Impact of dark matter direct searches and the LHC analyses on branon phenomenology

Abstract

Dark Matter direct detection experiments are able to exclude interesting parameter space regions of particle models which predict an important amount of thermal relics. We use recent data to constrain the branon model and to compute the region that is favored by CDMS measurements. Within this work, we also update present colliders constraints with new studies coming from the LHC. Despite the present low luminosity, it is remarkable that for heavy branons, CMS and ATLAS measurements are already more constraining than previous analyses performed with TEVATRON and LEP data. pacs 95.35

Constraining the parameter space of branon dark matter using white dwarf stars

“…Or, in models with a scalar dark matter particle the scattering cross section has only spin-independent contribution [40]. The same holds for the branon dark matter case [21]. So the above cross section is purely spinindependent (coherent) with no spin-dependent contribution.…”

“…The Feynman rules for the interaction vertices between branons and the standard model fields have been derived in [39]. Neglecting the difference between neutron and proton, the branon-nucleon scattering cross section is given by [15,21] …”

“…So the above cross section is purely spinindependent (coherent) with no spin-dependent contribution. Now if a nucleus consists of A nucleons in total, the branon-nucleus scattering cross section is given by [21] σ = A 2 σ n .…”

“…In these experiments an effort is made to observe the nucleus recoil after a dark matter particle scatters off the material of the detector. These direct detection experiments have put limits on the nucleon-dark matter candidate cross section for a given mass of the dark matter particle [18][19][20], while the prospects of branon direct detection have been presented in [21]. During the last 15 years or so observational data from astrophysical objects, such as the Sun [22][23][24], solar-like stars [25][26][27], white dwarfs and neutron stars [28][29][30], have been employed to offer us complementary bounds on the WIMP-nucleon cross section, see e.g.…”

Fundamental physics with the Square Kilometre Array

“…The emission from DM is mainly provided by faint sources at low redshift, and the median size of the source is large ( > ∼ arcmin). This implies that previous analyses of counts or angular correlation were not sensitive to a (Alcaraz et al 2003;Achard et al 2004) and LHC (Cembranos et al 2004(Cembranos et al , 2011Landsberg 2015;Khachatryan et al 2016) single photon event, and supernova cooling (Cembranos et al 2003c). The two solid (red) lines on the right are associated with the hot DM; the thicker line corresponds to the total DM range D h 2 = 0.126 − 0.114 (Ade et al 2016) and the thin line is the hot DM limit D h 2 < 0.126 − 0.114.…”