Spherical Jeans analysis for dark matter indirect detection in dwarf spheroidal galaxies- Impact of physical parameters and triaxiality

Dwarf spheroidal (dSph) galaxies are among the most promising targets for the indirect de-tection of dark matter (DM) from annihilation and/or decay products. Empirical estimates of their DM content—and hence the magnitudes of expected signals—rely on inferences from stellar-kinematic data. However, various kinematic analyses can give different results and it is not obvious which are most reliable. Using extensive sets of mock data of various sizes (mim-icking ‘ultra-faint ’ and ‘classical ’ dSphs) and an MCMC engine, here we investigate biases, uncertainties, and limitations of analyses based on parametric solutions to the spherical Jeans equation. For a variety of functional forms for the tracer and DM density profiles, as well as the orbital anisotropy profile, we examine reliability of estimates for the astrophysical J- and D-factors for annihilation and decay, respectively. For large (N & 1000) stellar-kinematic samples typical of ‘classical ’ dSphs, errors tend to be dominated by systematics, which can be reduced through the use of sufficiently general and flexible functional forms. For small (N. 100) samples typical of ‘ultrafaints’, statistical uncertainties tend to dominate sys-tematic errors and flexible models are less necessary. Finally, we find that the assumption of spherical symmetry can bias estimates of J (by up to a factor of a few) when the object is mildly triaxial (axis ratios b/a = 0.8, c/a = 0.6). A concluding table summarises the typical error budget and biases for the different sample sizes considered. We also define an optimal strategy that would mitigate sensitivity to priors and other aspects of analyses based on the spherical Jeans equation