Satellite kinematics – III. Halo masses of central galaxies in SDSS

By S. More, F. V. D. Bosch, M. Cacciato, R. Skibba, H. Mo, Xiaohu Yang. 2010

246 citations recorded by the source corpus.

We use the kinematics of satellite galaxies that orbit around the central galaxy in a dark matter halo to infer the scaling relations between halo mass and central galaxy properties. Using galaxies from the Sloan Digital Sky Survey, we investigate the halo mass-luminosity relation (MLR) and the halo mass-stellar mass relation (MSR) of central galaxies. In particular, we focus on the dependence of these scaling relations on the colour of the central galaxy. We find that red central galaxies on average occupy more massive haloes than blue central galaxies of the same luminosity. However, at fixed stellar mass there is no appreciable difference in the average halo mass of red and blue centrals, especially for M-* less than or similar to 1010.5 h-2 M-circle dot. This indicates that stellar mass is a better indicator of halo mass than luminosity. Nevertheless, we find that the scatter in halo masses at fixed stellar mass is non-negligible for both red and blue centrals. It increases as a function of stellar mass for red centrals but shows a fairly constant behaviour for blue centrals. We compare the scaling relations obtained in this paper with results from other independent studies of satellite kinematics, with results from a SDSS galaxy group catalog, from galaxy-galaxy weak lensing measurements and from subhalo abundance matching studies. Overall, these different techniques yield MLRs and MSRs in fairly good agreement with each other (typically within a factor of 2), indicating that we are converging on an accurate and reliable description of the galaxy-dark matter connection. We briefly discuss some of the remaining discrepancies among the various methods.

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

View Paper: https://www.semanticscholar.org/paper/f88502536170ab0c7e8616c13a0d893f6d1cfc63

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Citations in the corpus

THE DEPENDENCE OF QUENCHING UPON THE INNER STRUCTURE OF GALAXIES AT 0.5 ⩽ z < 0.8 IN THE DEEP2/AEGIS SURVEY (2012, background): “Recently, More et al. (2011) inferred the halo mass-stellar mass relation based on kinematics of SDSS satellite galaxies and found that red, central galaxies, on average, occupy more massive halos than blue centrals for fixed luminosity, but show a less ap- 38 An interesting corollary comes from…”
ON THE INTERPLAY BETWEEN STAR FORMATION AND FEEDBACK IN GALAXY FORMATION SIMULATIONS (2014, methodology): “…different methods, such as dark matter halo abundance matching (Conroy & Wechsler 2009; Guo et al. 2010), satellite kinematics (Klypin & Prada 2009; More et al. 2011), and weak lensing (Mandelbaum et al. 2006) (see Kravtsov et al. 2014, for a comprehensive discussion) point towards peak stellar to…”
Stellar Mass—Halo Mass Relation and Star Formation Efficiency in High-Mass Halos (2014, result): “…mass end to other observational estimates of this relation at smaller masses, such as weak lensing (Mandelbaum et al. 2006; Reyes et al. 2012; Hudson et al. 2013) and satellite kinematics (More et al. 2011, earlier results by Conroy et al. 2007b are consistent with these results and are not shown).”
Constraining the galaxy–halo connection over the last 13.3 Gyr: star formation histories, galaxy mergers and structural properties (2017, methodology): “In the case of satellite kinematics it has been noted that this method tends to give higher halo masses than other methods (like those described above, see e.g., More et al. 2011; Skibba et al. 2011; Rodŕıguez-Puebla et al. 2011).”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, methodology): “Dutton et al. (2010b) combines halo masses measured from satellite kinematics (Conroy et al. 2007; More et al. 2011), weak lensing (Mandelbaum et al. 2006; Schulz et al. 2010), group catalogs (Yang et al. 2009) and halo abundance matching (Moster et al. 2010; Guo et al. 2010; Behroozi et al. 2010),…”
First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies (2017, result): “Combined with the results of N-body simulations, several observational estimates of the scatter have been made (More et al. 2011; Leauthaud et al. 2012; Reddick et al. 2013; Zu & Mandelbaum 2016; Tinker et al. 2017).”
The BAHAMAS project: Calibrated hydrodynamical simulations for large-scale structure cosmology (2016, unknown): “…measurements from a variety of previous studies (WL: Mandelbaum et al. 2006, 2008; Schulz et al. 2010; SK: Conroy et al. 2007; Klypin & Prada 2009; More et al. 2011) and took care to scale the stellar masses from these studies to a common Chabrier IMF and to adopt a common halo mass definition…”
THE SPLASHBACK RADIUS AS A PHYSICAL HALO BOUNDARY AND THE GROWTH OF HALO MASS (2015, unknown): “…2004; Tasitsiomi et al. 2004; Vale & Ostriker 2004; Conroy et al. 2005; Mandelbaum et al. 2006; Cacciato et al. 2009, 2013; Conroy & Wechsler 2009; More et al. 2009, 2011, 2015; Behroozi et al. 2010, 2013; Moster et al. 2010; Zehavi et al. 2011; Leauthaud et al. 2012; Kravtsov 2013; Kravtsov et…”
Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes since z ~ 1.2 (2011, methodology): “…the stellar-to-halo mass ratio as function of halo mass (Mandelbaum et al. 2006; Zheng et al. 2007; Foucaud et al. 2010; Zehavi et al. 2011; More et al. 2011; Wake et al. 2011; Leauthaud et al. 2012b), and “abundance-matching” techniques based on N-body simulations (Conroy & Wechsler 2009;…”
The kinematic connection between galaxies and dark matter haloes (2010, methodology): “…techniques: Weak lensing (WL) from Mandelbaum et al. (2006; 2008) and Schulz et al. (2010); Satellite kinematics (SK) from Conroy et al. (2007); More et al. (2010); and Klypin, Prada & Montero-Dorta (2010, in prep); halo abundance matching (AM) from Moster et al. (2010), Guo et al. (2010) and…”
WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z ∼ 2 FROM CANDELS (2011, result): “This is consistent with the claim by More et al. (2011) that at fixed stellar mass there isno differencebetween the average halo masses of quiescent and starforming central galaxies.”
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).”
redMaPPer. I. ALGORITHM AND SDSS DR8 CATALOG (2013, background): “Although blue central galaxies are more common (although still rare) at the group scale (e.g., George et al. 2011; More et al. 2011; George et al. 2012; Tinker et al. 2012), the redMaPPer clusters are much more massive than the scale at which this is an issue.”
MaGICC discs: matching observed galaxy relationships over a wide stellar mass range (2012, result): “The results agree remarkably well with direct derivations of the relation, where dark matter halo masses are determined by gravitational lensing (Mandelbaum et al. 2006) and the dynamics of satellite galaxies (More et al. 2011).”
THE IMPACT OF INTERACTIONS, BARS, BULGES, AND ACTIVE GALACTIC NUCLEI ON STAR FORMATION EFFICIENCY IN LOCAL MASSIVE GALAXIES (2012, background): “…and morphological parameters such as Sersic index, stellar mass surface density, or central velocity dispersion (Kauffmann et al. 2003b; Schiminovich et al. 2007; More et al. 2011; Wuyts et al. 2011; Catinella et al. 2010; Catinella et al. 2012; Saintonge et al. 2011a; Kauffmann et al. 2012).”
Galaxy Masses: A Review (2013, methodology): “More et al. 2011a) to measure total masses within the virial radius of the dark matter halo.”
A DIRECT MEASUREMENT OF THE BARYONIC MASS FUNCTION OF GALAXIES AND IMPLICATIONS FOR THE GALACTIC BARYON FRACTION (2012, methodology): “The star symbols correspond to galaxies for which Mh was estimated form stellar 8The Baldry et al. (2008) abundance matching result uses a “galactic” halo mass function by Shankar et al. (2006). dynamics (Conroy et al. 2007; More et al. 2011).”