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Evolution of the Stellar-to-Dark Matter Relation: Separating Star-Forming and Passive Galaxies from z=1 to 0
Cosmology and Nongalactic Astrophysics · Submitted 13 Aug 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency.
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The abstract, sentence by sentence
We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z=[0.2,1.0]. For massive galaxies, M*>~10^10.6 Msol, our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z=1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M*~10^10 Msol, the fraction of central galaxies on the red sequence increases by a factor of ten over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z=1 to z=0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z=[0.2,1.0]. | method 0.79 | 0.96 | 0.05 | asserted 0.98 |
| s1 | For massive galaxies, M*>~10^10.6 Msol, our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. | result 1.00 | 0.95 | 0.36 | hedged possibility 0.97 |
| s2 | At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. | interpretation 0.53 | 0.91 | 0.14 | asserted 0.65 |
| s3 | Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. | contribution 0.71 | 0.95 | 0.04 | asserted 0.97 |
| s4 | At z=1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. | result 1.00 | 0.90 | 0.08 | asserted 1.00 |
| s5 | But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. | result 0.95 | 0.90 | 0.24 | asserted 1.00 |
| s6 | At M*~10^10 Msol, the fraction of central galaxies on the red sequence increases by a factor of ten over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. | result 1.00 | 0.92 | 0.14 | asserted 1.00 |
| s7 | We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. | contribution 0.54 | 0.88 | 0.05 | asserted 0.90 |
| s8 | We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z=1 to z=0. | result 1.00 | 0.97 | 0.17 | asserted 1.00 |
| s9 | These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency. | interpretation 1.00 | 0.62 | 0.58 | asserted 0.69 |
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The paper
Original abstract
We use measurements of the stellar mass function, galaxy clustering, and galaxy-galaxy lensing within the COSMOS survey to constrain the stellar-to-halo mass relation (SHMR) of star forming and quiescent galaxies over the redshift range z=[0.2,1.0]. For massive galaxies, M*>~10^10.6 Msol, our results indicate that star-forming galaxies grow proportionately as fast as their dark matter halos while quiescent galaxies are outpaced by dark matter growth. At lower masses, there is minimal difference in the SHMRs, implying that the majority low-mass quiescent galaxies have only recently been quenched of their star formation. Our analysis also affords a breakdown of all COSMOS galaxies into the relative numbers of central and satellite galaxies for both populations. At z=1, satellite galaxies dominate the red sequence below the knee in the stellar mass function. But the number of quiescent satellites exhibits minimal redshift evolution; all evolution in the red sequence is due to low-mass central galaxies being quenched of their star formation. At M*~10^10 Msol, the fraction of central galaxies on the red sequence increases by a factor of ten over our redshift baseline, while the fraction of quenched satellite galaxies at that mass is constant with redshift. We define a "migration rate" to the red sequence as the time derivative of the passive galaxy abundances. We find that the migration rate of central galaxies to the red sequence increases by nearly an order of magnitude from z=1 to z=0. These results imply that the efficiency of quenching star formation for centrals is increasing with cosmic time, while the mechanisms that quench the star formation of satellite galaxies in groups and clusters is losing efficiency.
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References
How the literature uses it
8 arXiv papers cite this in 18 sentences
Papers citing it · 10 sentences without a confident label
Compares with it 1 paper
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Of course, our analysis methods are not directly analogous to COSMOS analysis in [ref] : we have studied a different formulation of the HOD from theirs, and we have focused exclusively on galaxy clustering measurements, whereas they have included galaxy-galaxy lensing data (see below).
Galaxy Assembly Bias: A Significant Source of Systematic Error in the Galaxy-Halo Relationship · DISCUSSION · 0.91
Cites it as support 1 paper
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Nonetheless, [ref] have demonstrated the potential of the HOD to provide rich information about the history of star formation in galaxies, and so the results in [ref] provide strong motivation to constrain the true level of assembly bias in the data.
Galaxy Assembly Bias: A Significant Source of Systematic Error in the Galaxy-Halo Relationship · DISCUSSION · 1.00
Cites it as background 4 papers
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This implementation of the HOD-formalism in conjunction with the halo model formalism, or slight modifications thereof, is relatively standard and similar models have been used in numerous studies including the completed SDSS galaxy clustering analysis of [ref] as well as [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , [ref] , and [ref] , to name some of the recent contributions to this extensive literature.
Galaxy Assembly Bias: A Significant Source of Systematic Error in the Galaxy-Halo Relationship · The Halo Model and the Halo Occupation Distribution · 0.86
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Previous small-scale clustering studies of ELG samples at redshifts $∼1$ were performed in different frameworks, either HOD [ref] , Abundance Matching [ref] or conditional stellar mass function method [ref] .
The DESI One-Percent survey: exploring the Halo Occupation Distribution of Emission Line Galaxies with AbacusSummit simulations · Standard HOD results · 0.99
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In the CLF, the quantity $Φ(L|)$ plays the central role by specifying the mean abundance of galaxies of luminosity $L$ found in dark matter halos of mass $.$ These well-studied formalisms have both proven to be very powerful theoretical tools to constrain both the galaxy-halo connection [ref] and the fundamental parameters in cosmology [ref] .
Beyond Halo Mass: Galactic Conformity as a Smoking Gun of Central Galaxy Assembly Bias · INTRODUCTION · 0.92
What it cites · 3 sentences without a confident label
Uses the method or tool of 1 paper
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Quenched fractions in sub-populations of the group catalog are corrected for impurity and completeness statistically (see further details in [ref] ).
Are Halo and Galaxy Formation Histories Correlated? · Stellar Mass Functions and the Quenched Fraction of Galaxies · 0.92
Uses data or values from 1 paper
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In this figure we have included data from the SDSS groups catalog of [ref] .
Are Halo and Galaxy Formation Histories Correlated? · Central-Satellite Decomposition of the Stellar Mass Functions · 0.95
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