The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Data Releases 10 and 11 Galaxy samples

Anderson, Lauren; Aubourg, É.; Bailey, S.; Beutler, Florian; Bhardwaj, Vaishali; Blanton, Michael R.; Bolton, A.; Brinkmann, J.; Brownstein, Joel R.; Burden, A.; Chuang, Chia-Hsun; Cuesta, Antonio J.; Dawson, Kyle; Eisenstein, Daniel J.; Escoffier, S.; Gunn, James E.; Guo, Hong; Ho, Shirley; Honscheid, K.; Howlett, Cullan; Kirkby, D.; Lupton, Robert H.; Manera, Marc; Maraston, Claudia; McBride, Cameron K.; Mena, Olga; Montesano, Francesco; Nichol, R. C.; Nuza, Sebastián E.; Olmstead, Matthew D.; Padmanabhan, Nikhil; Palanque-Delabrouille, N.; Parejko, John K.; Percival, Will J.; Petitjean, P.; Prada, Francisco; Price-Whelan, Adrian M.; Reid, Beth; Roe, Natalie A.; Ross, Ashley J.; Ross, Nicholas P.; Sabiu, Cristiano G.; Saito, Shun; Samushia, Lado; Sánchez, Ariel G.; Schlegel, David J.; Schneider, Donald P.; Scóccola, Claudia G.; Seo, Hee-Jong; Skibba, Ramin; Strauss, Michael A.; Swanson, M. E. C.; Thomas, Daniel; Tinker, Jeremy L.; Tojeiro, Rita; Magaña, Mariana Vargas; Verde, Licia; Wake, David A.; Weaver, B. A.; Weinberg, David H.; White, Martin; Xu, Xiaoying; Yèche, Ch; Zehavi, Idit; Zhao, Gong-Bo

doi:10.1093/mnras/stu523

Cited by 1,360 publications

(1,144 citation statements)

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“…The difference in bias between samples is greatest for the voids with larger radii. Note that this densest sample is comparable to the density of the CMASS (Anderson et al 2014) and LOWZ (Tojeiro et al 2014) galaxy samples of the Baryon Oscillation Spectroscopic Survey 5 (BOSS) (Alam et al 2015).…”

Section: Void Biasmentioning

confidence: 71%

Clustering and bias measurements of SDSS voids

Clampitt

Jain

Sánchez

2016

Mon. Not. R. Astron. Soc.

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Using a void catalog from the SDSS survey, we present the first measurements of void clustering and the corresponding void bias. Over the range 30 − 200 Mpc/h the void auto-correlation is detected at 5σ significance for voids of radius 15 − 20 Mpc/h. We also measure the void-galaxy cross-correlation at higher signal-to-noise and compare the inferred void bias with the autocorrelation results. Void bias is constant with scale for voids of a given size, but its value falls from 5.6 ± 1.0 to below zero as the void radius increases from 15 to 30 Mpc/h. The comparison of our measurements with carefully matched galaxy mock catalogs, with no free parameters related to the voids, shows that model predictions can be reliably made for void correlations. We study the dependence of void bias on tracer density and void size with a view to future applications. In combination with our previous lensing measurements of void mass profiles, these clustering measurements provide another step towards using voids as cosmological tracers.

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Section: Void Biasmentioning

confidence: 71%

Clustering and bias measurements of SDSS voids

Clampitt

Jain

Sánchez

2016

Mon. Not. R. Astron. Soc.

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“…In order to correct for several observational artifacts in the catalogues, the CMASS and LOWZ samples incorporate weights: a redshift failure weight, w rf , a fibre collision weight, w fc , and a systematic weight, wsys (CMASS only), which combines a seeing condition weight and a stellar weight (Ross et al 2012;Anderson et al 2014;Reid et al 2015). Hence, each galaxy target contributes to our estimate of the target galaxy density field by wc = wsys(w rf + w fc − 1).…”

Section: The Sdss III Boss Datamentioning

confidence: 99%

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the LOS-dependent power spectrum of DR12 BOSS galaxies

Gil-Marín¹,

Percival²,

Brownstein³

et al. 2016

Mon. Not. R. Astron. Soc.

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172

247

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We measure and analyse the clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) relative to the line-of-sight (LOS), for LOWZ and CMASS galaxy samples drawn from the final Data Release 12 (DR12). The LOWZ sample contains 361 762 galaxies with an effective redshift of z lowz = 0.32, and the CMASS sample 777 202 galaxies with an effective redshift of z cmass = 0.57. From the power spectrum monopole and quadrupole moments around the LOS, we measure the growth of structure parameter f times the amplitude of dark matter density fluctuations σ 8 by modeling the Redshift-Space Distortion signal. When the geometrical Alcock-Paczynski effect is also constrained from the same data, we find joint constraints on f σ 8 , the product of the Hubble constant and the comoving sound horizon at the baryon drag epoch H(z)r s (z d ), and the angular distance parameter divided by the sound horizon D A (z)/r s (z d ). We find f (z lowz )σ 8 (z lowz ) = 0.394 ± 0.062, D A (z lowz )/r s (z d ) = 6.35 ± 0.19, H(z lowz )r s (z d ) = (11.41 ± 0.56) 10 3 kms −1 for the LOWZ sample, and f (z cmass )σ 8 (z cmass ) = 0.444 ± 0.038, D A (z cmass )/r s (z d ) = 9.42 ± 0.15, H(z cmass )r s (z d ) = (13.92 ± 0.44) 10 3 kms −1 for the CMASS sample. We find general agreement with previous BOSS DR11 measurements. Assuming the Hubble parameter and angular distance parameter are fixed at fiducial ΛCDM values, we find f (z lowz )σ 8 (z lowz ) = 0.485 ± 0.044 and f (z cmass )σ 8 (z cmass ) = 0.436 ± 0.022 for the LOWZ and CMASS samples, respectively.

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“…We include three different incompleteness weights to account for shortcomings of the BOSS dataset (see Ross et al 2012 andAnderson et al 2014 for details): a redshift failure weight, w rf , a fibre collision weight, w fc and a systematics weight, wsys, which is a combination of a stellar density weight and a seeing condition weight. Each galaxy is thus counted as wc = (w rf + w fc − 1)wsys.…”

Section: The Boss Dr1datasetmentioning

confidence: 99%

Constraining the relative velocity effect using the Baryon Oscillation Spectroscopic Survey

Beutler

Seljak

Vlah

2017

Monthly Notices of the Royal Astronomical Society

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We analyse the power spectrum of the Baryon Oscillation Spectroscopic Survey (BOSS), Data Release 12 (DR12) to constrain the relative velocity effect, which represents a potential systematic for measurements of the Baryon Acoustic Oscillation (BAO) scale. The relative velocity effect is sourced by the different evolution of baryon and cold dark matter perturbations before decoupling. Our power spectrum model includes all 1-loop redshift-space terms corresponding to v bc parameterised by the bias parameter b v 2 . We also include the linear terms proportional to the relative density, δ bc , and relative velocity dispersion, θ bc , which we parameterise with the bias parameters b bc δ and b bc θ . Our data does not support a detection of the relative velocity effect in any of these parameters. Combining the low and high redshift bins of BOSS, we find limits of b v 2 = 0.012 ± 0.015 (±0.031), b bc δ = −1.0 ± 2.5 (±6.2) and b bc θ = −114 ± 55 (±175) with 68% (95%) confidence levels. These constraints restrict the potential systematic shift in D A (z), H(z) and f σ 8 , due to the relative velocity, to 1%, 0.8% and 2%, respectively. Given the current uncertainties on the BAO measurements of BOSS these shifts correspond to 0.53σ, 0.5σ and 0.22σ for D A (z), H(z) and f σ 8 , respectively.

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The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Data Releases 10 and 11 Galaxy samples

Cited by 1,360 publications

References 107 publications

Clustering and bias measurements of SDSS voids

Clustering and bias measurements of SDSS voids

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: RSD measurement from the LOS-dependent power spectrum of DR12 BOSS galaxies

Constraining the relative velocity effect using the Baryon Oscillation Spectroscopic Survey

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