The dependence of clustering on galaxy properties

Li, Cheng; Kauffmann, Guinevere; Jing, Y. P.; White, Simon D. M.; Börner, G.; Cheng, F. Z.

doi:10.1111/j.1365-2966.2006.10066.x

Cited by 294 publications

(509 citation statements)

References 63 publications

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“…In particular, it has been found that more luminous and massive galaxies are more strongly clustered than fainter and less massive ones (Davis & Geller 1976;Davis et al 1988;Hamilton 1988;Loveday et al 1995;Benoist et al 1996;Guzzo et al 1997Guzzo et al , 2000Norberg et al 2001Norberg et al , 2002Zehavi et al 2002Zehavi et al , 2005Zehavi et al , 2011Brown et al 2003;Abbas & Sheth 2006;Li et al 2006;Swanson et al 2008;Ross et al 2011;Guo et al 2013;Marulli et al 2013); similar trends have been found also as a function of morphology and colours, for which galaxies with a rounder shape and redder show an enhanced clustering. The 2PCF is also often used to provide constraints on galaxy bias b, which quantifies the excess in clustering of the selected sample with respect to the underlying dark matter; however, these estimates have to assume a fiducial cosmology, and are degenerate with the amplitude of linear matter density fluctuations quantified at 8 h −1 Mpc , σ 8 , of the assumed model.…”

Section: Introductionsupporting

confidence: 53%

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Moresco

Marulli

Moscardini

et al. 2017

A&A

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Aims. The three-point correlation function (3PCF) is a powerful probe to investigate the clustering of matter in the Universe in a complementary way with respect to lower-order statistics, providing additional information with respect to the two-point correlation function and allowing us to shed light on biasing, nonlinear processes, and deviations from Gaussian statistics. In this paper, we analyse the first data release of the VIMOS Public Extragalactic Redshift Survey (VIPERS), determining the dependence of the three-point correlation function on luminosity and stellar mass at z = [0.5, 1.1]. Methods. We exploit the VIPERS Public Data Release 1, consisting of more than 50,000 galaxies with B-band magnitudes in the range −21.6 M B − 5 log(h) −19.9 and stellar masses in the range 9.8 log(M ⋆ [h −2 M ⊙ ]) 10.7. We measure both the connected 3PCF and the reduced 3PCF in redshift space, probing different configurations and scales, in the range 2.5 < r [h −1 Mpc ]< 20. Results. We find a significant dependence of the reduced 3PCF on scales and triangle shapes, with stronger anisotropy at larger scales (r ∼ 10 h −1 Mpc ) and an almost flat trend at smaller scales, r ∼ 2.5 h −1 Mpc . Massive and luminous galaxies present a larger connected 3PCF, while the reduced 3PCF is remarkably insensitive to magnitude and stellar masses in the range we explored. These trends, already observed at low redshifts, are confirmed for the first time to be still valid up to z = 1.1, providing support to the hierarchical scenario for which massive and bright systems are expected to be more clustered. The possibility of using the measured 3PCF to provide independent constraints on the linear galaxy bias b has also been explored, showing promising results in agreement with other probes.

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Section: Introductionsupporting

confidence: 53%

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

Moresco

Marulli

Moscardini

et al. 2017

A&A

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“…The dependence of galaxy clustering as a function of various intrinsic galaxy properties has been well determined by observations(e.g, Norberg et al 2002;Li et al 2006;Farrow et al 2015;Shi et al 2016). However, in galaxy formation models it is still difficult to reproduce the amplitude of correlation functions for low mass galaxies and on small scales (Guo et al 2011;Wang et al 2012;Campbell et al 2015).…”

Section: Galaxy Correlation Functionmentioning

confidence: 95%

“…Error bars are from bootstrapping simulation data (Barrow et al 1984). The circles with error bars show the SDSS DR7 results (Li et al 2006;Guo et al 2011). 2013; Gonzalez-Perez et al 2014). This reduces the inferred abundance at both low and high stellar masses, and smooths the bump near the "knee" of the function.…”

Section: Present Day Stellar Mass and Luminosity Functionsmentioning

confidence: 99%

The galaxy population in cold and warm dark matter cosmologies

Wang

González-Pérez²,

Xie

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We use a pair of high resolution N-body simulations implementing two dark matter models, namely the standard cold dark matter (CDM) cosmogony and a warm dark matter (WDM) alternative where the dark matter particle is a 1.5 keV thermal relic. We combine these simulations with the GALFORM semi-analytical galaxy formation model in order to explore differences between the resulting galaxy populations. We use GALFORM model variants for CDM and WDM that result in the same z = 0 galaxy stellar mass function by construction. We find that most of the studied galaxy properties have the same values in these two models, indicating that both dark matter scenarios match current observational data equally well. Even in under-dense regions, where discrepancies in structure formation between CDM and WDM are expected to be most pronounced, the galaxy properties are only slightly different. The only significant difference in the local universe we find is in the galaxy populations of "Local Volumes", regions of radius 1 to 8Mpc around simulated Milky Way analogues. In such regions our WDM model provides a better match to observed local galaxy number counts and is five times more likely than the CDM model to predict subregions within them that are as empty as the observed Local Void. Thus, a highly complete census of the Local Volume and future surveys of void regions could provide constraints on the nature of dark matter.

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“…For example, first taking the spectroscopic based work, Li et al (2006) presented the measured mass dependence of galaxy clustering at z < 0.3 using SDSS data, showing an increase in clustering with mass, which became more pronounced above M * . Moving to higher redshifts, Meneux et al (2008Meneux et al ( , 2009) measured the clustering of mass-selected samples in the VVDS-Deep and zCOSMOS Surveys respectively, finding a clustering mass dependence in their results at redshifts up to z ≈ 1.2.…”

Section: Introductionmentioning

confidence: 99%

The WIRCam Deep Survey

Bielby

González-Pérez

McCracken

et al. 2014

A&A

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We present an analysis of the clustering of galaxies from z ≈ 2 to the present day using the WIRCam Deep Survey (WIRDS). WIRDS combines deep optical data from the CFHTLS Deep fields with its own deep near-infrared data, providing a photometric data-set over an effective area of 2.4 deg 2 , from which accurate photometric redshifts and stellar masses can be estimated. We use the data to calculate the angular correlation function for galaxy samples split by star-formation activity, stellar mass and redshift. Using WIRDS with its large total area and multiple fields gives a low cosmic variance contribution to the error, which we estimate to be less than ∼2.8%. Based on power-law fits, we estimate the real-space clustering for each sample, determining clustering lengths and power-law slopes. For galaxies selected by constant mass, we find that the clustering scale shows no evolution up to z ≈ 2. Splitting the galaxy sample by mass, we see a consistent trend for higher mass galaxies to have larger clustering scales at all redshifts considered. We use our results to test the galform semi-analytical model of galaxy formation and evolution. The observed trends are well matched by the model galaxies for both the redshift evolution and the mass dependence of the galaxy clustering. We split the galaxy population into passive and star-forming populations based on rest-frame dust-corrected NUV-r colours. We find that the passive galaxy populations show a significantly larger clustering scale at all redshifts than the star-forming population below masses of M ∼ 10 11 h −1 M , showing that even at z ≈ 2 passive galaxies exist in denser environments than the bulk of the star-forming galaxy population. For star-forming galaxies with stellar masses of M 10 11 h −1 M , we find a clustering strength of ∼8 h −1 Mpc across all redshifts, comparable to the measurements for the passive population. Additionally, for star-forming galaxies we see that clustering strength increases for higher stellar mass systems, however little sign of a mass dependence in passive galaxies is observed over the range in stellar mass that is probed. Comparing our results to the model galaxy population produced by galform, we find a qualitative good agreement between the model predictions and the observed clustering. Finally, we investigate the connection between galaxy stellar mass and dark matter halo mass, showing a clear correlation between the two in both the WIRDS data and the galform predictions.

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The dependence of clustering on galaxy properties

Cited by 294 publications

References 63 publications

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

The VIMOS Public Extragalactic Redshift Survey (VIPERS)

The galaxy population in cold and warm dark matter cosmologies

The WIRCam Deep Survey

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