Massive black holes from dissipative dark matter

We show that a subdominant component of dissipative dark matter resembling the Standard Model can form many intermediate-mass black hole seeds during the first structure formation epoch. We also observe that, in the presence of this matter sector, the black holes will grow at a much faster rate with respect to the ordinary case. These facts can explain the observed abundance of supermassive black holes feeding high-redshift quasars. The scenario will have interesting observational consequences for dark substructures and gravitational wave production

Black hole formation in the context of dissipative dark matter

Black holes with masses of $\rm 10^6-10^9~M_{\odot}$ dwell in the centers of most galaxies, but their formation mechanisms are not well known. A subdominant dissipative component of dark matter with similar properties to the ordinary baryons, known as mirror dark matter, may collapse to form massive black holes during the epoch of first galaxies formation. In this study, we explore the possibility of massive black hole formation via this alternative scenario. We perform three-dimensional cosmological simulations for four distinct halos and compare their thermal, chemical and dynamical evolution in both the ordinary and the mirror sectors. We find that the collapse of halos is significantly delayed in the mirror sector due to the lack of $\rm H_2$ cooling and only halos with masses above $\rm \geq 10^7~ M_{\odot}$ are formed. Overall, the mass inflow rates are $\rm \geq 10^{-2}~M_{\odot}/yr$ and there is less fragmentation. This suggests that the conditions for the formation of massive objects, including black holes, are more favorable in the mirror sector

Gamma Ray Constraints on Flavor Violating Asymmetric Dark Matter

We show how cosmic gamma rays can be used to constrain models of asymmetric Dark Matter decaying into lepton pairs by violating flavor. First of all we require the models to explain the anomalies in the charged cosmic rays measured by PAMELA, FERMI and HESS; performing combined fits we determine the allowed values of the Dark Matter mass and lifetime. For these models, we then determine the constraints coming from the measurement of the isotropic gamma-ray background by FERMI for a complete set of lepton flavor violating primary modes and over a range of DM masses from 100 GeV to 10 TeV. We find that the FERMI constraints rule out the flavor violating asymmetric Dark Matter interpretation of the charged cosmic ray anomalies.Comment: 11 pages, 3 figures. v2: constraints derivation slightly modified, conclusions unchanged; some clarifications and some references added; matches version published on JCA

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.

Les Houches 2011: Physics at TeV Colliders New Physics Working Group Report

We present the activities of the "New Physics" working group for the "Physics at TeV Colliders" workshop (Les Houches, France, 30 May-17 June, 2011). Our report includes new agreements on formats for interfaces between computational tools, new tool developments, important signatures for searches at the LHC, recommendations for presentation of LHC search results, as well as additional phenomenological studies.Comment: 243 pages, report of the Les Houches 2011 New Physics Group; fix three figure

The physics case of a 3 TeV muon collider stage

In the path towards a muon collider with center of mass energy of 10 TeV ormore, a stage at 3 TeV emerges as an appealing option. Reviewing the physicspotential of such muon collider is the main purpose of this document. In orderto outline the progression of the physics performances across the stages, a fewsensitivity projections for higher energy are also presented. There are manyopportunities for probing new physics at a 3 TeV muon collider. Some of themare in common with the extensively documented physics case of the CLIC 3 TeVenergy stage, and include measuring the Higgs trilinear coupling and testingthe possible composite nature of the Higgs boson and of the top quark at the 20TeV scale. Other opportunities are unique of a 3 TeV muon collider, and stemfrom the fact that muons are collided rather than electrons. This isexemplified by studying the potential to explore the microscopic origin of thecurrent $g$-2 and $B$-physics anomalies, which are both related with muons.<br

The physics case of a 3 TeV muon collider stage

In the path towards a muon collider with center of mass energy of 10 TeV ormore, a stage at 3 TeV emerges as an appealing option. Reviewing the physicspotential of such muon collider is the main purpose of this document. In orderto outline the progression of the physics performances across the stages, a fewsensitivity projections for higher energy are also presented. There are manyopportunities for probing new physics at a 3 TeV muon collider. Some of themare in common with the extensively documented physics case of the CLIC 3 TeVenergy stage, and include measuring the Higgs trilinear coupling and testingthe possible composite nature of the Higgs boson and of the top quark at the 20TeV scale. Other opportunities are unique of a 3 TeV muon collider, and stemfrom the fact that muons are collided rather than electrons. This isexemplified by studying the potential to explore the microscopic origin of thecurrent $g$-2 and $B$-physics anomalies, which are both related with muons.<br

Muon Collider Physics Summary

The perspective of designing muon colliders with high energy and luminosity,which is being investigated by the International Muon Collider Collaboration,has triggered a growing interest in their physics reach. We present a concisesummary of the muon colliders potential to explore new physics, leveraging onthe unique possibility of combining high available energy with very precisemeasurements.<br

Muon Collider Physics Summary

The perspective of designing muon colliders with high energy and luminosity,which is being investigated by the International Muon Collider Collaboration,has triggered a growing interest in their physics reach. We present a concisesummary of the muon colliders potential to explore new physics, leveraging onthe unique possibility of combining high available energy with very precisemeasurements.<br