The size function of massive satellites from the $R_e-R_h$ and $M_{star}-M_h$ relations: constraining the role of environment

(2) University of Pennsylvania; (3) Universit\'e de Paris; (4) Instituto de Astrofisica de Canarias); Astroparticule et Cosmologie; CNRS; Francesco Shankar (1); Lorenzo Zanisi (1); Marc Huertas-Company (4) ((1) University of Southampton; Mariangela Bernardi (2); Simona Mei (3)

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The size function of massive satellites from the $R_e-R_h$ and $M_{star}-M_h$ relations: constraining the role of environment

Lorenzo Zanisi (1), Francesco Shankar (1), Mariangela Bernardi (2), Simona Mei (3), Marc Huertas-Company (4) ((1) University of Southampton, (2) University of Pennsylvania, (3) Université de Paris, CNRS

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Astroparticule et Cosmologie, (4) Instituto de Astrofisica de Canarias)

Astrophysics of Galaxies · Submitted 27 May 2021

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

The authors' main claim The $R_e-R_h$ appears to be fundamental to connect galaxies and their host haloes.

how it is stated · hedged possibility 0.81 read the record →

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arXiv ID2105.13363 (version 1)

Pith ID4NA4XSZ6, Pith's permanent record of this paper and its review

Citation(2) University of Pennsylvania, (3) Universit\'e de Paris, (4) Instituto de Astrofisica de Canarias), Astroparticule et Cosmologie, CNRS, Francesco Shankar (1), Lorenzo Zanisi (1), Marc Huertas-Company (4) ((1) University of Southampton, Mariangela Bernardi (2), Simona Mei (3). "The size function of massive satellites from the $R_e-R_h$ and $M_{star}-M_h$ relations: constraining the role of environment." arXiv:2105.13363 (2021). https://pith.science/paper/4NA4XSZ6

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,744 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.37 · human participants 0.01 · controlled comparison 0.13 · randomized assignment 0.02 · states quantitative result 0.35 · compares with prior results 0.86 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

In previous work we showed that a semi-empirical model in which galaxies in host dark matter haloes are assigned stellar masses via a stellar mass-halo mass (SMHM) relation and sizes ($R_e$) via a linear and tight $R_e-R_h$ relation, can faithfully reproduce the size function of local SDSS central galaxies and the strong size evolution of massive galaxies (MGs, $M_{\rm star}>10^{11.2}M_\odot$). In this third paper of the series, we focus on the population of satellite MGs. We find that without any additional calibration and irrespective of the exact SMHM relation, fraction of quenched galaxies or level of stellar stripping, the same model is able to reproduce the local size function of quiescent satellite MGs in SDSS. In addition, the same model can reproduce the puzzling weak dependence of mean size on host halo mass for both central and satellite galaxies. The model also matches the size function of starforming satellite MGs, after assuming that some of them transform into massive lenticulars in a few Gyr after infalling in the group/cluster environment. However, the vast majority of satellite lenticulars is predicted to form before infall. The $R_e-R_h$ appears to be fundamental to connect galaxies and their host haloes.

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	In previous work we showed that a semi-empirical model in which galaxies in host dark matter haloes are assigned stellar masses via a stellar mass-halo mass (SMHM) relation and sizes ($R_e$) via a linear and tight $R_e-R_h$ relation, can faithfully reproduce the size function of local SDSS central galaxies and the strong size evolution of massive galaxies (MGs, $M_{\rm star}>10^{11.2}M_\odot$).	background 0.99	0.34	0.07	asserted 1.00
s1	In this third paper of the series, we focus on the population of satellite MGs.	contribution 0.87	0.36	0.03	asserted 0.81
s2	We find that without any additional calibration and irrespective of the exact SMHM relation, fraction of quenched galaxies or level of stellar stripping, the same model is able to reproduce the local size function of quiescent satellite MGs in SDSS.	result 1.00	0.95	0.62	asserted 1.00
s3	In addition, the same model can reproduce the puzzling weak dependence of mean size on host halo mass for both central and satellite galaxies.	result 1.00	0.89	0.17	asserted 1.00
s4	The model also matches the size function of starforming satellite MGs, after assuming that some of them transform into massive lenticulars in a few Gyr after infalling in the group/cluster environment.	result 0.99	0.85	0.11	asserted 0.83
s5	However, the vast majority of satellite lenticulars is predicted to form before infall.	result 0.89	0.83	0.12	asserted 0.91
s6	The $R_e-R_h$ appears to be fundamental to connect galaxies and their host haloes.	interpretation 1.00	0.54	0.61	hedged possibility 0.81

What kind of paper the classifier reports this is: theoretical result 0.76 · evidence from analysis of existing data 0.62.

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arXiv listing abstract v1

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full text
figures and tables
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S sections
T body sentences
C citations
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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

In previous work we showed that a semi-empirical model in which galaxies in host dark matter haloes are assigned stellar masses via a stellar mass-halo mass (SMHM) relation and sizes ($R_e$) via a linear and tight $R_e-R_h$ relation, can faithfully reproduce the size function of local SDSS central galaxies and the strong size evolution of massive galaxies (MGs, $M_{\rm star}>10^{11.2}M_\odot$). In this third paper of the series, we focus on the population of satellite MGs. We find that without any additional calibration and irrespective of the exact SMHM relation, fraction of quenched galaxies or level of stellar stripping, the same model is able to reproduce the local size function of quiescent satellite MGs in SDSS. In addition, the same model can reproduce the puzzling weak dependence of mean size on host halo mass for both central and satellite galaxies. The model also matches the size function of starforming satellite MGs, after assuming that some of them transform into massive lenticulars in a few Gyr after infalling in the group/cluster environment. However, the vast majority of satellite lenticulars is predicted to form before infall. The $R_e-R_h$ appears to be fundamental to connect galaxies and their host haloes.

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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 · 2 sentences without a confident label

Uses the method or tool of 1 paper

We here closely follow the modelling approach of Papers I and II[We make extensive use of the Python package [ref] .]: * Dark matter catalogues.

COLOSSUS: A python toolkit for cosmology, large-scale structure, and dark matter halos · Methods · 0.97

Uses data or values from 1 paper

By using current estimates of the galaxy stellar mass function for quenched and star forming galaxies ( [ref] , [ref] ), in Paper 2, we have found that $μ$ is likely to lie at intermediate values, $μ≈2.5$.

The evolution of the galaxy stellar mass function over the last twelve billion years from a combination of ground-based and HST surveys · Methods · 0.93

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