The dependence of clustering on galaxy properties

By Cheng Li, G. Kauffmann, Yipeng Jing, Simon D. M. White, G. Börner, F. Cheng. 2005

219 citations recorded by the source corpus.

We use a sample of similar to 200 000 galaxies drawn from the Sloan Digital Sky Survey (SDSS) with 0.01 5 h(-1) Mpc). This large-scale clustering dependence is not seen for the parameters C or mu*. On small scales ( 1.5. In contrast, the dependence of the amplitude of wp(r(p)) on concentration on scales less than 1 h(-1) Mpc is strongest for disc-dominated galaxies with C < 2.6. This demonstrates that different processes are required to explain environmental trends in the structure and in the star formation history of galaxies.

Subfields: Astronomy and Astrophysics, Ecology, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/0eef0bc7cc948bed2f50a25bfb1db326c44cbd2c

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Citations in the corpus

Statistical analysis of galaxy surveys – I. Robust error estimation for two-point clustering statistics (2008, background): “…al. 2000), satisfies both of these requirements and can be divided into large subsamples to study clustering trends with galaxy properties (e.g. Norberg et al. 2001, 2002; Zehavi et al. 2002, 2004, 2005; Madgwick et al. 2003; Croton et al. 2004, 2007; Gaztañaga et al. 2005; Li et al. 2006, 2007).”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, methodology): “It is, in fact, possible to correct for fiber collisions down to scales as small as 0.01 h−1 Mpc using the ratio of small-angle pairs in the spectroscopic and photometric catalogs (Masjedi et al. 2006; Li et al. 2006; Li & White 2009), but we have not implemented this technique here.”
The clustering of intermediate-redshift quasars as measured by the Baryon Oscillation Spectroscopic Survey (2012, methodology): “The upweighting is derived by comparing the angular correlation function of all targets with c© 0000 RAS, MNRAS000, 000–000 that of the quasars for which we obtained redshifts (Hawkinset al. 2003; Li et al. 2006; Ross et al. 2007; White et al. 2011).”
Galaxy Groups in the SDSS DR4. I. The Catalog and Basic Properties (2007, methodology): “As shown in Li et al. (2006) these fits accurately capture the distribution of galaxies in the color-magnitude plane.”
The dark side of galaxy colour (2013, background): “The color dependence of galaxy location within the cosmic web also manifests in measurements of two-point statistics (e.g., Norberg et al. 2002; Zehavi et al. 2002, 2005; Li et al. 2006; Yang et al. 2011; Zehavi et al. 2011; Mostek et al. 2012).”
Interaction-induced star formation in a complete sample of 105 nearby star-forming galaxies (2007, methodology): “The right-hand panel shows the results after the two samples are matched in stellar mass with each other (This is important because massive galaxies are more clustered than less massive galaxies Li et al. 2006a).”
Galaxy Zoo: Disentangling the Environmental Dependence of Morphology and Colour ⋆ (2008, methodology): “In most galaxy clustering analyses, a galaxy catalogue is cut into subsamples based on the mark, and the two-point clustering in the subsample is studied by treating each galaxy in it equally (e.g., Norberg et al. 2002, Madgwick et al. 2003, Zehavi et al. 2005, Li et al. 2006, Tinker et al. 2008).”
The distribution of stellar mass in the low‐redshift Universe (2009, methodology): “(6) c© 2008 RAS, MNRAS 000, 1–12 Detailed tests of this procedure can be found in Li et al. (2006b).”
GALAXY GROUPS IN THE SDSS DR4. III. THE LUMINOSITY AND STELLAR MASS FUNCTIONS (2008, methodology): “…are separated into red and blue subsamples according to their bi-normal distribution in the 0.1(g−r) color (Baldry et al. 2004; Blanton et al. 2005a; Li et al. 2006), using the separation criteria (see Paper II), 0.1(g − r) = 1.022 − 0.0651x− 0.00311x2 , (1) where x = 0.1Mr − 5 logh + 23.0.”
Measures of Galaxy Environment I - What is "Environment"? (2011, background): “Some galaxy properties, such as luminosity, colour and stellar mass, are directly correlated with the large-scale environment through the host dark matter halo (e.g. Zehavi et al. 2005; Li et al. 2006).”
GALAXY CLUSTERING IN THE NEWFIRM MEDIUM BAND SURVEY: THE RELATIONSHIP BETWEEN STELLAR MASS AND DARK MATTER HALO MASS AT 1 < z < 2 (2010, background): “…such as luminosity, color, star formation rate, and morphology (Norberg et al. 2001, 2002; Zehavi et al. 2002; Budavári et al. 2003; Madgwick et al. 2003; Zehavi et al. 2005; Li et al. 2006; Swanson et al. 2008; Ross & Brunner 2009; Loh et al. 2010; Ross et al. 2010; Zehavi et al. 2010).”
MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, background): “…the fraction of blue satellites is lower than that observed, and the observed small-scale clustering of star-forming or blue galaxies tends to be poorly reproduced (see references above and Cooper et al. 2006, 2007; Park et al. 2007; Blanton & Berlind 2007; Li et al. 2006; Coil et al. 2008).”
THE CLUSTERING OF MASSIVE GALAXIES AT z ∼ 0.5 FROM THE FIRST SEMESTER OF BOSS DATA (2010, unknown): “The weight is derived by comparing the angular correlation function of the entire photometric sample with that of the galaxies for which we obtained redshifts (Hawkins et al. 2003; Li et al. 2006; Ross et al. 2007).”
The 2dF-SDSS LRG and QSO Survey: the LRG 2-point correlation function and redshift-space distortions (2006, methodology): “To correct for this effect, we use a similar method to Hawkins et al. (2003) and Li et al. (2006).”
EMERGE – an empirical model for the formation of galaxies since z ∼ 10 (2017, methodology): “Stellar masses in Li et al. (2006) and Guo et al. (2011) are computed following Kauffmann et al. (2003), while Yang et al. (2012) follow Bell et al. (2003).”