Dark Matter CMB Constraints and Likelihoods for Poor Particle Physicists
  The cosmic microwave background provides constraints on the annihilation and
decay of light dark matter at redshifts between 100 and 1000, the strength of
which depends upon the fraction of energy ending up in the form of electrons
and photons. The resulting constraints are usually presented for a limited
selection of annihilation and decay channels. Here we provide constraints on
the annihilation cross section and decay rate, at discrete values of the dark
matter mass, for all the annihilation and decay channels whose secondary
spectra have been computed using PYTHIA in arXiv:1012.4515 ("PPPC4DMID: A Poor
Particle Physicist Cookbook for Dark Matter Indirect Detection"), namely e, mu,
tau, V -> e, V -> mu, V -> tau, u, d, s, c, b, t, gamma, g, W, Z and h. By
interpolating in mass, these can be used to find the CMB constraints and
likelihood functions from WMAP7 and Planck for a wide range of dark matter
models, including those with annihilation or decay into a linear combination of
different channels.
