same compact form as (\[scaling\]), primarily because of the likely dependence on the annihilation rate. These fluxes are typically much smaller than those generated by WIMP annihilation in the solar interior except for some special cases with resonant energy loss [@Gould]. Nevertheless, the annihilation of secluded WIMPs inside the Earth does allow a probe of much shorter mediator lifetimes, and offers additional signatures in neutrino detectors. In certain models, the signature involves pair production of muons via the decays of the mediators, a possibility that can be efficiently explored with neutrino telescopes such as SuperK and IceCube.

### 2.4 Observational sensitivity {#observational-sensitivity .unnumbered}

Some of the primary $\gamma$-ray observatories, such as atmospheric Čerenkov detectors are of limited utility in this case, as they are unable to directly observe the Sun. While, as noted above, they can be used to place limits on the flux from Jupiter, a fiducial WIMP-nucleon cross section of $10^{-40}$cm$^2$ would generate a flux that is generally too low to provide competitive sensitivity from this source. Thus, we will focus on water Čerenkov detectors and space-borne $\gamma$-ray observatories such as Fermi.

The primary limit we will use here comes from the Milagro water Čerenkov detector [@milagro], which 