The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: the low-redshift sample

Parejko, John K.; Sunayama, Tomomi; Padmanabhan, Nikhil; Wake, David A.; Berlind, Andreas A.; Bizyaev, Dmitry; Blanton, Michael R.; Bolton, A.; Bosch, Frank van den; Brinkmann, J.; Brownstein, Joel R.; Costa, L. A. N. da; Eisenstein, Daniel J.; Guo, Hong; Kazin, Eyal; Maia, M. A. G.; Maraston, Claudia; McBride, Cameron K.; Nichol, R. C.; Oravetz, Daniel; Pan, Kaike; Percival, Will J.; Prada, Francisco; Ross, Ashley J.; Ross, Nicholas P.; Schlegel, David J.; Schneider, Donald P.; Simmons, Audrey; Skibba, Ramin; Tinker, Jeremy L.; Tojeiro, Rita; Weaver, B. A.; Wetzel, Andrew; White, Martin; Weinberg, David H.; Thomas, Daniel; Zehavi, Idit; Zheng, Zheng

doi:10.1093/mnras/sts314

Cited by 117 publications

(122 citation statements)

References 84 publications

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“…Our selection criteria in terms of the Sloan five-model magnitudes ugriz followed those given in Sect. 2 of Parejko et al (2013). With a total number of sources close to 600 000, this photometric sample contains a higher number density of galaxies in the southern part of the footprint than in the northern one (by more than 3%), which seems to be at odds with ΛCDM predictions.…”

Section: Sdss-lowzmentioning

confidence: 79%

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

134

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Based on cosmic microwave background (CMB) maps from the 2013 Planck Mission data release, this paper presents the detection of the integrated Sachs-Wolfe (ISW) effect, that is, the correlation between the CMB and large-scale evolving gravitational potentials. The significance of detection ranges from 2 to 4σ, depending on which method is used. We investigated three separate approaches, which essentially cover all previous studies, and also break new ground. (i) We correlated the CMB with the Planck reconstructed gravitational lensing potential (for the first time). This detection was made using the lensing-induced bispectrum between the low-and high-temperature anisotropies; the correlation between lensing and the ISW effect has a significance close to 2.5σ. (ii) We cross-correlated with tracers of large-scale structure, which yielded a significance of about 3σ, based on a combination of radio (NVSS) and optical (SDSS) data. (iii) We used aperture photometry on stacked CMB fields at the locations of known large-scale structures, which yielded and confirms a 4σ signal, over a broader spectral range, when using a previously explored catalogue, but shows strong discrepancies in amplitude and scale when compared with expectations. More recent catalogues give more moderate results that range from negligible to 2.5σ at most, but have a more consistent scale and amplitude, the latter being still slightly higher than what is expected from numerical simulations within ΛCMD. Where they can be compared, these measurements are compatible with previous work using data from WMAP, where these scales have been mapped to the limits of cosmic variance. Planck's broader frequency coverage allows for better foreground cleaning and confirms that the signal is achromatic, which makes it preferable for ISW detection. As a final step we used tracers of large-scale structure to filter the CMB data, from which we present maps of the ISW temperature perturbation. These results provide complementary and independent evidence for the existence of a dark energy component that governs the currently accelerated expansion of the Universe.

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Section: Sdss-lowzmentioning

confidence: 79%

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

Ade¹,

Aghanim²,

Armitage-Caplan³

et al. 2014

A&A

134

View full text Add to dashboard Cite

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“…HOD modeling has been used to interpret clustering in nearly all large-scale galaxy redshift surveys (e.g. Zheng et al 2007;Zheng et al 2009;Zehavi et al 2011;White et al 2011;Parejko et al 2013;Guo et al 2014). The HOD results provide physically informative and important information to test theories of galaxy formation and evolution.…”

Section: −1mentioning

confidence: 99%

“…Note that a FKP type radial weighting is not applied here, as it has no impact on the clustering at this scale (White et al 2011;Parejko et al 2013). We generate the random catalogs in the survey area which satisfies the completeness threshold, and assign a weight of 1 to all of these randoms.…”

Section: Clustering Measurementsmentioning

confidence: 99%

The Clustering of Luminous Red Galaxies at z ∼ 0.7 from EBOSS and BOSS Data

Zhai

Tinker

Hahn

et al. 2017

ApJ

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We present the first scientific results from the luminous red galaxy sample (LRG) of the extended Baryon Oscillation Spectroscopic Survey (eBOSS) combined with the high-redshift of the previous BOSS sample. We measure the small and intermediate scale clustering from a sample of more than 97,000 galaxies in the redshift range 0.6 < z < 0.9. We interpret these measurements in the framework of the Halo Occupation Distribution. The bias of this sample of LRGs is 2.30 ± 0.03, with a satellite fraction of 13 ± 3% and a mean halo mass of 2.5 × 10 13 h −1 M . These results are consistent with expectations, demonstrating that these LRGs will be reliable tracers of large scale structure at z ∼ 0.7. The galaxy bias implies a scatter of luminosity at fixed halo mass, σ log L , of 0.19 dex. Using the clustering of massive galaxies from BOSS-CMASS, BOSS-LOWZ, and SDSS, we find that σ log L = 0.19 is consistent with observations over the full redshift range that these samples cover. The addition of eBOSS to previous surveys allows investigation of the evolution of massive galaxies over the past ∼ 7 Gyr. Subject headings: large scale structure of universe

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“…Since LRGs are thought to be predominantly central galaxies (see e.g. Wake et al 2008;Zheng et al 2009;Parejko et al 2013), we set N s |M to zero and only fit for M mean and σ M in our nominal runs. We test the effect of this assumption on the derived quantities in the result sections by additionally fitting for M 1 .…”

Section: Halo Modelmentioning

confidence: 99%

Evolution of the luminosity-to-halo mass relation of LRGs from a combined analysis of SDSS-DR10+RCS2

Uitert¹,

Cacciato

Hoekstra

et al. 2015

A&A

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We study the evolution of the luminosity-to-halo mass relation of luminous red galaxies (LRGs). We selected a sample of 52 000 LOWZ and CMASS LRGs from the Baryon Oscillation Spectroscopic Survey (BOSS) SDSS-DR10 in the ∼450 deg 2 that overlaps with imaging data from the second Red-sequence Cluster Survey (RCS2), grouped them into bins of absolute magnitude and redshift and measured their weak-lensing signals. The source redshift distribution has a median of 0.7, which allowed us to study the lensing signal as a function of lens redshift. We interpreted the lensing signal using a halo model, from which we obtained the halo masses as well as the normalisations of the mass-concentration relations. The concentration of haloes that host LRGs is consistent with dark-matter-only simulations once we allow for miscentering or satellites in the modelling. The slope of the luminosity-to-halo mass relation has a typical value of 1.4 and does not change with redshift, but we find evidence for a change in amplitude: the average halo mass of LOWZ galaxies increases by 25 +16 −14 % between z = 0.36 and 0.22 to an average value of (6.43 ± 0.52) × 10 13 h −1 70 M . If we extend the redshift range using the CMASS galaxies and assume that they are the progenitors of the LOWZ sample, the average mass of LRGs increases by 80 +39 −28 % between z = 0.6 and 0.2.

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The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: the low-redshift sample

Cited by 117 publications

References 84 publications

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

Planck2013 results. XIX. The integrated Sachs-Wolfe effect

The Clustering of Luminous Red Galaxies at z ∼ 0.7 from EBOSS and BOSS Data

Evolution of the luminosity-to-halo mass relation of LRGs from a combined analysis of SDSS-DR10+RCS2

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