Modeling color-dependent galaxy clustering in cosmological simulations

Naoki Yoshida; Shogo Masaki; Yen-Ting Lin

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Modeling color-dependent galaxy clustering in cosmological simulations

Shogo Masaki, Yen-Ting Lin, Naoki Yoshida

Cosmology and Nongalactic Astrophysics · Submitted 7 Jan 2013

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

The authors' main claim We show that the extended abundance matching method using the local dark matter density as a color proxy provides an accurate description of the galaxy populations in the local universe.

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arXiv ID1301.1217 (version 2)

Pith IDGHLYNMQD, Pith's permanent record of this paper and its review

CitationNaoki Yoshida, Shogo Masaki, Yen-Ting Lin. "Modeling color-dependent galaxy clustering in cosmological simulations." arXiv:1301.1217 (2013). https://pith.science/paper/GHLYNMQD

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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.46 · human participants 0.01 · controlled comparison 0.10 · randomized assignment 0.02 · states quantitative result 0.07 · compares with prior results 0.92 · mentions code or data availability 0.02.

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arXiv listing abstract v2. Results and the main claim are underlined; show every role.

We extend the subhalo abundance matching method to assign galaxy color to subhalos. We separate a luminosity-binned subhalo sample into two groups by a secondary subhalo property which is presumed to be correlated with galaxy color. The two subsamples then represent red and blue galaxy populations. We explore two models for the secondary property, namely subhalo assembly time and local dark matter density around each subhalo. The model predictions for the galaxy two-point correlation functions are compared with the recent results from the Sloan Digital Sky Survey. We show that the observed color dependence of galaxy clustering can be reproduced well by our method applied to cosmological N-body simulations without baryonic processes. We then compare the model predictions for the color-dependent galaxy-mass cross correlation functions with the results from gravitational lensing observations. The comparison allows us to distinguish the models, and also to discuss what subhalo property should be used to assign color to subhalos accurately. We show that the extended abundance matching method using the local dark matter density as a color proxy provides an accurate description of the galaxy populations in the local universe. We also study impacts of scatter in the local dark matter density-color relations. Introducing scatter improves agreements of our model predictions with the observed red and blue galaxy clustering and is needed to explain observed correlation functions in finer color bins. Finally, we study red galaxy fraction profiles in galaxy group- and cluster-sized halos and find the red fraction profiles have a relatively strong dependence on our model parameters. We argue that the red fraction profiles can be an important observational clue, in addition to galaxy clustering and galaxy-galaxy lensing, to explore the galaxy-(sub)halo connections.

background contribution method result interpretation main claim

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 extend the subhalo abundance matching method to assign galaxy color to subhalos.	contribution 0.73	0.96	0.03	asserted 0.98
s1	We separate a luminosity-binned subhalo sample into two groups by a secondary subhalo property which is presumed to be correlated with galaxy color.	method 0.99	0.94	0.02	asserted 0.73
s2	The two subsamples then represent red and blue galaxy populations.	method 0.94	0.63	0.03	asserted 0.99
s3	We explore two models for the secondary property, namely subhalo assembly time and local dark matter density around each subhalo.	method 0.98	0.88	0.02	asserted 0.91
s4	The model predictions for the galaxy two-point correlation functions are compared with the recent results from the Sloan Digital Sky Survey.	method 0.83	0.78	0.03	asserted 0.64
s5	We show that the observed color dependence of galaxy clustering can be reproduced well by our method applied to cosmological N-body simulations without baryonic processes.	result 1.00	0.95	0.46	asserted 1.00
s6	We then compare the model predictions for the color-dependent galaxy-mass cross correlation functions with the results from gravitational lensing observations.	method 0.63	0.89	0.04	asserted 0.69
s7	The comparison allows us to distinguish the models, and also to discuss what subhalo property should be used to assign color to subhalos accurately.	interpretation 0.47	0.90	0.09	asserted 0.67
s8	We show that the extended abundance matching method using the local dark matter density as a color proxy provides an accurate description of the galaxy populations in the local universe.	result 0.99	0.95	0.73	asserted 1.00
s9	We also study impacts of scatter in the local dark matter density-color relations.	contribution 0.88	0.94	0.04	unclear 0.69
s10	Introducing scatter improves agreements of our model predictions with the observed red and blue galaxy clustering and is needed to explain observed correlation functions in finer color bins.	result 0.97	0.95	0.11	asserted 0.99
s11	Finally, we study red galaxy fraction profiles in galaxy group- and cluster-sized halos and find the red fraction profiles have a relatively strong dependence on our model parameters.	result 0.90	0.97	0.06	asserted 1.00
s12	We argue that the red fraction profiles can be an important observational clue, in addition to galaxy clustering and galaxy-galaxy lensing, to explore the galaxy-(sub)halo connections.	interpretation 0.84	0.52	0.13	hedged possibility 0.70

What kind of paper the classifier reports this is: simulation study 0.54 · evidence from simulation or computation 0.99.

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references and citing sentences
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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 extend the subhalo abundance matching method to assign galaxy color to subhalos. We separate a luminosity-binned subhalo sample into two groups by a secondary subhalo property which is presumed to be correlated with galaxy color. The two subsamples then represent red and blue galaxy populations. We explore two models for the secondary property, namely subhalo assembly time and local dark matter density around each subhalo. The model predictions for the galaxy two-point correlation functions are compared with the recent results from the Sloan Digital Sky Survey. We show that the observed color dependence of galaxy clustering can be reproduced well by our method applied to cosmological N-body simulations without baryonic processes. We then compare the model predictions for the color-dependent galaxy-mass cross correlation functions with the results from gravitational lensing observations. The comparison allows us to distinguish the models, and also to discuss what subhalo property should be used to assign color to subhalos accurately. We show that the extended abundance matching method using the local dark matter density as a color proxy provides an accurate description of the galaxy populations in the local universe. We also study impacts of scatter in the local dark matter density-color relations. Introducing scatter improves agreements of our model predictions with the observed red and blue galaxy clustering and is needed to explain observed correlation functions in finer color bins. Finally, we study red galaxy fraction profiles in galaxy group- and cluster-sized halos and find the red fraction profiles have a relatively strong dependence on our model parameters. We argue that the red fraction profiles can be an important observational clue, in addition to galaxy clustering and galaxy-galaxy lensing, to explore the galaxy-(sub)halo connections.

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References

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2 arXiv papers cite this in 3 sentences

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

Papers citing it · 1 sentence without a confident label

Compares with it 1 paper

The model studied in [ref] is in essence a CAM model in which the conditional abundance is performed with halo central density rather than $.$ It is not particularly surprising that both models are effective, because in age matching $$ is primarily governed by halo concentration, which is of course strongly correlated with central density.

The Dark Side of Galaxy Color: evidence from new SDSS measurements of galaxy clustering and lensing · Future Work · 0.93

Cites it as background 1 paper

Extensive effort has been put forth to understand how the star formation activity in galaxies maps to dark matter halos in a cosmological context, typically via galaxy color [ref] .

The Dark Side of Galaxy Color: evidence from new SDSS measurements of galaxy clustering and lensing · INTRODUCTION · 0.99

What it cites · 3 sentences without a confident label

Uses the method or tool of 1 paper

We project all simulation particles around each subhalo along a direction in the simulation box to measure the surface mass density [ref] .

Looking at the relation between haloes and galaxies under the lens · Color dependence of lensing profile · 1.00

Compares with 1 paper

After the submission of this paper, [ref] presented an approach that is similar in spirit to our method in assigning colors to subhalos.

The Dark Side of Galaxy Color · Introduction · 0.91

Cites as support 1 paper

[ref] studied the fraction of central galaxies that are not forming stars actively (“quenched centrals”) as a function of the local galaxy density using a SDSS group catalog.

Are Halo and Galaxy Formation Histories Correlated? · Summary and Discussion · 0.98

Cites as background 3 papers

The second method is called the subhalo abundance matching [ref] .

SHAM Beyond Clustering: New Tests of Galaxy-Halo Abundance Matching with Galaxy Groups · Introduction · 0.85
The second method is called the subhalo abundance matching [ref] .

Understanding the nature of luminous red galaxies (LRGs): Connecting LRGs to central and satellite subhalos · Introduction · 0.85
The second method is called the subhalo abundance matching [ref] .

The Dark Side of Galaxy Color · Introduction · 0.85

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