PPPC 4 DM ID: A Poor Particle Physicist Cookbook for Dark Matter Indirect Detection

TL;DR

This paper offers comprehensive computational tools and data for predicting signals from TeV-scale dark matter annihilations and decays, aiding indirect detection efforts across multiple particle channels.

Contribution

It provides detailed energy spectra, propagation functions, and flux calculations for dark matter signals, incorporating high-statistics simulations and improved propagation methods.

Findings

Energy spectra for various particles at production are computed.

Propagation functions for charged particles are provided for different models.

Predicted gamma ray fluxes include prompt and inverse Compton contributions.

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 electrons and positrons, antiprotons, antideuterons, gamma rays, neutrinos and antineutrinos 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 electrons and positrons 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 electrons and positrons, antiprotons and antideuterons 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.