Constraining Interactions in Cosmology's Dark Sector

By R. Bean, E. Flanagan, I. László, M. Trodden. 2008

138 citations recorded by the source corpus.

We consider the cosmological constraints on theories in which there exists a nontrivial coupling between the dark matter sector and the sector responsible for the acceleration of the universe, in light of the most recent supernovae, large scale structure and cosmic microwave background data. For a variety of models, we show that the strength of the coupling of dark matter to a quintessence field is constrained to be less than 7% of the coupling to gravity. We also show that long-range interactions between fermionic dark matter particles mediated by a light scalar with a Yukawa coupling are constrained to be less than 5% of the strength of gravity at a distance scale of 10 Mpc. We show that all of the models we consider are quantum mechanically weakly coupled, and argue that some other models in the literature are ruled out by quantum mechanical strong coupling.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/cd8ec6e36fd2afcd0b620e525cb9d97c0da023b0

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

The effective field theory of dark energy (2012, background): “On the other hand, couplings to the dark matter sector are far less constrained (order 10% [77, 78]) and play a crucial role in models of coupled quintessence (e.”
Observational constraints on an interacting dark energy model (2009, background): “…of other interacting models have been investigated in Amendola et al. (2003); Koivisto (2005); Olivares et al. (2006); Mainini & Bonometto (2007); Bean et al. (2008); Vergani et al. (2009); Pettorino & Baccigalupi (2008); Schäfer (2008); Schaefer et al. (2008); La Vacca & Colombo (2008); He et…”
The growth of structure in interacting dark energy models (2009, background): “[7–28]).”
Equivalence Principle Implications of Modified Gravity Models (2009, background): “elementary baryons and dark matter particles are coupled to the scalar with different strengths [39, 40, 41, 42, 43, 44].”
Approaches to understanding cosmic acceleration (2009, methodology): “In [122] the datasets used included the measurements of the CMB temperature and polarization power spectrum from the WMAP 5-year data release [39, 123], the ‘union’ set of supernovae compiled by the Supernovae Cosmology Project [37], the matter power spectrum of Luminous Red Galaxies (LRG) as measur”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, background): “06 (at 95% CL for a constant coupling and an exponential potential) [152, 62, 47, 59], or possibly more [720, 711] if neutrinos are taken into account or for more realistic timedependent choices of the coupling.”
Hydrodynamical N-body simulations of coupled dark energy cosmologies (2008, methodology): “…imprints on observable features like, for example, the CMB and structure formation (Matarrese, Pietroni & Schimd 2003; Lee, Liu & Ng 2006; Bertolami, Gil Pedro & Le Delliou 2007; Guo, Ohta & Tsujikawa 2007; Mainini & Bonometto 2007a; Wang et al. 2007; Bean et al. 2008; La Vacca et al. 2009).”