The coevolution of the velocity and mass functions of galaxies and dark haloes

Kyu-Hyun Chae

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The coevolution of the velocity and mass functions of galaxies and dark haloes

Kyu-Hyun Chae

Cosmology and Nongalactic Astrophysics · Submitted 3 Mar 2010

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim Our results support the simple picture that as the halo grows hierarchically, the stellar mass and the central stellar velocity dispersion grow in parallel.

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What the abstract itself states, as probabilities: claims first 0.81 · states limitation 0.12 · human participants 0.01 · controlled comparison 0.35 · randomized assignment 0.01 · states quantitative result 0.11 · compares with prior results 0.94 · mentions code or data availability 0.02.

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We employ a bias-corrected abundance matching technique to investigate the coevolution of the LCDM dark halo mass function (HMF), the observationally derived velocity dispersion and stellar mass functions (VDF, SMF) of galaxies between z=1 and 0. We use for the first time the evolution of the VDF constrained through strong lensing statistics by Chae (2010) for galaxy-halo abundance matching studies. As a local benchmark we use a couple of z ~ 0 VDFs (a Monte-Carlo realised VDF based on SDSS DR5 and a directly measured VDF based on SDSS DR6). We then focus on connecting the VDF evolution to the HMF evolution predicted by N-body simulations and the SMF evolution constrained by galaxy surveys. On the VDF-HMF connection, we find that the local dark halo virial mass-central stellar velocity dispersion (Mvir-sigma) relation is in good agreement with the individual properties of well-studied low-redshift dark haloes, and the VDF evolution closely parallels the HMF evolution meaning little evolution in the Mvir-sigma relation. On the VDF-SMF connection, it is also likely that the stellar mass-stellar velocity dispersion (Mstar-sigma) relation evolves little taking the abundance matching results together with other independent observational results and hydrodynamic simulation results. Our results support the simple picture that as the halo grows hierarchically, the stellar mass and the central stellar velocity dispersion grow in parallel. We discuss possible implications of this parallel coevolution for galaxy formation and evolution under the LCDM paradigm.

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What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We employ a bias-corrected abundance matching technique to investigate the coevolution of the LCDM dark halo mass function (HMF), the observationally derived velocity dispersion and stellar mass functions (VDF, SMF) of galaxies between z=1 and 0.	contribution 0.71	0.93	0.05	asserted 0.82
s1	We use for the first time the evolution of the VDF constrained through strong lensing statistics by Chae (2010) for galaxy-halo abundance matching studies.	contribution 0.83	0.67	0.03	asserted 1.00
s2	As a local benchmark we use a couple of z ~ 0 VDFs (a Monte-Carlo realised VDF based on SDSS DR5 and a directly measured VDF based on SDSS DR6).	method 0.99	0.54	0.02	asserted 0.96
s3	We then focus on connecting the VDF evolution to the HMF evolution predicted by N-body simulations and the SMF evolution constrained by galaxy surveys.	contribution 0.52	0.66	0.04	unclear 0.69
s4	On the VDF-HMF connection, we find that the local dark halo virial mass-central stellar velocity dispersion (Mvir-sigma) relation is in good agreement with the individual properties of well-studied low-redshift dark haloes, and the VDF evolution closely parallels the HMF evolution meaning little evolution in the Mvir-sigma relation.	result 1.00	0.95	0.34	asserted 1.00
s5	On the VDF-SMF connection, it is also likely that the stellar mass-stellar velocity dispersion (Mstar-sigma) relation evolves little taking the abundance matching results together with other independent observational results and hydrodynamic simulation results.	result 0.87	0.44	0.15	hedged possibility 1.00
s6	Our results support the simple picture that as the halo grows hierarchically, the stellar mass and the central stellar velocity dispersion grow in parallel.	interpretation 0.91	0.70	0.78	asserted 0.61
s7	We discuss possible implications of this parallel coevolution for galaxy formation and evolution under the LCDM paradigm.	interpretation 0.94	0.47	0.05	unclear 0.80

What kind of paper the classifier reports this is: empirical study 0.32 · evidence from analysis of existing data 0.98.

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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

We employ a bias-corrected abundance matching technique to investigate the coevolution of the LCDM dark halo mass function (HMF), the observationally derived velocity dispersion and stellar mass functions (VDF, SMF) of galaxies between z=1 and 0. We use for the first time the evolution of the VDF constrained through strong lensing statistics by Chae (2010) for galaxy-halo abundance matching studies. As a local benchmark we use a couple of z ~ 0 VDFs (a Monte-Carlo realised VDF based on SDSS DR5 and a directly measured VDF based on SDSS DR6). We then focus on connecting the VDF evolution to the HMF evolution predicted by N-body simulations and the SMF evolution constrained by galaxy surveys. On the VDF-HMF connection, we find that the local dark halo virial mass-central stellar velocity dispersion (Mvir-sigma) relation is in good agreement with the individual properties of well-studied low-redshift dark haloes, and the VDF evolution closely parallels the HMF evolution meaning little evolution in the Mvir-sigma relation. On the VDF-SMF connection, it is also likely that the stellar mass-stellar velocity dispersion (Mstar-sigma) relation evolves little taking the abundance matching results together with other independent observational results and hydrodynamic simulation results. Our results support the simple picture that as the halo grows hierarchically, the stellar mass and the central stellar velocity dispersion grow in parallel. We discuss possible implications of this parallel coevolution for galaxy formation and evolution under the LCDM paradigm.

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What this paper does with the arXiv papers it cites

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

What it cites · 12 sentences without a confident label

Uses data or values from 1 paper

By relating the maximum circular velocity to the halo virial mass using the scaling given by [ref] , we find a varying fraction from $f_sub ≈0.25$ ($≈0.18$) at $10^11$ (this mass scale corresponds to the [ref] completeness limit) to $≈0.08$ ($≈0.08$) at $10^13$ for $z=0$ ($z=1$).

Halos and galaxies in the standard cosmological model: results from the Bolshoi simulation · Connection between the observational VDF and the HMF from N-body simulations · 0.84

Compares with 1 paper

However, our results for less massive galaxies ($10^2.3$) give systematically higher median values of $/$ compared with the [ref] results for late-type galaxies although the estimated intrinsic scatters (not shown here) overlap.

The Kinematic Connection Between Galaxies and Dark Matter Haloes · The $$-$$ relation at $z=0$ · 1.00

Cites as support 2 papers

The observation that the amount of star formation (i.e. stellar mass $$) is correlated with $$ (e.g. [ref] ) is consistent with the above picture.

Constraints on the relationship between stellar mass and halo mass at low and high redshift · Implications for the $$ paradigm and galaxy evolution · 0.99
The observation that the amount of star formation (i.e. stellar mass $$) is correlated with $$ (e.g. [ref] ) is consistent with the above picture.

How do galaxies populate Dark Matter halos? · Implications for the $$ paradigm and galaxy evolution · 0.99

Cites as background 3 papers

Some recent works in the literature are focused on the connection of the HMF with the broadly measured stellar mass function (SMF) of galaxies (e.g., [ref] ).

Constraints on the relationship between stellar mass and halo mass at low and high redshift · Introduction · 0.98
Some recent works in the literature are focused on the connection of the HMF with the broadly measured stellar mass function (SMF) of galaxies (e.g., [ref] ).

How do galaxies populate Dark Matter halos? · Introduction · 0.98
Accordingly, it includes the stellar mass once the galaxy is formed.] function (HMF) over cosmic time (e.g., [ref] ).

Halos and galaxies in the standard cosmological model: results from the Bolshoi simulation · Introduction · 0.84

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