The Halo Masses of Galaxies to z ∼ 3: A Hybrid Observational and Theoretical Approach

Abstract

We use a hybrid observational/theoretical approach to study the relation between galaxy kinematics and the derived stellar and halo masses of galaxies up to z = 3 as a function of stellar mass, redshift and morphology. Our observational sample consists of a concatenation of 1125 galaxies with kinematic measurements at 0.4 < z < 3 from long-slit and integral-field studies. We investigate several ways to measure halo masses from observations based on results from semi-analytical models, showing that galaxy halo masses can be retrieved with a scatter of ∼ 0.4 dex by using only stellar masses. We discover a third parameter, relating to the time of the formation of the halo, which reduces the scatter in the relation between the stellar and halo masses, such that systems forming earlier have a higher stellar mass to halo mass ratio, which we also find observationally. We find that this scatter correlates with morphology, such that early-type, or older stellar systems, have higher M * /M halo ratios. We furthermore show using this approach, and through weak lensing and abundance matching, that the ratio of stellar to halo mass does not significantly evolve with redshift at 1 < z < 3. This is evidence for the regulated hierarchical assembly of galaxies such that the ratio of stellar to dark matter mass remains approximately constant since z = 2. We use these results to show that the dark matter accretion rate evolves from dM halo /dt ∼ 4000 M year −1 at z ∼ 2.5, to a few 100 M year −1 by z ∼ 0.5.

The clustering of X-ray AGN at 0.5 &lt; z &lt; 4.5: host galaxies dictate dark matter halo mass

“…In Figure 8(a), we plot our clustering measurements of the AGN and find that AGN in high mass galaxies are more strongly clustered and appear to reside in halos that are almost an order of magnitude (0.9 dex) more massive than AGN in low mass hosts out to z ∼ 2 (at 1.7σ ). This is consistent with expectations from the galaxy stellar mass-halo mass relation (e.g., Li et al 2006;Meneux et al 2008;Wake et al 2011;Leauthaud et al 2012;Marulli et al 2013;Conselice et al 2018).…”

Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

“…Finally, we carried out an exploratory analysis of the stellarto-halo mass relation using the method outlined by our group (Lampichler et al 2017) and in Conselice et al (2018). We find that our cluster and field samples follow the theoretical predictions proposed by Moster et al (2013) at the redshift of our targets.…”

“…Recently, Conselice et al 2018 adopted several combined observational and theoretical approaches to derive the halo mass of field galaxies up to z∼3. In the next sections, we follow a method introduced by Lampichler et al ( 2017) and tested by Conselice et al (2018) to derive the halo mass values for our sample of galaxies. This method is only valid for objects with v/σ>1.…”

Galaxy formation and evolution science in the era of the Large Synoptic Survey Telescope

“…Given that this complexity results in remarkably regular sequences with galaxy mass, the outcome of the galaxy formation pro cess is often described by the connection between galaxy luminosity, or stellar mass, and their host dark matter halos 41,[48][49][50][51] . Known as the stellar mass-halo mass rela tion, this relation succinctly captures how the physics of galaxy formation leads to an efficiency of star formation that varies with the host dark matter halo mass [52][53][54][55] .…”