Indirect search for dark matter with micrOMEGAs_2.4

Abstract

We present a new module of micrOMEGAs devoted to the computation of indirect signals from dark matter annihilation in any new model with a stable weakly interacting particle. The code provides the mass spectrum, cross-sections, relic density and exotic fluxes of gamma rays, positrons and antiprotons. The propagation of charged particles in the Galactic halo is handled with a new module that allows to easily modify the propagation parameters. Program summaryProgram title: micrOMEGAs2.4 Catalogue identifier: ADQR_v2_3 Program summary URL: RAM: 50 MB depending on the number of processes required Classification: 1.9, 11.6 Catalogue identifier of previous version: ADQR_v2_3 Journal reference of previous version: Comput. Phys. Comm. 180 (2009) 747 Does the new version supersede the previous version?: Yes Nature of problem: Calculation of the relic density and detection rates of the lightest stable particle in a generic new model of particle physics. Solution method: In numerically solving the evolution equation for the density of dark matter, relativistic formulas for the thermal average are used. All tree-level processes for annihilation and coannihilation of new particles in the model are included. The cross-sections for all processes are calculated exactly with CalcHEP after definition of a model file. The propagation of the charged cosmic rays is solved within a semi-analytical two-zone model. Reasons for new version:There are many experiments that are currently searching for the remnants of dark matter annihilation. In this version we perform the computation of indirect signals from dark matter annihilation in any new model with a stable weakly interacting particle. We include the propagation of charged particles in the Galactic halo. Summary of revisions:• Annihilation cross-sections for all 2-body tree-level processes and for radiative emission of a photon for all models.• Annihilation cross-sections into polarised gauge bosons.• Annihilation cross-sections for the loop induced processes γ γ and γ Z 0 in the MSSM.• Modelling of the DM halo with a general parameterization and with the possibility of including DM clumps.• Computation of the propagation of charged particles through the Galaxy, including the possibility of modifying the propagation parameters.• Effect of solar modulation on the charged particle spectrum.• Model independent predictions of the indirect detection signals.Unusual features: Depending on the parameters of the model, the program generates additional new code, compiles it and loads it dynamically. Running time: 3 sec

Probing light higgsinos in natural SUSY from monojet signals at the LHC

“…As a complementary searches for the light higgsinos, we also investigate the probing ability of the dark matter direct detections. We computed the dark matter observables by using the package MicrOmega [51] and scan the following parameter space: 100 GeV ≤ µ ≤ 200 GeV, 0.6 TeV ≤ mQ…”

Dark matter and vectorlike leptons from gauged lepton number

“…using the procedure presented in [36]. We have opted instead to implement the model into the numerical code MICROMEGAS [38]. Not only does this facilitate the exploration of regions of parameter space where the O(v 2 ) expansion breaks down, but it also simplifies the computation of direct and indirect detection signals.…”

Testing the light dark matter scenario of the MSSM at the LHC

“…For this end, we focus on the effective spin independent (SI) DM-nucleon scattering cross section σ SI eff , which is defined by σ SI eff = × σ SĨ χ 0 1 p with being the fraction of theχ 0 1 in total DM and σ SĨ χ 0 1 p being the SIχ 0 1 − p scattering rate, and calculate it by the package micrOMEGAs [66] with its default setting σ πN = 34 MeV and σ 0 = 42 MeV. 4 In figure 4, we display σ SI eff versus mχ0 1 for the samples surviving the constraints considered in section 3 and section 4 together with 4 We note that if we take σπN = 59 MeV from [81] and σ0 = 58 MeV from [82], the SI cross section will be enhanced by a factor from 20% to 40%.…”

“…In the case that theχ 0 1 is only a fraction of the total DM, we assume that the other components of the DM have no interaction with nucleon, and consequently we can implement the constraint of the LUX experiment only by scaling the experimental upper bound of the cross section with a factor 1/ . In our analysis, both the relic density and the scattering rate are obtained by the code micrOMEGAs [66].…”