7 research outputs found
Model-independent implications of the e+, e-, anti-proton cosmic ray spectra on properties of Dark Matter
Taking into account spins, we classify all two-body non-relativistic Dark
Matter annihilation channels to the allowed polarization states of Standard
Model particles, computing the energy spectra of the stable final-state
particles relevant for indirect DM detection. We study the DM masses,
annihilation channels and cross sections that can reproduce the PAMELA
indications of an e+ excess consistently with the PAMELA p-bar data and the
ATIC/PPB-BETS e++e- data. From the PAMELA data alone, two solutions emerge: (i)
either the DM particles that annihilate into W,Z,h must be heavier than about
10 TeV or (ii) the DM must annihilate only into leptons. Thus in both cases a
DM particle compatible with the PAMELA excess seems to have quite unexpected
properties. The solution (ii) implies a peak in the e++e- energy spectrum,
which, indeed, seems to appear in the ATIC/PPB-BETS data around 700 GeV. If
upcoming data from ATIC-4 and GLAST confirm this feature, this would point to a
O(1) TeV DM annihilating only into leptons. Otherwise the solution (i) would be
favored. We comment on the implications of these results for DM models, direct
DM detection and colliders as well as on the possibility of an astrophysical
origin of the excess.Comment: Version 4: addendum about the 2013 AMS positron data (version 5: just
refinements and additions to fig. 14
PPPC 4 DM ID: A Poor Particle Physicist Cookbook for Dark Matter Indirect Detection
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.Comment: 57 pages with many figures and tables. v4: updated to include a 125
higgs boson, computation and discussion of extragalactic spectra corrected,
some other typos fixed; all these corrections and updates are reflected on
the numerical ingredients available at
http://www.marcocirelli.net/PPPC4DMID.html they correspond to Release 2.
Dark Matter in the MSSM
We have recently examined a large number of points in the parameter space of
the phenomenological MSSM, the 19-dimensional parameter space of the
CP-conserving MSSM with Minimal Flavor Violation. We determined whether each of
these points satisfied existing experimental and theoretical constraints. This
analysis provides insight into general features of the MSSM without reference
to a particular SUSY breaking scenario or any other assumptions at the GUT
scale. This study opens up new possibilities for SUSY phenomenology both in
colliders and in astrophysical experiments. Here we shall discuss the
implications of this analysis relevant to the study of dark matter.Comment: 27 pages, 19 figs; Journal version in NJP issue "Focus on Dark Matter
and Particle Physics". Previous version had 26 pages, 19 figures. Text and
some figures have been update