micrOMEGAs: Version 1.3

Sparticle spectra and LHC signatures for large volume string compactifications

“…Assuming a thermal relic abundance, we compute the neutralino contribution to dark matter using micrOmegas1.3 [44]. The lower bound in (3.6) is only applicable if we require that the dark matter is solely composed of neutralinos.…”

Collider signatures of gravitino dark matter with a sneutrino NLSP

“…The latter can occur if the co-annihilation cross section is small, due to the presence in the thermal bath of the slightly heavier states that can decay into the NLSP [32]. We therefore use micrOMEGAs 2.0 [29][30][31] to compute Yν numerically without approximation, and obtain that in our region of the parameter space the 1.…”

Thermal relic abundances of long-lived staus

“…T f1 marks the point at which the stau starts to decouple chemically from the background plasma, Y e τ (T f1 ) − Y eq e τ (T f1 ) ≃ λY eq e τ (T f1 ) with λ = 0.1 [54] chosen in our code. Since we use a globally adaptive Gaussian integration routine to calculate (3.3), the computation of σv (T ) is time-demanding.…”

“…Therefore, in order to ensure numerical stability, we expand the Bessel functions in (3.3) for m e τ 1 /T > 35 as in (3.5) and cancel the exponents analytically. 5 We find the starting point for the numerical integration of (3.1) by solving [54] dY eq…”

“…In contrast, the most striking findings of our study-in which Sommerfeld enhancement is not taken into account-are related to the Higgs sector of the MSSM. At this point, we should also stress that the micrOMEGAs code [53,54,55,56] allows for sophisticated calculations of the thermal relic stau abundance also in regions in which coannihilation effects become important. In fact, micrOMEGAs has already been applied in several studies to calculate Y e τ [38,40,57,42,52].…”