal for a TeV-scale wino is 