We provide ingredients and recipes for computing signals of TeV-scale Dark Matter annihilations and decays in the Galaxy and beyond. For each DM channel, we present the energy spectra of e(+/-); (p) over bar, (d) over bar, gamma, V(e,mu,tau)((-)) at production, computed by high-statistics simulations. We estimate the Monte Carlo uncertainty by comparing the results yielded by the PYTHIA and HERWIG event generators. We then provide the propagation functions for charged particles in the Galaxy, for several DM distribution profiles and sets of propagation parameters. Propagation of e(+/-) is performed with an improved semi-analytic method that takes into account position-dependent energy losses in the Milky Way. Using such propagation functions, we compute the energy spectra of e(+/-), (p) over bar and (d) over bar at the location of the Earth. We then present the gamma ray fluxes, both from prompt emission and from Inverse Compton scattering in the galactic halo. Finally, we provide the spectra of extragalactic gamma rays. All results are available in numerical form and ready to be consumed.
PPPC 4 DM ID: a poor particle physicist cookbook for dark matter indirect detection
Panci P;STRUMIA, ALESSANDRO
2011-01-01
Abstract
We provide ingredients and recipes for computing signals of TeV-scale Dark Matter annihilations and decays in the Galaxy and beyond. For each DM channel, we present the energy spectra of e(+/-); (p) over bar, (d) over bar, gamma, V(e,mu,tau)((-)) at production, computed by high-statistics simulations. We estimate the Monte Carlo uncertainty by comparing the results yielded by the PYTHIA and HERWIG event generators. We then provide the propagation functions for charged particles in the Galaxy, for several DM distribution profiles and sets of propagation parameters. Propagation of e(+/-) is performed with an improved semi-analytic method that takes into account position-dependent energy losses in the Milky Way. Using such propagation functions, we compute the energy spectra of e(+/-), (p) over bar and (d) over bar at the location of the Earth. We then present the gamma ray fluxes, both from prompt emission and from Inverse Compton scattering in the galactic halo. Finally, we provide the spectra of extragalactic gamma rays. All results are available in numerical form and ready to be consumed.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
