Constraints on interacting dark energy models from Planck 2015 and redshift-space distortion data

Costa, André A.; Xu, X. W.; Wang, Bin; Abdalla, Élcio

doi:10.1088/1475-7516/2017/01/028

Cited by 114 publications

(135 citation statements)

References 46 publications

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“…Percival et al 2004;Davis et al 2011;Feix et al 2015;Huterer et al 2017;Adams & Blake 2017). Moreover, it has been shown that RSD provide a powerful probe to constrain the mass of relic cosmological neutrinos (Marulli et al 2011;Upadhye 2019) and the main parameters of interacting DE models (Marulli et al 2012a;Costa et al 2017), as well as helping in breaking the degeneracy between modified gravity and massive neutrino cosmologies (Moresco & Marulli 2017;Wright et al 2019;García-Farieta et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Validating the methodology for constraining the linear growth rate from clustering anisotropies

García-Farieta

Marulli

Moscardini

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Redshift-space clustering distortions provide one of the most powerful probes to test the gravity theory on the largest cosmological scales. In this paper we perform a systematic validation study of the state-of-the-art statistical methods currently used to constrain the linear growth rate from redshift-space distortions in the galaxy two-point correlation function. The numerical pipelines are tested on mock halo catalogues extracted from large N-body simulations of the standard cosmological framework, in the redshift range 0.5 z 2. We consider both the monopole and quadrupole multipole moments of the redshift-space two-point correlation function, as well as the radial and transverse clustering wedges, in the comoving scale range 10 < r[h −1 Mpc] < 55. Moreover, we investigate the impact of redshift measurement errors, up to δz ∼ 0.5%, which introduce spurious clustering anisotropies. We quantify the systematic uncertainties on the growth rate and linear bias measurements due to the assumptions in the redshiftspace distortion model. Considering both the dispersion model and two widely-used models based on perturbation theory, that is the Scoccimarro (2004) model and the Taruya et al. (2010) model, we find that the linear growth rate is underestimated by about 5 − 10% at z < 1, while limiting the analysis at larger scales, r > 30 h −1 Mpc, the discrepancy is reduced below 5%. At higher redshifts, we find instead an overall good agreement between measurements and model predictions. The Taruya et al. (2010) model is the one which performs better, with growth rate uncertainties below about 3%. The effect of redshift errors is degenerate with the one of small-scale random motions, and can be marginalised over in the statistical analysis, not introducing any statistically significant bias in the linear growth constraints, especially at z ≥ 1.

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Section: Introductionmentioning

confidence: 99%

Validating the methodology for constraining the linear growth rate from clustering anisotropies

García-Farieta

Marulli

Moscardini

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…These values of the interaction parameters were chosen so as to maximise the effects of the interaction while at the same time respecting the constraints obtained in Refs. [31,32], which we took as guidelines. The evolution for each model was computed by setting the same initial conditions for all models well inside the past DM-dominated era and numerically integrating the evolution equations.…”

Section: Distinguishing Interactionsmentioning

confidence: 99%

3-Form Cosmology: Phantom Behaviour, Singularities and Interactions

2017

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Abstract:The latest cosmological observations by the Planck collaboration (and combined with others) are compatible with a phantom-like behaviour (w < −1) for the dark energy equation of state that drives the current acceleration of the Universe. With this mindset, we look into models where dark energy is described by a 3-form field minimally coupled to gravity. When compared to a scalar field, these models have the advantage of more naturally accommodating a cosmological-constant and phantom-like behaviours. We show how the latter happens for a fairly general class of positive-valued potentials, and through a dynamical system approach, we find that in such cases the 3-form field leads the Universe into a Little Sibling of the Big Rip singular event into the future. In this work, we explore the possibility of avoiding such singularity via an interaction in the dark sector between cold dark matter and the 3-form field. For the kind of interactions considered, we deduce a condition for replacing the LSBR by a late time de Sitter phase. For specific examples of interactions that meet this condition, we look for distinctive imprints in the statefinder hierarchy {S 3(1) ; S 4 (1) }, {S 3 (1) ; S 5 (1) }, and in the growth rate of matter, (z), through the composite null diagnostic (CND).

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“…Alternatively, one can take into account modifications of the standard cold DM scenario, including a cannibal dark matter [17], partially acoustic dark matter models [18], dissipative dark matter models [19], hot axions [20], charged DM with chiral photons [21] and decaying DM scenarios [22][23][24][25][26][27][28][29][30][31][32][33][34][35][36], etc., which provide other possible solutions to resolve the tensions. Moreover, DM self-interactions [37] and DM-DE interacting models [38][39][40][41][42][43][44][45][46][47][48][49] as well as the modified gravity [50,51] are also possible solutions to fix such the tensions.…”

Section: Introductionmentioning

confidence: 99%

Fractional Dark Matter decay: cosmological imprints and observational constraints

Xiao¹,

Zhang²,

An³

et al. 2020

J. Cosmol. Astropart. Phys.

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If a fraction f dcdm of the Dark Matter decays into invisible and massless particles (so-called "dark radiation") with the decay rate (or inverse lifetime) Γ dcdm , such decay will leave distinctive imprints on cosmological observables. With a full consideration of the Boltzmann hierarchy, we calculate the decay-induced impacts not only on the CMB but also on the redshift distortion and the kinetic Sunyaev-Zel'dovich effect, while providing detailed physical interpretations based on evaluating the evolution of gravitational potential. By using the current cosmological data with a combination of Planck 2015, Baryon Acoustic Oscillation and redshift distortion measurements which can improve the constraints, we update the 1σ bound on the fraction of decaying DM from f dcdm 5.26% to f dcdm 1.99% for the short-lived DM (assuming Γ dcdm /H 0 10 4 ). However, no constraints are improved from RSD data (f dcdm 1.03%) for the long-lived DM (i.e., Γ dcdm /H 0 10 4 ). We also find the fractional DM decay can only slightly reduce the H 0 and σ 8 tensions, which is consistent with other previous works. Furthermore, our calculations show that the kSZ effect in future would provide a further constraining power on the decaying DM.

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Constraints on interacting dark energy models from Planck 2015 and redshift-space distortion data

Cited by 114 publications

References 46 publications

Validating the methodology for constraining the linear growth rate from clustering anisotropies

Validating the methodology for constraining the linear growth rate from clustering anisotropies

3-Form Cosmology: Phantom Behaviour, Singularities and Interactions

Fractional Dark Matter decay: cosmological imprints and observational constraints

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