The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: modelling of the luminosity and colour dependence in the Data Release 10

Guo, Hong; Zheng, Zheng; Zehavi, Idit; Xu, Haojie; Eisenstein, Daniel J.; Weinberg, David H.; Bahcall, Neta A.; Berlind, Andreas A.; Comparat, Johan; McBride, Cameron K.; Ross, Ashley J.; Schneider, Donald P.; Skibba, Ramin; Swanson, M. E. C.; Tinker, Jeremy L.; Tojeiro, Rita; Wake, David A.

doi:10.1093/mnras/stu763

Cited by 89 publications

(110 citation statements)

References 110 publications

(168 reference statements)

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“…Besides the halo mass difference, on small scales there may also be contributions from the difference in the satellite fraction of red and blue CMASS galaxies. Guo et al (2014) require a fraction of the galaxies to be satellites in massive halos in order to explain strong small-scale clustering. Guo et al (2013Guo et al ( , 2014 conducted similar studies to ours, using the same spectroscopic data set (CMASS) and redshift range, but using auto-correlation rather than cross-correlation with a photometric sample.…”

Section: Strategymentioning

confidence: 99%

“…Guo et al (2014) require a fraction of the galaxies to be satellites in massive halos in order to explain strong small-scale clustering. Guo et al (2013Guo et al ( , 2014 conducted similar studies to ours, using the same spectroscopic data set (CMASS) and redshift range, but using auto-correlation rather than cross-correlation with a photometric sample. Their analysis considered luminosity and color rather than stellar mass and color, and used an r − i rather than g − i color definition, so we cannot make an exact comparison.…”

Section: Strategymentioning

confidence: 99%

“…In selecting intermediate redshifts of 0.6 < z < 0.65, we can further quantify how the relationship between clustering and properties evolves over time. This work can also be compared with recent efforts using the same data sets and redshift range (Guo et al 2013(Guo et al , 2014), as we use a different method (crosscorrelation rather than auto-correlation).…”

Section: Introductionmentioning

confidence: 99%

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The Color and Stellar Mass Dependence of Small-scale Galaxy Clustering in SDSS-III BOSS

Law-Smith

Eisenstein

2017

ApJ

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We measure the color and stellar mass dependence of clustering in spectroscopic galaxies at 0.6 < z < 0.65 using data from the Baryon Oscillation Spectroscopic Survey component of the Sloan Digital Sky Survey. We greatly increase the statistical precision of our clustering measurements by using the cross-correlation of 66,657 spectroscopic galaxies to a sample of 6.6 million fainter photometric galaxies. The clustering amplitude w(R) is measured as the ratio of the mean excess number of photometric galaxies found within a specified radius annulus around a spectroscopic galaxy to that from a random photometric galaxy distribution. We recover many of the familiar trends at high signal-to-noise ratio. We find the ratio of the clustering amplitudes of red and blue massive galaxies to be w red /w blue = 1.92 ± 0.11 in our smallest annulus of 75-125 kpc. At our largest radii (2-4 Mpc), we find w red /w blue = 1.24 ± 0.05. Red galaxies therefore have denser environments than their blue counterparts at z ∼ 0.625, and this effect increases with decreasing radius. Irrespective of color, we find that w(R) does not obey a simple power-law relation with radius, showing a dip around 1 Mpc. Holding stellar mass fixed, we find a clear differentiation between clustering in red and blue galaxies, showing that clustering is not solely determined by stellar mass. Holding color fixed, we find that clustering increases with stellar mass, especially for red galaxies at small scales (more than a factor of 2 effect over 0.75 dex in stellar mass).

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Section: Strategymentioning

confidence: 99%

Section: Strategymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Color and Stellar Mass Dependence of Small-scale Galaxy Clustering in SDSS-III BOSS

Law-Smith

Eisenstein

2017

ApJ

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“…A possible exception to the trade-off between large area and high redshift is the work of Guo et al (2014); here, the authors used the CMASS sample of SDSS to show that clustering was stronger for brighter and redder galaxies at z ∼ 0.5. However, the complicated selection of the CMASS sample limits their work to a very narrow luminosity and redshift range.…”

mentioning

confidence: 98%

Galaxy and mass assembly (GAMA): projected galaxy clustering

Farrow

Cole

Norberg

et al. 2015

Mon. Not. R. Astron. Soc.

137

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We measure the projected 2-point correlation function of galaxies in the 180 deg 2 equatorial regions of the GAMA II survey, for four different redshift slices between z = 0.0 and z = 0.5. To do this we further develop the Cole (2011) method of producing suitable random catalogues for the calculation of correlation functions. We find that more r-band luminous, more massive and redder galaxies are more clustered. We also find that red galaxies have stronger clustering on scales less than ∼ 3 h −1 Mpc. We compare to two different versions of the GALFORM galaxy formation model, Lacey et al (in prep.) and Gonzalez-Perez et al. (2014), and find that the models reproduce the trend of stronger clustering for more massive galaxies. However, the models under predict the clustering of blue galaxies, can incorrectly predict the correlation function on small scales and under predict the clustering in our sample of galaxies with ∼ 3L * r . We suggest possible avenues to explore to improve these clustering predictions. The measurements presented in this paper can be used to test other galaxy formation models, and we make the measurements available online to facilitate this.

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“…A generalized NFW profile is adopted, with the concentration parameter c and inner slope γ as two additional free parameters (e.g. Watson et al 2010Watson et al , 2012van den Bosch et al 2013;Guo et al 2014),…”

Section: Modeling Resultsmentioning

confidence: 99%

On the clustering of faint red galaxies

Zheng

Guo

et al. 2016

Mon. Not. R. Astron. Soc.

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Faint red galaxies in the Sloan Digital Sky Survey show a puzzling clustering pattern in previous measurements. In the two-point correlation function (2PCF), they appear to be strongly clustered on small-scales, indicating a tendency to reside in massive haloes as satellite galaxies. However, their weak clustering on large scales suggests that they are more likely to be found in low mass haloes. The interpretation of the clustering pattern suffers from the large sample variance in the 2PCF measurements, given the small volume of the volume-limited sample of such faint galaxies. We present improved clustering measurements of faint galaxies by making a full use of a flux-limited sample to obtain volume-limited measurements with an increased effective volume. In the improved 2PCF measurements, the fractional uncertainties on large-scales drop by more than 40 per cent, and the strong contrast between small-scale and large-scale clustering amplitudes seen in previous work is no longer prominent. From halo occupation distribution modelling of the measurements, we find that a considerable fraction of faint red galaxies to be satellites in massive haloes, a senario supported by the strong covariance of small-scale 2PCF measurements and the relative spatial distribution of faint red galaxies and luminous galaxies. However, the satellite fraction is found to be degenerate with the slope of the distribution profile of satellites in inner haloes. We compare the modelling results with semi-analytic model predictions and discuss the implications.

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The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: modelling of the luminosity and colour dependence in the Data Release 10

Cited by 89 publications

References 110 publications

The Color and Stellar Mass Dependence of Small-scale Galaxy Clustering in SDSS-III BOSS

The Color and Stellar Mass Dependence of Small-scale Galaxy Clustering in SDSS-III BOSS

Galaxy and mass assembly (GAMA): projected galaxy clustering

On the clustering of faint red galaxies

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