A travel guide to the dark matter annihilation signal

We provide a “Baedecker” or travel guide to the directions on the sky where the dark matter annihilation signal may be expected. We calculate the flux of high energy [Formula Presented] rays from annihilation of neutralino dark matter in the center of the Milky Way and the three nearest dwarf spheroidals (Sagittarius, Draco, and Canis Major), using realistic models of the dark matter distribution. Other investigators have used cusped dark halo profiles (such as the Navarro-Frenk-White profile) to claim a significant signal. This ignores the substantial astrophysical evidence that the Milky Way is not dark-matter dominated in the inner regions. We show that the annihilation signal from the Galactic Center falls by two orders of magnitude on substituting a cored dark matter density profile for a cusped one. The present and future generation of high energy [Formula Presented]-ray detectors, whether atmospheric Cherenkov telescopes or space missions such as GLAST, lack the sensitivity to detect any of the monochromatic [Formula Presented]-ray annihilation lines. The continuum [Formula Presented]-ray signal above 1 GeV and above 50 GeV may, however, be detectable either from the dwarf spheroidals or from the Milky Way itself. If the density profiles of the dwarf spheroidals are cusped, then the best prospects are for detecting Sagittarius and Canis Major. However, if the dwarf spheroidals have milder, cored profiles, then the annihilation signal is not detectable. For GLAST, an attractive strategy is to exploit the wide field of view and observe the Milky Way at medium latitudes, as suggested by Stoehr et al. This is reasonably robust against changes in the density profile.