Towards a concordant model of halo occupation statistics

By F. V. D. Bosch, Xiaohu Yang, H. Mo, Simone M. Weinmann, A. Macciò, S. More, M. Cacciato, R. Skibba, X. Kang. 2006

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We use the conditional luminosity function (CLF) and data from the 2-degree Field Galaxy Redshift survey (2dFGRS) to constrain the average relation between light and mass in a Lambda cold dark matter (Lambda CDM) cosmology with Omega(m) = 0.23 and sigma(8) = 0.74 (hereafter WMAP3 cosmology). Reproducing the observed luminosity dependence of the galaxy two-point correlation function results in average mass-to-light ratios that are similar to 35 percent lower than those in a Lambda CDM cosmology with Omega(m), = 0.3 and sigma(8) = 0.9 (hereafter WMAP1 cosmology). This removes an important problem with previous halo occupation models which had a tendency to predict cluster mass-to-light ratios that were too high. For the WMAP3 cosmology, our model yields average mass-to-light ratios, central galaxy luminosities, halo occupation numbers, satellite fractions and luminosity-gap statistics, that are all in excellent agreement with those obtained from a 2dFGRS group catalogue and from other independent studies. We also use our CLF model to compute the probability distribution P(M vertical bar L-cen), that a central galaxy of luminosity L-cen resides in a halo of mass M. We find this distribution to be much broader than what is typically assumed in halo occupation distribution models, which has important implications for the interpretation of satellite kinematics and galaxy-galaxy lensing data. Finally, reproducing the luminosity dependence of the pairwise peculiar velocity dispersions in the 2dFGRS requires relatively low mass-to-light ratios for clusters and a satellite fraction that decreases strongly with increasing luminosity. This is only marginally consistent with the constraints obtained from the luminosity dependence of the galaxy two-point correlation function. We argue that a cosmology with parameters between those of the WMAP1 and WMAP3 cosmologies is likely to yield results with a higher level of consistency.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/5424f26cf68afd0b959a3a4cf6a4d95af1d09dbd

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Citations in the corpus

CANDELS: THE COSMIC ASSEMBLY NEAR-INFRARED DEEP EXTRAGALACTIC LEGACY SURVEY (2011, unknown): “…is done by taking advantage of our excellent understanding of the clustering properties of dark matter halos, and adopting a prescription to populate halos with galaxies (often called “Halo Occupation Distribution” or “Conditional Luminosity Function” formalism (e.g., van den Bosch et al. 2007).”
There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, background): “These results led the authors to conclude that the frequency of mergers may present a substantial challenge to our understanding of disk galaxy stability, as the majority of galaxies in MWmass halos are disk-dominated (Weinmann et al. 2006; van den Bosch et al. 2007; Park et al. 2007)).”
Merger Histories of Galaxy Halos and Implications for Disk Survival (2007, background): “As mentioned in the introduction, broad-brush categorizations of “late type” vs. “early type” suggest that ∼ 70% of Milky Way-sized halos host late-type galaxies (e.g. Weinmann et al. 2006; van den Bosch et al. 2007; Ilbert et al. 2006; Choi et al. 2007; Park et al. 2007).”
What determines satellite galaxy disruption (2009, result): “Similarly, van den Bosch et al. (2007) find a lower limit of 0.2 dex scatter in halo mass at fixed luminosity from conditional luminosity function modeling, consistent with the results of More et al. (2009) from satellite kinematics.”
NEW CONSTRAINTS ON THE EVOLUTION OF THE STELLAR-TO-DARK MATTER CONNECTION: A COMBINED ANALYSIS OF GALAXY–GALAXY LENSING, CLUSTERING, AND STELLAR MASS FUNCTIONS FROM z = 0.2 to z = 1 (2011, background): “Previous HOD analyses of clustering results at varying redshifts also vary little from a value of unity (Zehavi et al. 2005, 2011b; Zheng et al. 2007; van den Bosch et al. 2007; Tinker et al. 2007).”
MERGERS AND BULGE FORMATION IN ΛCDM: WHICH MERGERS MATTER? (2009, background): “…in low-mass systems from rotation curve fitting (see e.g. Persic & Salucci 1988; Persic et al. 1996; Borriello & Salucci 2001; Avila-Reese et al. 2008), or in high-mass systems from X-ray gas or group kinematics (Eke et al. 2004; Yang et al. 2005; Brough et al. 2006; van den Bosch et al. 2007).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. I. Galaxy Mergers and Quasar Activity (2007, methodology): “…we populate subhalos according to an empirical halo occupation model (e.g., Tinker et al. 2005; Conroy et al. 2006; Vale & Ostriker 2006; van den Bosch et al. 2007; Wang et al. 2006)—i.e., matching the observed statistics of where galaxies of a given type live (accounting for different…”
Galaxy clustering and galaxy-galaxy lensing: a promising union to constrain cosmological parameters (2008, methodology): “3, are similar, though slightly higher, than for the WMAP3 cosmology, in excellent agreement with van den Bosch et al. (2007).”
Galaxy assembly bias: a significant source of systematic error in the galaxy–halo relationship (2013, methodology): “…completed SDSS galaxy clustering analysis of Zehavi et al. (2011) as well as Zehavi et al. (2005),Yang et al. (2005), Zheng et al. (2007), van den Bosch et al. (2007), Zheng et al. (2009), Simon et al. (2009), Abbas et al. (2010), Ross et al. (2010), Watson et al. (2010), Matsuoka et al. (2011),…”
Cosmological constraints from the clustering of the Sloan Digital Sky Survey DR7 luminous red galaxies (vol 404, pg 60, 2010) (2009, background): “In some of these cases, both the first and second brightest galaxies would be identified as LRGs; van den Bosch et al. (2007) showed that the luminosity difference between first and second brightest galaxies in massive groups is typically small.”
MERGERS IN ΛCDM: UNCERTAINTIES IN THEORETICAL PREDICTIONS AND INTERPRETATIONS OF THE MERGER RATE (2010, background): “…masses of massive groups and clusters from e.g. X-ray gas and group kinematics, as a function of central galaxy mass in massive brightest group or brightest cluster galaxies (BGGs/BCGs; see Eke et al. 2004; Yang et al. 2005a; Brough et al. 2006; van den Bosch et al. 2007, and references therein).”
THE IMPACT OF COLD GAS ACCRETION ABOVE A MASS FLOOR ON GALAXY SCALING RELATIONS (2009, background): “…fraction in galaxies is a strong function of the total halo mass (e.g. van den Bosch et al. 2003b; Eke et al. 2005; Shankar et al. 2006; van den Bosch et al. 2007; Kravtsov 2010; Moster et al. 2010; Guo et al. 2010) owing to the very different shapes of the halo mass function and the galaxy…”
GALAXY GROUPS IN THE SDSS DR4. III. THE LUMINOSITY AND STELLAR MASS FUNCTIONS (2008, methodology): “…with those obtained from the clustering properties of galaxies using the CLF and HOD formalism (Yang et al. 2003; Tinker et al 2005; van den Bosch et al. 2007; Cacciato et al. 2008), and at the relative massive end with those obtained from weak lensing observations (e.g. Sheldon et al.…”
THE PSEUDO-EVOLUTION OF HALO MASS (2012, background): “…of galaxies and their clustering (Yang et al. 2003; Zehavi et al. 2004; Tinker et al. 2005; Zehavi et al. 2005; Skibba et al. 2006; van den Bosch et al. 2007; Brown et al. 2008; Conroy & Wechsler 2009; Moster et al. 2010, 2013; Behroozi et al. 2010; Yang et al. 2012), or a combination of…”