Satellite kinematics – II. The halo mass–luminosity relation of central galaxies in SDSS

By S. More, F. V. D. Bosch, M. Cacciato, H. Mo, Xiaohu Yang, Ran Li. 2008

160 citations recorded by the source corpus.

The kinematics of satellite galaxies reflect the masses of the extended dark matter haloes in which they orbit, and thus shed light on the mass-luminosity relation (MLR) of their corresponding central galaxies. In this paper, we select a large sample of centrals and satellites from the Sloan Digital Sky Survey and measure the kinematics (velocity dispersions) of the satellite galaxies as a function of the r-band luminosity of the central galaxies. Using the analytical framework presented in More, van den Bosch & Cacciato, we use these data to infer both the mean and the scatter of the MLR of central galaxies, carefully taking account of selection effects and biases introduced by the stacking procedure. As expected, brighter centrals on average reside in more massive haloes. In addition, we find that the scatter in halo masses for centrals of a given luminosity, sigma(log) (M), also increases with increasing luminosity. As we demonstrate, this is consistent with sigma(log L), which reflects the scatter in the conditional probability function P(L(c)|M), being independent of halo mass. Our analysis of the satellite kinematics yields sigma(log L) = 0.16 +/- 0.04, in excellent agreement with constraints from clustering and group catalogues, and with predictions from a semi- analytical model of galaxy formation. We thus conclude that the amount of stochasticity in galaxy formation, which is characterized by sigma(log L) , is well constrained, independent of halo mass and in a good agreement with current models of galaxy formation.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ca5a303b66f0cc16271008e8de64467e469fb470

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Citations in the corpus

HALO OCCUPATION DISTRIBUTION MODELING OF CLUSTERING OF LUMINOUS RED GALAXIES (2008, unknown): “More et al. (2009) constrain the high-mass slope to be 0.28+0.07−0.09 for z < 0.072 SDSS galaxies based on satellite kinematics.”
THE CONNECTION BETWEEN GALAXIES AND DARK MATTER STRUCTURES IN THE LOCAL UNIVERSE (2012, background): “This has been shown by previous authors (More et al. 2009; Leauthaud et al. 2012), and is shown to be excluded by our later analysis.”
Erratum: From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology (2010, background): “In their own comparison of a similar relation to observational data on satellite galaxy dynamics, More et al. (2009) estimated the scatter in logL for relatively massive halos (logMvir ∼ 13) to be 0.16±0.04.”
Cosmological constraints from a combination of galaxy clustering and lensing – I. Theoretical framework (2012, background): “Very similar results were obtained by van den Bosch et al. (2007) and by Tinker et al. (2007).”
Cosmological Constraints from a Combination of Galaxy Clustering and Lensing -- III. Application to SDSS Data (2012, methodology): “However, a number of recent studies have argued that the spatial distribution of satellite galaxies is less centrally concentrated than the dark matter (e.g., Yang et al. 2005; Chen 2008; More et al. 2009).”
The dark side of galaxy colour (2013, result): “Our luminosity abundance matching technique results in ∼ 0.15dex of scatter in luminosity at fixed Vmax over the luminosity range of our sample, in accord with results from satellite kinematics (More et al. 2009) as well as other abundance matching studies (Reddick et al. 2012).”
The kinematic connection between galaxies and dark matter haloes (2010, background): “…the liter- ⋆ dutton@uvic.ca † CITA National Fellow ature has focused on the relation between halo mass and galaxy luminosity or stellar mass (e.g. Yang et al. 2003; Kravtsov et al. 2004; van den Bosch et al. 2004; Hoekstra et al. 2005; Mandelbaum et al. 2006; Conroy et al. 2007; More et al. 2009).”
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.”
A COMPREHENSIVE ANALYSIS OF UNCERTAINTIES AFFECTING THE STELLAR MASS–HALO MASS RELATION FOR 0 < z < 4 (2010, methodology): “As the Yang et al. (2009b) value is consistent with the More et al. (2009) value, we set the prior using the More et al. (2009) value and error bounds onξ, We assume a Gaussian prior on the probability distribution forξ, and we assume that the scatter itself is log-normal.”
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): “For example, Yang et al. (2009) find that σlog M∗ = 0.17 dex and More et al. (2009) find a scatter in luminosity at fixed halo mass of 0.16 ± 0.04 dex.”
How do galaxies populate dark matter haloes (2009, methodology): “3 show mean halo mass as a function of central stellar mass as derived from the stacked kinematics of the satellites of a large sample of SDSS central galaxies (More et al. 2009).”
THE PSEUDO-EVOLUTION OF HALO MASS (2012, background): “…aspects of galaxy formation and have been studied via a variety of probes such as satellite kinematics (Prada et al. 2003; Conroy et al. 2007; More et al. 2009, 2011b), galaxy-galaxy weak lensing (Seljak 2000; McKay et al. 2001; Mandelbaum et al. 2006; Parker et al. 2007; Schulz et al.…”
DARK MATTER HALOS IN THE STANDARD COSMOLOGICAL MODEL: RESULTS FROM THE BOLSHOI SIMULATION (2010, background): “…Klypin et al. 1999; Coĺın et al. 1999), the potential annihilation signal of dark matter (e.g., Kuhlen et al. 2008; Springel et al. 2008; Ando 2009), and motion of satellites as a probe for masses of isolated galaxies and groups (e.g., Prada et al. 2003; Klypin & Prada 2009; More et al. 2009).”
UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, background): “Larger haloes host larger galaxies, with relatively tight scatter in the stellar mass—halo mass relation (More et al. 2009; Yang et al. 2009; Leauthaud et al. 2012; Reddick et al. 2013; Watson & Conroy 2013; Tinker et al. 2013; Gu et al. 2016).”
Are Brightest Halo Galaxies Central Galaxies (2010, methodology): “More et al. (2009) obtained a similar value from their analysis of satellite kinematics: σcen = 0.16 ± 0.04.”
Making Galaxies in a Cosmological Context: The Need for Early Stellar Feedback (2012, background): “Direct comparisons of stellar mass and total halo mass have also been done based on satellite dynamics (Klypin & Prada 2009; More et al. 2009, 2011) and weak lensing (Mandelbaum et al. 2009; Schulz et al. 2010).”
THE AVERAGE STAR FORMATION HISTORIES OF GALAXIES IN DARK MATTER HALOS FROM z = 0–8 (2012, background): “While current studies have indicated that this is approximately 0.16–0.2 dex atz = 0 (More et al. 2009; Yang et al. 2009b; Reddick et al. 2012) with no evidence for a mass trend at least down to 1012M⊙ in halo mass (Reddick et al. 2012), little is known about the redshift evolution of this scatter.”
FastPM: a new scheme for fast simulations of dark matter and haloes (2016, background): “A 10% stochasticity is likely more accurate than our current level understanding of the halo mass - galaxy luminosity relation (Behroozi, Conroy & Wechsler 2010; More et al. 2009; Yang, Mo & van den Bosch 2009).”