Cosmological tests using redshift space clustering in BOSS DR11

Song, Yong-Seon; Sabiu, Cristiano G.; Okumura, Teppei; Oh, Minji; Linder, Eric V.

doi:10.1088/1475-7516/2014/12/005

Cited by 16 publications

(21 citation statements)

References 52 publications

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“…While the investigation of redshift-space distortions between pairs of galaxies has received enormous attention in the literature, both theoretical and observational (see e.g., [24][25][26][27][28][29][30][31][32][33][34][35][36][37][38][39][40] and [41][42][43][44][45][46][47][48][49][50][51][52][53][54][55], respectively), comparable studies concerning voids remain rare [18,19,21,23]. The aim of this paper is to assess the feasibility of measuring redshift-space distortions around voids using galaxies from a realistic mock galaxy catalog, and to compare this data with a physically motivated model.…”

Section: Contentsmentioning

confidence: 99%

Probing cosmology and gravity with redshift-space distortions around voids

Hamaus

Sutter

Lavaux

et al. 2015

J. Cosmol. Astropart. Phys.

117

163

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Abstract. Cosmic voids in the large-scale structure of the Universe affect the peculiar motions of objects in their vicinity. Although these motions are difficult to observe directly, the clustering pattern of their surrounding tracers in redshift space is influenced in a unique way. This allows to investigate the interplay between densities and velocities around voids, which is solely dictated by the laws of gravity. With the help of N -body simulations and derived mock-galaxy catalogs we calculate the average density fluctuations around voids identified with a watershed algorithm in redshift space and compare the results with the expectation from general relativity and the ΛCDM model. We find linear theory to work remarkably well in describing the dynamics of voids. Adopting a Bayesian inference framework, we explore the full posterior of our model parameters and forecast the achievable accuracy on measurements of the growth rate of structure and the geometric distortion through the Alcock-Paczyński effect. Systematic errors in the latter are reduced from ∼ 15% to ∼ 5% when peculiar velocities are taken into account. The relative parameter uncertainties in galaxy surveys with number densities comparable to the SDSS MAIN (CMASS) sample probing a volume of 1h −3 Gpc 3 yield σ f /b /(f /b) ∼ 2% (20%) and σ D A H /D A H ∼ 0.2% (2%), respectively. At this level of precision the linear-theory model becomes systematics dominated, with parameter biases that fall beyond these values. Nevertheless, the presented method is highly model independent; its viability lies in the underlying assumption of statistical isotropy of the Universe.

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Section: Contentsmentioning

confidence: 99%

Probing cosmology and gravity with redshift-space distortions around voids

Hamaus

Sutter

Lavaux

et al. 2015

J. Cosmol. Astropart. Phys.

117

163

View full text Add to dashboard Cite

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“…The RSD in galaxy redshift surveys has proven to be an important field of study (see Hamilton 1998 for a review). It offers a distinct way of estimating the cosmological parameters and/or any departure from the standard theory of structure formation (Cole et al 2005;Parkinson et al 2012;Song et al 2014;Li et al 2016). This also gives an independent estimate of the cosmological expansion rate (Guzzo et al 2008;Kazin et al 2012) and can also help to break the degeneracy between various models of modified gravity (Johnson et al 2016;de la Torre et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Modelling redshift space distortion in the post-reionization H i 21-cm power spectrum

Sarkar

Bharadwaj

2018

Monthly Notices of the Royal Astronomical Society

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The post-reionization HI 21-cm signal is an excellent candidate for precision cosmology, this however requires accurate modelling of the expected signal. Sarkar et al. (2016) have simulated the real space HI 21-cm signal, and have modelled the HI power spectrum as P HI (k) = b 2 P (k) where P (k) is the dark matter power spectrum and b(k) is a (possibly complex) scale dependent bias for which fitting formulas have been provided. This paper extends these simulations to incorporate redshift space distortion and predict the expected redshift space HI 21-cm power spectrum P s HI (k ⊥ , k ) using two different prescriptions for the HI distributions and peculiar velocities. We model P s HI (k ⊥ , k ) assuming that it is the product of P HI (k) = b 2 P (k) with a Kaiser enhancement term and a Finger of God (FoG) damping which has σ p the pair velocity dispersion as a free parameter. Considering several possibilities for the bias and the damping profile, we find that the models with a scale dependent bias and a Lorentzian damping profile best fit the simulated P

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“…The incomplete knowledge of perturbation theory results in unpredictable FoG effect as well. This theoretical limit is fully investigated in our previous work [48], and assumed [48]. Note that the reported uncertainty with the parenthesis is calculated with the assumption that the probability distribution is Gaussian.…”

Section: Boss Dr11 Catalogue and Estimatorsmentioning

confidence: 99%

Measuring neutrino mass imprinted on the anisotropic galaxy clustering

Song

2017

J. Cosmol. Astropart. Phys.

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The anisotropic galaxy clustering of large scale structure observed by the Baryon Oscillation Spectroscopic Survey Data Release 11 is analyzed to probe the sum of neutrino mass in the small mν < ∼ 1 eV limit in which the early broadband shape determined before the last scattering surface is immune from the variation of mν. The signature of mν is imprinted on the altered shape of the power spectrum at later epoch, which provides an opportunity to access the non-trivial mν through the measured anisotropic correlation function in redshift space (hereafter RSD instead of Redshift Space Distortion). The non-linear RSD corrections with massive neutrinos in the quasi linear regime are approximately estimated using one-loop order terms computed by tomographic linear solutions. We suggest a new approach to probe mν simultaneously with all other distance measures and coherent growth functions, exploiting this deformation of the early broadband shape of the spectrum at later epoch. If the origin of cosmic acceleration is unknown, mν is poorly determined after marginalising over all other observables. However, we find that the measured distances and coherent growth functions are minimally affected by the presence of mild neutrino mass. Although the standard model of cosmic acceleration is assumed to be the cosmological constant, the constraint on mν is little improved. Interestingly, the measured CMB distance to the last scattering surface sharply slices the degeneracy between the matter content and mν, and the hidden mν is excavated to be mν = 0.19 +0.28 −0.17 eV which is different from massless neutrino more than 68% confidence.PACS numbers: 98.80.-k,95.36.+x

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Cosmological tests using redshift space clustering in BOSS DR11

Cited by 16 publications

References 52 publications

Probing cosmology and gravity with redshift-space distortions around voids

Probing cosmology and gravity with redshift-space distortions around voids

Modelling redshift space distortion in the post-reionization H i 21-cm power spectrum

Measuring neutrino mass imprinted on the anisotropic galaxy clustering

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