Galaxy Groups in the SDSS DR4. II. Halo Occupation Statistics

By Xiaohu Yang, H. Mo, F. V. D. Bosch. 2007

269 citations recorded by the source corpus.

We investigate various galaxy occupation statistics of dark matter halos using a large galaxy group catalog constructed from the Sloan Digital Sky Survey Data Release 4 (SDSS DR4) with an adaptive halo-based group finder. The conditional luminosity function (CLF) is measured separately for all, red, and blue galaxies, as well as in terms of central and satellite galaxies. The CLFs for central and satellite galaxies can be well modeled with a lognormal distribution and a modified Schechter form, respectively. About 85% of the central galaxies and about 80% of the satellite galaxies in halos with masses Mh≳ 1014 h−1 M☉ are red galaxies. These numbers decrease to 50% and 40%, respectively, in halos with Mh ∼ 1012 h−1 M☉. For halos of a given mass, the distribution of the luminosities of central galaxies, Lc, has a dispersion of about 0.15 dex. The mean luminosity (stellar mass) of the central galaxies scales with halo mass as Lc ∝ Mh0.17 (M*,c ∝ Mh0.22) for halos with masses M ≫ 1012.5 h−1 M☉, and both relations are significantly steeper for less massive halos. We also measure the luminosity and stellar mass gaps between the first and second brightest (most massive) member galaxies, log L1 − log L2 (log M*,1 − log M*,2). These gap statistics, especially in halos with Mh≲ 1014.0 h−1 M☉, indicate that the luminosities of central galaxies are clearly distinct from those of their satellites. The fraction of fossil groups, defined as those groups with log L1 − log L2 ⩾ 0.8, ranges from ~2.5% for groups with Mh ∼ 1014 h−1 M☉ to 18%-60% for groups with Mh ∼ 1013 h−1 M☉. Finally, we measure the fraction of satellites, which changes from ~5.0% for galaxies with 0.1Mr − 5 log h ∼ − 22.0 to ~40% for galaxies with 0.1Mr − 5 log h ∼ − 17.0.

Subfields: Astronomy and Astrophysics, Computer Vision and Pattern Recognition, Ecology

View Paper: https://www.semanticscholar.org/paper/260cdcc3d4eb1e7310e7192baa5d2aefb81b1909

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. C. Conroy
4. R. Somerville
5. F. V. D. Bosch
6. R. Dav'e
7. A. Dekel
8. Volker Springel

In Computer Vision and Pattern Recognition

1. F. V. D. Bosch
2. Xiaohu Yang
3. H. Mo
4. S. More
5. Andrew Wetzel
6. P. Hopkins
7. M. Cacciato
8. R. Somerville

In Ecology

1. F. V. D. Bosch
2. Xiaohu Yang
3. H. Mo
4. S. More
5. Andrew Wetzel
6. M. White
7. R. Skibba
8. L. Hernquist

Citations in the corpus

• What determines satellite galaxy disruption (2009, methodology): “Tinker et al. (2007) used a similar technique applied to 2dFGRS. Additionally, Yang et al. (2008) satellite fractions were obtained directly from the SDSS group catalogs of Yang et al. (2007).”
• THE CONNECTION BETWEEN GALAXIES AND DARK MATTER STRUCTURES IN THE LOCAL UNIVERSE (2012, methodology): “Unlike in Yang et al. (2008, 2009), we choose not to fix the relationship betweenM∗,c andM∗,s explicitly.”
• EVOLUTION OF THE GALAXY–DARK MATTER CONNECTION AND THE ASSEMBLY OF GALAXIES IN DARK MATTER HALOS (2011, methodology): “The stellar mass to halo mass ratio has a minimum for halos of ∼ 1012 h−1M⊙, and increases rapidly towards both lower and higher halo masses (Yang et al. 2003, 2005b, 2008, 2009b; van den Bosch et al. 2003a; Tinker et al. 2005; Leauthaud et al. 2012), suggesting that galaxy formation is most…”
• Are Brightest Halo Galaxies Central Galaxies (2010, methodology): “Motivated by the CLF inferred from the SDSS group catalogue by Yang et al. (2008), C09 adopted Q = 0.562, with no dependence on halo mass.”
• Cosmological Constraints from a Combination of Galaxy Clustering and Lensing -- III. Application to SDSS Data (2012, methodology): “Note that neither of these functional forms has a physical motivation; they merely were found to adequately describe the results obtained by Yang et al. (2008) from the SDSS galaxy group catalog.”
• GALAXY CLUSTERING IN THE NEWFIRM MEDIUM BAND SURVEY: THE RELATIONSHIP BETWEEN STELLAR MASS AND DARK MATTER HALO MASS AT 1 < z < 2 (2010, background): “Both fits show a general trend of decreasing satellite fraction with increasing stellar mass limit, a trend which has previously been seen in clustering measurements, group catalogs and from lensing at z < 1 (e.g. Zehavi et al. 2005; Zheng et al. 2007; Mandelbaum et al. 2006; Yang et al. 2008).”
• MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, methodology): “The observational results are taken from Kimm et al. (2009), from their analysis of the Yang et al. (2005b, 2008) SDSS (z = 0) galaxy catalogs, with the passive population identified by the observed bimodal distribution of specific star formation rates at each mass.”
• GALAXY CLUSTERS IDENTIFIED FROM THE SDSS DR6 AND THEIR PROPERTIES (2009, methodology): “According the halo occupation distribution obtained by Yang et al. (2008), we derive the number of the galaxies of0.”
• THE BARYON CONTENT OF COSMIC STRUCTURES (2009, result): “This is broadly consistent with previous results based on counting statistics (Yang et al. 2008).”
• Galaxy evolution in groups and clusters: satellite star formation histories and quenching time-scales in a hierarchical Universe (2012, result): “While SHAM in its simplest implementation assumes a one-to-one correspondence between Mmax and Mstar, a scatter of 0.15 − 0.2 dex in this relation is suggested by observations (e.g., Zheng et al. 2007; Yang et al. 2008; More et al. 2009; Wetzel & White 2010; Leauthaud et al. 2012).”
• Environmental effects on satellite galaxies: the link between concentration, size and colour profile (2008, methodology): “The MGRS is constructed by populating dark matter haloes in numerical simulations of cosmological volumes with galaxies according to the conditional luminosity function (CLF) as described in Cacciato et al. (2008) and Yang et al. (2008).”
• A CATALOG OF GLOBULAR CLUSTER SYSTEMS: WHAT DETERMINES THE SIZE OF A GALAXY'S GLOBULAR CLUSTER POPULATION? (2013, methodology): “A flexible and simpler conversion relation from Yang et al. (2008) and also used by S09 is M⋆ = M0 (Mhalo/M1) α+β (1 +Mhalo/M1)β .”
• Satellite kinematics – II. The halo mass–luminosity relation of central galaxies in SDSS (2008, methodology): “This parametrization is motivated by the results of Yang et al. (2008) who measure the CLF from the SDSS group catalogue described in Yang et al. (2007).”
• Physical properties and environments of nearby galaxies (2009, background): “HST imaging and optical spectroscopy by Yang et al. (2008) suggests that currently they are discrepant from the fundamental plane of ellipticals — that is, they are consistent with having the lower mass-to-light ratios appropriate to their young stellar populations, and may fade onto the…”
• GALAXY GROUPS IN THE SDSS DR4. III. THE LUMINOSITY AND STELLAR MASS FUNCTIONS (2008, methodology): “…the galaxy - dark halo connection (e.g. HOD/CLF models) is to use galaxy groups as a representation of dark matter halos and to study how the galaxy population changes with the properties of the groups (e.g., Y05c; Zandivarez et al. 2006; Robotham et al. 2006; Hansen et al. 2007; Yang et al. 2008).”
• Dependence of galaxy quenching on halo mass and distance from its centre (2012, background): “Yang et al. (2008) find that galaxies above Mh ∼ 10 12.5 follow a very weak scaling of M∗ ∝ M 0.22 h while below this mass, M∗ scales more steeply with Mh, scaling as M∗ ∝ M 1.83 h for galaxies well below Mh ∼ 10 12.5M⊙ (Yang et al. 2008).”
• THE VELOCITY WIDTH FUNCTION OF GALAXIES FROM THE 40% ALFALFA SURVEY: SHEDDING LIGHT ON THE COLD DARK MATTER OVERABUNDANCE PROBLEM (2011, background): “30% underestimate of the abundance of low-width galaxies by ALFALFA (e.g Yang et al. 2008; Klypin et al. 2010), not nearly enough to explain the observed discrepancies.”