A 2.5 per cent measurement of the growth rate from small-scale redshift space clustering of SDSS-III CMASS galaxies

By B. Reid, H. Seo, A. Leauthaud, J. Tinker, M. White. 2014

181 citations recorded by the source corpus.

Author(s): Reid, BA; Seo, HJ; Leauthaud, A; Tinker, JL; White, M | Abstract: © 2014 The Authors. We perform the first fit to the anisotropic clustering of Sloan Digital Sky Survey III CMASS data release 10 galaxies on scales of ~0.8-32 h-1 Mpc.Astandard halo occupation distribution model evaluated near the best-fitting Planck ? cold dark matter (?CDM) cosmology provides a good fit to the observed anisotropic clustering, and implies a normalization for the peculiar velocity field of M~2 × 1013h-1 M haloes of fσ8(z = 0.57) = 0.450 ± 0.011. Since this constraint includes both quasi-linear and non-linear scales, it should severely constrain modified gravity models that enhance pairwise infall velocities on these scales. Though model dependent, our measurement represents a factor of 2.5 improvement in precision over the analysis of DR11 on large scales, fσ8(z = 0.57) = 0.447 ± 0.028, and is the tightest single constraint on the growth rate of cosmic structure to date. Our measurement is consistent with the Planck ?CDM prediction of 0.480 ± 0.010 at the ~1.9σ level. Assuming a halo mass function evaluated at the best-fitting Planck cosmology,we also find that 10 per cent of CMASS galaxies are satellites in haloes of mass M ~ 6 × 1013 h-1 M. While none of our tests and model generalizations indicate systematic errors due to an insufficiently detailed model of the galaxy-halo connection, the precision of these first results warrant further investigation into the modelling uncertainties and degeneracies with cosmological parameters.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/914362268ecd58be4ea5fd10018fb8575366a173

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

Planck2015 results (2015, unknown): “…of the RSD signal currently comes from scales where nonlinear effects and galaxy bias are significant and must be accurately modelled in order to relate the density and velocity fields (see, e.g., the discussions in Bianchi et al. 2012; Okumura et al. 2012; Reid et al. 2014; White et al. 2015).”
Consistent modeling of velocity statistics and redshift-space distortions in one-loop perturbation theory (2020, background): “nation by FoG eects at high . Devising such an estimator is outside the scope of this work, though we note that related strategies have been suggested to deal with systematics in conguration space [110,111] and plane-of-the-sky eects near = 0 [92]. The above suggests that rather than simply discardi”
Intrinsic alignments of SDSS-III BOSS LOWZ sample galaxies (2014, background): “…to correct the bias in galaxy-galaxy correlation function on large scales (& fiber collision scale), but can introduce some bias at small scales since the redshift separation between the collided pair of galaxies has been artificially set to zero, which is not always correct (Reid et al. 2014).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Measuring growth rate and geometry with anisotropic clustering (2013, background): “The amplitude constraints from 4 For an update on the small-scale σ2FOG estimate and its effect on fσ8 measurement see Reid et al. (2014). monopole are collinear to the combination A0 = (b2 + 2/3b f + 1/5 f 2)σ28, also as expected from linear theory.”
The VIMOS Public Extragalactic Redshift Survey (VIPERS): The growth of structure at $0.5 < z < 1.2$ from redshift-space distortions in the clustering of the PDR-2 final sample (2016, background): “These included in particular the 6dfGS (Beutler et al. 2012), WiggleZ (e.g. Blake et al. 2011; Contreras et al. 2013) and BOSS (e.g. Reid et al. 2014; Beutler et al. 2016; Satpathy et al. 2016; Sanchez et al. 2016; Grieb et al. 2016).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Testing gravity with redshift-space distortions using the power spectrum multipoles (2013, background): “These issues are beyond the scope of this paper and should be addressed using the galaxy clustering or the galaxy–galaxy lensing signal at somewhat smaller scales where the 1-halo term is more dominant (for CMASS see Miyatake et al. 2013; Reid et al. 2014).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements from CMASS anisotropic galaxy clustering (2013, methodology): “Similar analysis have been also applied on the SDSS-III BOSS galaxy sample (Reid et al. 2012, 2014; Tojeiro et al. 2012, 2014; Anderson et al. 2013, 2014a,b; Chuang et al. 2013; Kazin et al. 2013; Manera et al. 2013; Nuza et al. 2013; Samushia et al. 2013, 2014; Sanchez et al. 2013a; Beutler et al.…”
THE ELEVENTH AND TWELFTH DATA RELEASES OF THE SLOAN DIGITAL SKY SURVEY: FINAL DATA FROM SDSS-III (2015, background): “…clustering (Guo et al. 2015), anisotropic galaxy clustering (Song et al. 2014; Samushia et al. 2014; Sánchez et al. 2014; Gil-Maŕın et al. 2014b,a; Reid et al. 2014; Beutler et al. 2014b), galaxy clustering in the low-redshift sample (LOWZ; Tojeiro et al. 2014), the baryon oscillations (BAO)…”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the configuration-space clustering wedges (2016, unknown): “…the bispectrum (Gil-Marı́n et al. 2015), a detailed study of RSDs on small scales including the impact of effects such as velocity or assembly bias (Reid et al. 2014), or the advancement of methods to reconstruct the underlying density field (Kitaura et al. 2016b) are strategies that could help…”
Lensing is Low: Cosmology, Galaxy Formation, or New Physics? (2016, methodology): “…only be carried out in tandem with the modelling of the CMASS–halo connection), differences between the lensing and predictions from models trained on the two-dimensional redshift-space correlation function (Reid et al. 2014; Rodrı́guez-Torres et al. 2016) could be a signature of modified gravity.”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the power spectrum and bispectrum of the DR12 BOSS galaxies (2016, methodology): “…et al ’14 Gil-Marin ’16 This work DR11 DR12 fσ 8 LOWZ sample 0.25 0.3 0.35 0.4 0.45 0.5 0.55 0.6 Beutler et al. ’14 Samushia et al. ’14 Sanchez et al ’14 Reid et al. ’14 Alam et al ’15 Gil-Marin ’15 Chuang et al. ’16 Gil-Marin ’16 This W ork DR11 DR12 fσ 8 CMASS sample Figure 14.”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample (2016, methodology): “RSD measurements from earlier BOSS data releases, using a variety of technical approaches, include Reid et al. (2012, 2014); Tojeiro et al. (2012); Chuang et al. (2013a); Samushia et al. (2013, 2014); Sánchez et al. (2013, 2014); Beutler et al. (2014a); Gil-Marı́n et al. (2016b); Alam et al.…”
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: measurement of the growth rate of structure from the anisotropic correlation function between redshift 0.8 and 2.2 (2018, background): “In their measurement of fσ 8 at small scales where the effect of collisions is large, Reid et al. (2014) redefined the correlation function multipoles by excluding the region above a given threshold μs(s) depending on the separation s and defined by the minimum angular distance between two objects…”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Fourier space (2016, methodology): “The runPB simulations use a CMASSlike halo occupation distribution (HOD) model to populate dark matter haloes with galaxies (see Reid et al. 2014 for details).”
THE SDSS-IV EXTENDED BARYON OSCILLATION SPECTROSCOPIC SURVEY: OVERVIEW AND EARLY DATA (2015, methodology): “The mean pixel width within the forest is recorded as dx (units of Mpc/h) and SNR is the mean signal-to-noise ratio per pixel within the forest.”