On detecting interactions in the dark sector with<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>H</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>z</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:math>data

Ferreira, P. Castelo; Pavón, Diego; Carvalho, J. C.

doi:10.1103/physrevd.88.083503

Cited by 15 publications

(7 citation statements)

References 42 publications

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“…As it can be seen in Ref. [26], a positive coupling constant implies that the quantity r ≡ ρ DM /ρ DE decreases at a slower rate in the interacting model than in the ΛCDM model. This makes the energy density of dark energy closer to that of dark matter in the past, giving us a better understanding of their closer values today.…”

Section: A Theoretical Setupmentioning

confidence: 64%

Evidence for interacting dark energy from BOSS

et al. 2017

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The result presented by the BOSS-SDSS Collaboration measuring the baryon acoustic oscillations of the Lyman-alpha forest from high-redshift quasars indicates a 2.5σ departure from the standard Λ-cold-dark-matter model. This is the first time that the evolution of dark energy at high redshifts has been measured, and the current results cannot be explained by simple generalizations of the cosmological constant. We show here that a simple phenomenological interaction in the dark sector provides a good explanation for this deviation, naturally accommodating the Hubble parameter obtained by BOSS, H(z = 2.34) = 222 ± 7 km s −1 Mpc −1 . By performing a global fit of the parameters with the inclusion of this new data set together with the Planck data for the interacting model, we are able to show that some interacting models have constraints for H(2.34) and DA(2.34) that are compatible with the ones obtained by the BOSS Collaboration, showing a better concordance than ΛCDM. We also show that the interacting models that have a small positive coupling constant, which helps alleviate the coincidence problem, are compatible with the cosmological observations. Adding the likelihood of these new baryon acoustic oscillations data shows an improvement in the global fit, although it is not statistically significant. The coupling constant could not be fully constrained by the data sets used, but the dark energy equation of state shows a slight preference for a value different from a cosmological constant.PACS numbers: 95.36.+x, 98.80.Es, 95.30.Sf, 98.80.Jk

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Section: A Theoretical Setupmentioning

confidence: 64%

Evidence for interacting dark energy from BOSS

et al. 2017

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“…In fact, r + = (2/3ξ) − 1 + (9/4ξ 2 ) − (3/ξ), as is apparent in the right panel of Fig. 1 of [39] and in Fig. 2 of Olivares et al [40].…”

Section: Some Proposed Interaction Termsmentioning

confidence: 75%

Interaction in the dark sector

2015

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It may well happen that the two main components of the dark sector of the Universe, dark matter and dark energy, do not evolve separately but interact nongravitationally with one another. However, given our current lack of knowledge on the microscopic nature of these two components there is no clear theoretical path to determine their interaction. Yet, over the years, phenomenological interaction terms have been proposed on mathematical simplicity and heuristic arguments. In this paper, based on the likely evolution of the ratio between the energy densities of these dark components, we lay down reasonable criteria to obtain phenomenological, useful, expressions of the said term independent of any gravity theory. We illustrate this with different proposals which seem compatible with the known evolution of the Universe at the background level. Likewise, we show that two possible degeneracies with noninteracting models are only apparent as they can be readily broken at the background level. Further, we analyze some interaction terms that appear in the literature. PACS numbers:PACS: 98.80.-k, 95.35.+d, 95.36.+x

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“…This has resulted in the first mapping out of the cosmological deceleration-acceleration transition, the epoch when dark energy took over from nonrelativistic matter, and the first measurement of the redshift of this transition (see, e.g., Moresco et al 2016). 4 H(z) measurements have also been used to constrain some more conventional cosmological parameters, such as the density of dark energy and the density of nonrelativistic matter (see, e.g., Samushia & Ratra 2006;Chen & Ratra 2011b;Chimento & Richarte 2013;Ferreira et al 2013;Akarsu et al 2014;Bamba et al 2014;Capozziello et al 2014;Dankiewicz et al 2014;Forte 2014;Gruber & Luongo 2014;Chen et al 2015;Meng et al 2015;Alam et al 2016;Guo & Zhang 2016;Mukherjee & Banerjee 2016), typically providing constraints comparable to or better than those provided by SN Ia data, but not as good as those from BAO or CMB anisotropy measurements. More recently, H(z) data have been used to measure the Hubble constant H 0 (Verde et al 2014;Chen et al 2016a), with the resulting H 0 value being more consistent with recent lower values determined from a median statistics analysis of Huchra's H 0 compilation (Chen & Ratra 2011a), from CMB anisotropy data (Hinshaw et al 2013;Sievers et al 2013;Ade et al 2015), from BAO measurements (Aubourg et al 2015;Ross et al 2015;L'Huillier & Shafieloo 2016), and from current cosmological data and the standard model of particle physics with only three light neutrino species (see, e.g., Calabrese et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Hubble Parameter Measurement Constraints on the Redshift of the Deceleration–acceleration Transition, Dynamical Dark Energy, and Space Curvature

Farooq

Madiyar

Crandall

2017

ApJ

378

270

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We compile an updated list of 38 measurements of the Hubble parameter H(z) between redshifts 0.07z2.36 and use them to place constraints on model parameters of constant and time-varying dark energy cosmological models, both spatially flat and curved. We use five models to measure the redshift of the cosmological deceleration-acceleration transition, z da , from these H(z) data. Within the error bars, the measured z da are insensitive to the model used, depending only on the value assumed for the Hubble constant H 0 . The weighted mean of our measurements is z da =0.72±0.05 (0.84±0.03) for H 0 =68±2.8 (73.24±1.74) km sand should provide a reasonably model-independent estimate of this cosmological parameter. The H(z) data are consistent with the standard spatially flat ΛCDM cosmological model but do not rule out nonflat models or dynamical dark energy models.

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On detecting interactions in the dark sector withH(z)data

Cited by 15 publications

References 42 publications

Evidence for interacting dark energy from BOSS

Evidence for interacting dark energy from BOSS

Interaction in the dark sector

Hubble Parameter Measurement Constraints on the Redshift of the Deceleration–acceleration Transition, Dynamical Dark Energy, and Space Curvature

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