micrOMEGAs4.1: Two dark matter candidates

By G. B'elanger, Fawzi Boudjema, Alexander Pukhov, A. Semenov. Computer Physics Communications, 2014

460 citations recorded by the source corpus.

micrOMEGAs is a code to compute dark matter observables in generic extensions of the standard model. This version of micrOMEGAs includes a generalization of the Boltzmann equations to take into account the possibility of two dark matter candidates. The modification of the relic density calculation to include interactions between the two dark matter sectors as well as semi-annihilation is presented. Both dark matter signals in direct and indirect detection are computed as well. An extension of the standard model with two scalar doublets and a singlet is used as an example. Program summary Program title: MicrOMEGAs4.1 Catalogue identifier: ADQR_v4_0 Program summary URL:http://cpc.cs.qub.ac.uk/summaries/ADQR_v4_0.html Program obtainable from: CPC Program Library, Queen’s University, Belfast, N. Ireland Licensing provisions: Standard CPC licence, http://cpc.cs.qub.ac.uk/licence/licence.html No. of lines in distributed program, including test data, etc.: 738425 No. of bytes in distributed program, including test data, etc.: 9807620 Distribution format: tar.gz Programming language: C and Fortran. Computer: PC, Mac. Operating system: UNIX (Linux, Darwin). RAM: 50MB depending on the number of processes required. Classification: 1.9, 11.6. Catalogue identifier of previous version: ADQR_v3.0 Journal reference of previous version: Comput. Phys. Comm. 185 (2014) 960 External routines: CalcHEP, SuSpect, NMSSMTools, CPSuperH, LoopTools, HiggsBounds Does the new version supersede the previous version?: Yes Nature of problem: Calculation of the relic density and direct and indirect detection rates of the lightest stable particle in particle physics models with at most two stable dark matter candidates. Solution method: In the case where the two dark matter particles have very different masses, we find that the equations for the evolution of the density of dark matter behave as stiff equations. To solve these we use the backward scheme and the Rosenbrock algorithm. The standard solution based on the Runge–Kutta method is still used for models with only one dark matter candidate. Reasons for new version: There are many experiments that are currently searching for the remnants of dark matter annihilation and the relic density is determined precisely from cosmological measurements. In this version we generalize the Boltzmann equations to take into account the possibility of two dark matter candidates. Thus, in solving for the relic density we include interactions between the two dark matter sectors as well as semi-annihilation. The dark matter signals in direct and indirect detection are computed as well. Summary of revisions: • Generalization of the Boltzmann equations to include two dark matter candidates, their interactions and semi-annihilations, the relative density of the two dark matter components is taken into account when computing direct/indirect detection rates. • Upgrade of the numerical method for solving the Boltzmann equations. • Include sample extensions of the standard model with extra doublet and singlets which contain two stable neutral particles. Unusual features: Depending on the parameters of the model, the program generates additional new code, compiles it and loads it dynamically. Running time: 4 sec

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/6286289ecfbd86c3b8f4dea02be0e3cfb82f6a5e

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Citations in the corpus

Recommendations on presenting LHC searches for missing transverse energy signals using simplified s-channel models of dark matter (2016, methodology): “s are typically active, and are particularly important when g DM ˛g q (e.g. [21]), for which cross sections are typically insensitive to g q, unlike LHC processes. Numerical tools, such as micrOMEGAs [33] and MadDM [34], can be used to calculate the regions of relic overproduction or underproduction”
Beyond the Standard Model Physics at the HL-LHC and HE-LHC (2018, background): “5 [277], and then restrict the new Yukawa couplings to lie on the relic surface when considering the reach of various experiments.”
Revised constraints and Belle II sensitivity for visible and invisible axion-like particles (2017, methodology): “by the observed relic abundance therefore depends slightly on m a even for xed mass ratio r. We take this dependence into account by solving the Boltzmann equation numerically using micrOmegas v4.2.5 [88]. We note that this calculation assumes that DM couples suciently strongly to photons that it re”
Gravitational wave, collider and dark matter signals from a scalar singlet electroweak baryogenesis (2017, background): “der has a much bigger time frame than other discussed experiments. Therefore, it will not be included in our comparisons. 3We use the tabulated values of g e as a function of Tfrom micrOMEGAs 3.6.9.2 [51]. { 8 { The second possibility for indirect detection of the new scalar Sis through its modicati”
Implications of unitarity and gauge invariance for simplified dark matter models (2015, methodology): “In order to calculate the relic abundance we have implemented the model in micrOMEGAs v4 [69], assuming that the mass of the Higgs singlet saturates”
Probing the pre-BBN universe with gravitational waves from cosmic strings (2018, methodology): “om T/a 1 dictated by entropy conservation, and depends on the eective number of energy density (g ) and entropy (g S) degrees of freedom for which we use the SM parametrization in micrOMEGAs 3.6.9.2 [109]. An early period of domination by something other than radiation would show up in the GW freque”
Toward (finally!) ruling out Z and Higgs mediated dark matter models (2016, methodology): “ thermal freeze-out) and for v= 10 3 c(as is typically relevant for indirect detection). Throughout this paper, unless otherwise stated, we use version 4.2.5 of the publicly available code MicrOMEGAS [1] to calculate all annihilation cross sections, thermal relic abundances, and elastic scattering c”