Dwarf spheroidal galaxies are among the most promising targets for indirect dark matter (DM) searches in -rays. The -ray flux from DM annihilation in a dwarf spheroidal galaxy is proportional to the -factor of the source. The -factor of a dwarf spheroidal galaxy is the line-of-sight integral of the DM mass density squared times $\langle \sigma_{\rm ann} v_{\rm rel} \rangle/(\sigma_{\rm ann} v_{\rm rel})0\sigma{\rm ann} v_{\rm rel}v_{\rm rel}=|{\bf v}{\rm rel}|{\bf v}{\rm rel}(\sigma_{\rm ann} v_{\rm rel})0v{\rm rel}$-independent part of . If is constant in , -factors only depend on the DM space distribution in the source. However, if varies with $v_{\rm rel}J$-factors also depend on the DM velocity distribution, and on the strength and range of the DM self-interaction. Models for self-interacting DM are increasingly important in the study of the small scale clustering of DM, and are compatible with current cosmological observations. Here we derive the -factor of 20 dwarf spheroidal galaxies from stellar kinematic data under the assumption of Yukawa DM self-interactions. -factors are derived through a profile Likelihood approach, assuming either NFW or cored DM profiles. We also compare our results with -factors derived assuming the same velocity for all DM particles in the target galaxy. We find that this common approximation overestimates the -factors by up to one order of magnitude. -factors for a sample of DM particle masses, self-interaction coupling constants and density profiles are provided electronically, ready to be used in other projects.

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