Investigating the degeneracy between modified gravity and massive neutrinos with redshift-space distortions

Wright, Bill S.; Koyama, K.; Winther, Hans A.; Zhao, Gong-Bo

doi:10.1088/1475-7516/2019/06/040

Cited by 30 publications

(33 citation statements)

References 76 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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

View full text Add to dashboard Cite

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.

show abstract

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

View full text Add to dashboard Cite

show abstract

“…Further worth noting is that an extension of the current framework has also been developed to include massive neutrinos (Cataneo et al 2020;Wright et al 2019) and its implementation into ReACT will be the focus of an upcoming work. We also look to extend the current code to galaxy clustering observables, namely the redshift space power spectrum for biased tracers.…”

Section: Discussionmentioning

confidence: 99%

“…Including both MG and massive neutrinos in the 1-loop computations for Equation 15 can be done as in Wright et al (2019) as follows…”

Section: The Halo Model Reaction: Rmentioning

confidence: 99%

See 1 more Smart Citation

On the road to per cent accuracy IV: ReACT – computing the non-linear power spectrum beyond ΛCDM

Bose

Cataneo

Tröster

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

To effectively exploit large-scale structure surveys, we depend on accurate and reliable predictions of non-linear cosmological structure formation. Tools for efficient and comprehensive computational modelling are therefore essential to perform cosmological parameter inference analyses. We present the public software package ReACT, demonstrating its capability for the fast and accurate calculation of non-linear power spectra from non-standard physics. We showcase ReACT through a series of analyses on the DGP and f(R) gravity models, adopting LSST-like cosmic shear power spectra. Accurate non-linear modelling with ReACT has the potential to more than double LSST’s constraining power on the f(R) parameter, in contrast to an analysis that is limited to the quasi-linear regime. We find that ReACT is sufficiently robust for the inference of consistent constraints on theories beyond ΛCDM for current and ongoing surveys. With further improvement, particularly in terms of the accuracy of the non-linear ΛCDM power spectrum, ReACT can, in principle, meet the accuracy requirements for future surveys such as Euclid and LSST.

show abstract

“…A notorious example is the cosmic degeneracy between the ΛCDM + GR and the νCDM + MG cosmologies, where GR and MG stand for the general relativity and modified gravity, respectively (see e.g. Baldi et al 2014;Wright et al 2019). All different versions of the MG theory adopt a common tenet that the apparent acceleration of the present Universe is caused not by the dominance of the anti-gravitational Λ at the present epoch but by the deviation of the gravitational law from the prediction of GR on cosmological scales.…”

Section: Introductionmentioning

confidence: 99%

Constraining the Neutrino Mass with the Drifting Coefficient of the Field Cluster Mass Function

Ryu

Lee

2020

ApJ

View full text Add to dashboard Cite

We present a numerical analysis supporting the evidence that the redshift evolution of the drifting coefficient of the field cluster mass function is capable of breaking several cosmic degeneracies. This evidence is based on the data from the CoDECS and DUSTGRAIN-pathfinder simulations performed separately for various non-standard cosmologies including coupled dark energy, f (R) gravity and combinations of f (R) gravity with massive neutrinos as well as for the standard ΛCDM cosmology. We first numerically determine the field cluster mass functions at various redshifts in the range of 0 ≤ z ≤ 1 for each cosmology. Then, we compare the analytic formula developed in previous works with the numerically obtained field cluster mass functions by adjusting its drifting coefficient, β, at each redshift. It is found that the analytic formula with the best-fit coefficient provides a good match to the numerical results at all redshifts for all of the cosmologies. The empirically determined redshift evolution of the drifting coefficient, β(z), turns out to significantly differ among different cosmologies. It is also shown that even without using any prior information on the background cosmology the drifting coefficient, β(z), can discriminate with high statistical significance the degenerate non-standard cosmologies not only from the ΛCDM but also from one another. It is concluded that the evolution of the departure from the Einstein-de Sitter state and spherically symmetric collapse processes quantified by β(z) is a powerful probe of gravity and dark sector physics.

show abstract

Investigating the degeneracy between modified gravity and massive neutrinos with redshift-space distortions

Cited by 30 publications

References 76 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

On the road to per cent accuracy IV: ReACT – computing the non-linear power spectrum beyond ΛCDM

Constraining the Neutrino Mass with the Drifting Coefficient of the Field Cluster Mass Function

Contact Info

Product

Resources

About