[@Pato:2010ih], so that this may allow us to probe essentially all the wino mass range if it is the dominant component of the dark matter [@Hall:2012zp].

In summary, unless $T_R \lesssim 10^{-3}\, m_{\rm LSP}$ and $B_\phi 
\approx 0$ (or $R$-parity is broken), the mass of the LSP must be much smaller than $\tilde{m}$, and for the wino LSP $$270~{\rm GeV} < M_{\tilde{W}} \lesssim 3~{\rm TeV}.
\label{eq:m_wino}$$ (In addition, small portions of this mass range may be excluded by dark matter constraints; see e.g. Ref. [@Hryczuk:2014hpa].) The spectrum of the model in this case is depicted in Fig. \[fig:spectrum\]. Below, we consider both this TeV-scale wino case and the case with $m_{\rm LSP} 
\sim O(\tilde{m})$.

Gauge coupling unification {#subsec:gcu}
--------------------------

We now discuss unification of the SM gauge couplings in the ISS model described here. Following Ref. [@Hall:2013eko], we consider two variables $$\begin{aligned}
  R_X &= \frac{1}{\sqrt{38}} 
    \left( \frac{5}{g_1^2} -\frac{3}{g_2^2} - \frac{2}{g_3^2} \right),
\label{eq:R_X}\\
  R_H &= \frac{1}{\sqrt{14}} 
    \left( \frac{3}{g_2^2} -\frac{2}{g_3^2} - \frac{1}{g_1^2} \right).
\label{eq:R_H}\end{aligned}$$ In the absence of higher-dimensional gauge kinetic operators involving $\Sigma$, the energies at which $R_X$ and $R_H$ cross zero would correspond to the masses of the $XY$ GUT gauge fields, $M_X$, and the colored Higgs fields, $M_{H_C}$, respectively. 