Linking early‐ and late‐type galaxies to their dark matter haloes

By F. V. D. Bosch, Xiaohu Yang, H. Mo. 2002

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Using data from the 2 Degree Field Galaxy Redshift Survey (2dFGRS) we compute the conditional luminosity functions (CLFs) of early- and late-type galaxies. These functions give the average number of galaxies with luminosities in the range L ′ dL/2 that reside in a halo of mass M, and are a powerful statistical tool to link the distribution of galaxies to that of dark matter haloes. Although some amount of degeneracy remains, the CLFs are well constrained. They indicate that the average mass-to-light ratios of dark matter haloes have a minimum of ∼100 h(M/L) O . around a halo mass of ∼3 x 10 1 1 h - 1 M O .. Towards lower masses (M/L) increases rapidly, and matching the faint-end slope of the observed luminosity function (LF) requires that haloes with M < 10 1 0 h - 1 M O . are virtually devoid of galaxies. At the high-mass end, the observed clustering properties of galaxies require that clusters have b J -band mass-to-light ratios in the range 500-1000 h (M/L) O .. Finally, the fact that early-type galaxies are more strongly clustered than late-type galaxies requires that the fraction of late-type galaxies is a strongly declining function of halo mass. We compute two-point correlation functions as a function of both luminosity and galaxy type. The agreement with observations, in terms of normalization and power-law slope, is remarkably good. When including predictions for the correlation functions of faint galaxies we find a weak (strong) luminosity dependence for the late- (early-) type galaxies. We also investigate the inferred halo occupation numbers. Late-type and faint galaxies reveal a shallower (N)(M) than bright, early-type galaxies, which explains why (N)(M) transforms from a single power law for bright galaxies to a more complicated form when fainter galaxies are included. Finally, we compare our CLFs with predictions from several semi-analytical models for galaxy formation. As long as these models accurately fit the 2dFGRS luminosity function the agreement with our predictions is remarkably good. This indicates that the technique used here has recovered a statistical description of how galaxies populate dark matter haloes, which is not only in perfect agreement with the data, but which in addition fits nicely within the standard framework for galaxy formation.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/75dfdd263885d446b714a2dc45dc5550b20258e4

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Citations in the corpus

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): “…Φ(L|Mh)dL which specifies the average number of galaxies of luminosity L ± dL/2 that reside in a halo of mass Mh (e.g., Yang et al. 2003; van den Bosch et al. 2003, 2007; Vale & Ostriker 2004, 2008; Cooray 2006) and the conditional stellar mass function (SMF) Φ(M∗|Mh)dM∗ which yields the…”
Towards a concordant model of halo occupation statistics (2006, methodology): “…2005b, 2006), to study the environment dependence of the galaxy luminosity function (Mo et al. 2004), to constrain cosmological parameters (van den Bosch et al. 2003b; Tinker et al. 2005), to study the pairwise peculiar velocity dispersion (PVD) of galaxies (Jing & Börner 2004; Yang et al. 2004;…”
Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, methodology): “This method was first used by van den Bosch et al. (2003b) and Tinker et al. (2005), who were able to obtain relatively tight constraints on Ωm and σ8 from combinations of clustering data plus constraints on the mass-to-light ratios of clusters.”
Red Galaxy Growth and the Halo Occupation Distribution (2008, background): “…& Mohr 2004), X-ray luminosity (e.g., Brough et al. 2008), group velocity dispersion (e.g., Brough et al. 2006), galaxy clustering (e.g., van den Bosch et al. 2003; Zheng et al. 2007), and matching the galaxy luminosity function with the predicted halo mass function (e.g., Vale & Ostriker 2004).”
The Luminosity and Color Dependence of the Galaxy Correlation Function (2004, methodology): “…been applied to interpret clustering data from a number of surveys at low and high redshift (e.g., Jing & Börner 1998; Jing et al. 2002; Bullock et al. 2002; Moustakas & Somerville 2002; van den Bosch et al. 2003b; Magliocchetti & Porciani 2003; Yan et al. 2003; Zheng 2004; Porciani et al. 2004).”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, background): “…of surveys at low and high redshifts (e.g., Jing & Börner 1998; Jing, Börner, & Suto 2002; Bullock et al. 2002; Moustakas & Somerville 2002; van den Bosch et al. 2003a; Magliocchetti & Porciani 2003; Yan, Madgwick, & White 2003; Zheng 2004; Yang et al. 2005b; Zehavi et al. 2005b; Cooray 2006;…”
Radiative feedback and the low efficiency of galaxy formation in low-mass haloes at high redshift (2013, background): “This ratio is a strong function of the virial mass and it decreases strongly at intermediate-to-low mass halos, Mv <∼ 1011 M⊙, owing to the different shapes of the halo mass function and the galaxy stellar mass function at the low-mass end (van den Bosch et al. 2003; Shankar et al. 2006).”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, methodology): “Another powerful tool to link galaxies to dark matter halos is the so-called halo occupation model (Yang et al. 2003b; van den Bosch et al. 2003; Berlind et al. 2003; Zheng et al. 2005; Vale & Ostriker 2004; Kravtsov et al. 2004; for earlier work, see Jing et al. 1998; Peacock & Smith 2000; Seljak…”
The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation (2005, methodology): “Similar biases could potentially manifest in weak-lensing measurements and could lead to overestimates of the mass-tolight ratios in methods that use clustering to constrain the HOD or the conditional luminosity function (e.g., van den Bosch et al. 2003b).”
Cosmic ray feedback in hydrodynamical simulations of galaxy formation (2006, background): “We note that conditional luminosity function analysis of the 2 Degree Field Galaxy Redshift Survey (2dFGRS) has shown (van den Bosch et al., 2003) that there appears to be a minimum in the observed mass-to-light ratio of galaxies around a halo mass of ≈ 3×1011 h−1M⊙.”
The Halo Occupation Distribution and the Physics of Galaxy Formation (2002, background): “The mass dependence of the SA young fraction differs from that of the ‘‘ late-type fraction ’’ parameterization assumed by van den Bosch et al. (2003), which is forced to zero at high halo masses.”
Galaxy Evolution from Halo Occupation Distribution Modeling of DEEP2 and SDSS Galaxy Clustering (2007, methodology): “…luminosity function” (CLF) method (Yang, Mo, & van den Bosch 2003), has been applied to interpret clustering data from these local surveys (e.g., Jing & Börner 1998; Jing, Börner, & Suto 2002; van den Bosch et al. 2003; Magliocchetti & Porciani 2003; Zehavi et al. 2005; Yang et al. 2005).”
HALO OCCUPATION DISTRIBUTION MODELING OF CLUSTERING OF LUMINOUS RED GALAXIES (2008, methodology): “…measurements in several galaxy surveys (e.g., Jing & Börner 1998; Jing et al. 2002; Bullock et al. 2002; Moustakas & Somerville 2002; van den Bosch et al. 2003; Magliocchetti & Porciani 2003; Yan et al. 2003; Zheng 2004; Yang et al. 2005; Zehavi et al. 2005b; Lee et al. 2006; Hamana et al.…”
Properties of galaxy groups in the Sloan Digital Sky Survey – I. The dependence of colour, star formation and morphology on halo mass (2005, methodology): “The sample of galaxies is split in ‘early-types’ and ‘late-types’ using a probability function P late(L , M) (see van den Bosch et al. 2003).”