New constraints on coupled dark energy from the Planck satellite experiment

Salvatelli, Valentina; Marchini, Agnese; Lopez-Honorez, Laura; Mena, Olga

doi:10.1103/physrevd.88.023531

Cited by 157 publications

(163 citation statements)

References 54 publications

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“…IV, baryons, DM and DE interact only indirectly by gravitation (via the Poisson equation). However, DE may interact with DM non-gravitationally, via a reciprocal exchange of energy and momentum; thus, is called interacting DE (IDE) [7,73,[109][110][111]. In this section we probe the magnification angular power spectrum for an IDE scenario-assuming (hereafter) a latetime universe dominated by DM and DE only.…”

Section: The Power Spectrum With Interacting Dark Energymentioning

confidence: 99%

Large-scale imprint of relativistic effects in the cosmic magnification

Duniya

2016

Phys. Rev. D

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Apart from the known weak gravitational lensing effect, the cosmic magnification acquires relativistic corrections owing to Doppler, integrated Sachs-Wolfe, time-delay and other (local) gravitational potential effects, respectively. These corrections grow on very large scales and high redshifts z, which will be the reach of forthcoming surveys. In this work, these relativistic corrections are investigated in the magnification angular power spectrum, using both (standard) noninteracting dark energy (DE), and interacting DE (IDE). It is found that for noninteracting DE, the relativistic corrections can boost the magnification large-scale power by ∼40% at z = 3, and increases at lower z. It is also found that the IDE effect is sensitive to the relativistic corrections in the magnification power spectrum, particularly at low z-which will be crucial for constraints on IDE. Moreover, the results show that if relativistic corrections are not taken into account, this may lead to an incorrect estimate of the large-scale imprint of IDE in the cosmic magnification; including the relativistic corrections can enhance the true potential of the cosmic magnification as a cosmological probe.

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Section: The Power Spectrum With Interacting Dark Energymentioning

confidence: 99%

Large-scale imprint of relativistic effects in the cosmic magnification

Duniya

2016

Phys. Rev. D

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“…It has been suggested that a different dark sector interaction may be able to resolve the tension (Salvatelli et al 2013(Salvatelli et al , 2014Costa et al 2014;Murgia et al 2016). As a simple test, we apply the geometrical probes to a particular coupled dark energy and dark matter model which has the interaction term proportional to the dark energy component Q = ξHρ DE .…”

Section: Gcgmentioning

confidence: 99%

An Evaluation of Cosmological Models from the Expansion and Growth of Structure Measurements

Zhai

Blanton

Slosar

et al. 2017

ApJ

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We compare a large suite of theoretical cosmological models to observational data from the cosmic microwave background, baryon acoustic oscillation measurements of expansion, Type Ia SNe measurements of expansion, redshift space distortion measurements of the growth of structure, and the local Hubble constant. Our theoretical models include parametrizations of dark energy as well as physical models of dark energy and modified gravity. We determine the constraints on the model parameters, incorporating the redshift space distortion data directly in the analysis. To determine whether models can be ruled out, we evaluate the p-value (the probability under the model of obtaining data as bad or worse than the observed data). In our comparison, we find the well known tension of H 0 with the other data; no model resolves this tension successfully. Among the models we consider, the large scale growth of structure data does not affect the modified gravity models as a category particularly differently than dark energy models; it matters for some modified gravity models but not others, and the same is true for dark energy models. We compute predicted observables for each model under current observational constraints, and identify models for which future observational constraints will be particularly informative.

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“…It is also important to compare our results (and those of [44]) with those obtained for DE models or similar CDM-DE mixtures in FLRW cosmologies [1,2,7,8,[13][14][15][16]48,49], since the dynamics of LTB solutions described by q-scalars and their fluctuations can be mapped to linear perturbation on an FLRW background [40]. While the spherical symmetry of the LTB models allows for the description of a single structure, the evolution of the latter can be studied exactly throughout the full non-linear regime.…”

Section: Discussionmentioning

confidence: 75%

“…In [6,13,14] and for a similar coupling term with positive defined coupling constant, the authors find that the observational data suggest that α is smaller than 0.003 to 1σ , and smaller than 0.01 to 2σ , while a value of order 0.1 is ruled out at better than 99.95%. On the other hand, in [49] the evolution of linear perturbations in a FLRW background sharing our assumptions on CDM, DE and J q leads to the bounds − 0.22 > 3α > − 0.90 to comply with the constraints of CMB anisotropy. These results are specially interesting, since the dynamics of LTB solutions described by q-scalars and their fluctuations can be mapped to linear perturbation on an FLRW background [40].…”

Section: Critical Points In Terms Of the Parameters W And αmentioning

confidence: 74%

Interactive mixture of inhomogeneous dark fluids driven by dark energy: a dynamical system analysis

2018

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We examine the evolution of an inhomogeneous mixture of non-relativistic pressureless cold dark matter (CDM), coupled to dark energy (DE) characterised by the equation of state parameter w < −1/3, with the interaction term proportional to the DE density. This coupled mixture is the source of a spherically symmetric Lemaître-Tolman-Bondi (LTB) metric admitting an asymptotic Friedman-Lemaître-Robertson-Walker (FLRW) background. Einstein's equations reduce to a 5-dimensional autonomous dynamical system involving quasi-local variables related to suitable averages of covariant scalars and their fluctuations. The phase space evolution around the critical points (past/future attractors and five saddles) is examined in detail. For all parameter values and both directions of energy flow (CDM to DE and DE to CDM) the phase space trajectories are compatible with a physically plausible early cosmic times behaviour near the past attractor. This result compares favourably with mixtures with interaction driven by the CDM density, whose past evolution is unphysical for DE to CDM energy flow. Numerical examples are provided describing the evolution of an initial profile that can be associated with idealised structure formation scenarios.

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New constraints on coupled dark energy from the Planck satellite experiment

Cited by 157 publications

References 54 publications

Large-scale imprint of relativistic effects in the cosmic magnification

Large-scale imprint of relativistic effects in the cosmic magnification

An Evaluation of Cosmological Models from the Expansion and Growth of Structure Measurements

Interactive mixture of inhomogeneous dark fluids driven by dark energy: a dynamical system analysis

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