Testing Galaxy Quenching Theories with Scatter in the Stellar to Halo Mass Relation. Tinker, J. L. arXiv:1607.06099 [astro-ph], July, 2016. arXiv: 1607.06099![Testing Galaxy Quenching Theories with Scatter in the Stellar to Halo Mass Relation [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We use the scatter in the stellar-to-halo mass relation to constrain galaxy evolution models. If the efficiency of converting accreted baryons into stars varies with time, halos of the same present-day mass but different formation histories will have different z=0 galaxy stellar mass. This is one of the sources of scatter in stellar mass at fixed halo mass, \${\textbackslash}sigma_\{{\textbackslash}log M{\textbackslash}ast\}\$. For massive halos that undergo rapid quenching of star formation at z\textasciitilde2, different mechanisms that trigger this quenching yield different values of \${\textbackslash}sigma_\{{\textbackslash}log M{\textbackslash}ast\}\$. We use this framework to test various models in which quenching begins after a galaxy crosses a threshold in one of the following physical quantities: redshift, halo mass, stellar mass, and stellar-to-halo mass ratio. Our model is highly idealized, with other sources of scatter likely to arise as more physics is included. Thus, our test is whether a model can produce scatter lower than observational bounds, leaving room for other sources. Recent measurements find \${\textbackslash}sigma_\{{\textbackslash}log M{\textbackslash}ast\}=0.16\$ dex for 10\textasciicircum11 Msol galaxies. Under the assumption that the threshold is constant with time, such a low value of \${\textbackslash}sigma_\{{\textbackslash}log M{\textbackslash}ast\}\$ rules out all of these models with the exception of quenching by a stellar mass treshold. Most physical quantities, such as metallicity, will increase scatter if they are uncorrelated with halo formation history. Thus, to decrease the scatter of a given model, galaxy properties would correlate tightly with formation history, creating testable predictions for their clustering. Understanding why \${\textbackslash}sigma_\{{\textbackslash}log M{\textbackslash}ast\}\$ is so small may be key to understanding the physics of galaxy formation.
@article{tinker_testing_2016,
title = {Testing {Galaxy} {Quenching} {Theories} with {Scatter} in the {Stellar} to {Halo} {Mass} {Relation}},
url = {http://arxiv.org/abs/1607.06099},
abstract = {We use the scatter in the stellar-to-halo mass relation to constrain galaxy evolution models. If the efficiency of converting accreted baryons into stars varies with time, halos of the same present-day mass but different formation histories will have different z=0 galaxy stellar mass. This is one of the sources of scatter in stellar mass at fixed halo mass, \${\textbackslash}sigma\_\{{\textbackslash}log M{\textbackslash}ast\}\$. For massive halos that undergo rapid quenching of star formation at z{\textasciitilde}2, different mechanisms that trigger this quenching yield different values of \${\textbackslash}sigma\_\{{\textbackslash}log M{\textbackslash}ast\}\$. We use this framework to test various models in which quenching begins after a galaxy crosses a threshold in one of the following physical quantities: redshift, halo mass, stellar mass, and stellar-to-halo mass ratio. Our model is highly idealized, with other sources of scatter likely to arise as more physics is included. Thus, our test is whether a model can produce scatter lower than observational bounds, leaving room for other sources. Recent measurements find \${\textbackslash}sigma\_\{{\textbackslash}log M{\textbackslash}ast\}=0.16\$ dex for 10{\textasciicircum}11 Msol galaxies. Under the assumption that the threshold is constant with time, such a low value of \${\textbackslash}sigma\_\{{\textbackslash}log M{\textbackslash}ast\}\$ rules out all of these models with the exception of quenching by a stellar mass treshold. Most physical quantities, such as metallicity, will increase scatter if they are uncorrelated with halo formation history. Thus, to decrease the scatter of a given model, galaxy properties would correlate tightly with formation history, creating testable predictions for their clustering. Understanding why \${\textbackslash}sigma\_\{{\textbackslash}log M{\textbackslash}ast\}\$ is so small may be key to understanding the physics of galaxy formation.},
urldate = {2016-09-09},
journal = {arXiv:1607.06099 [astro-ph]},
author = {Tinker, Jeremy L.},
month = jul,
year = {2016},
note = {arXiv: 1607.06099},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}
Downloads: 0
{"_id":"sZ3uAh96MHP4t5Gea","bibbaseid":"tinker-testinggalaxyquenchingtheorieswithscatterinthestellartohalomassrelation-2016","author_short":["Tinker, J. L."],"bibdata":{"bibtype":"article","type":"article","title":"Testing Galaxy Quenching Theories with Scatter in the Stellar to Halo Mass Relation","url":"http://arxiv.org/abs/1607.06099","abstract":"We use the scatter in the stellar-to-halo mass relation to constrain galaxy evolution models. If the efficiency of converting accreted baryons into stars varies with time, halos of the same present-day mass but different formation histories will have different z=0 galaxy stellar mass. This is one of the sources of scatter in stellar mass at fixed halo mass, \\${\\textbackslash}sigma_\\{{\\textbackslash}log M{\\textbackslash}ast\\}\\$. For massive halos that undergo rapid quenching of star formation at z\\textasciitilde2, different mechanisms that trigger this quenching yield different values of \\${\\textbackslash}sigma_\\{{\\textbackslash}log M{\\textbackslash}ast\\}\\$. We use this framework to test various models in which quenching begins after a galaxy crosses a threshold in one of the following physical quantities: redshift, halo mass, stellar mass, and stellar-to-halo mass ratio. Our model is highly idealized, with other sources of scatter likely to arise as more physics is included. Thus, our test is whether a model can produce scatter lower than observational bounds, leaving room for other sources. Recent measurements find \\${\\textbackslash}sigma_\\{{\\textbackslash}log M{\\textbackslash}ast\\}=0.16\\$ dex for 10\\textasciicircum11 Msol galaxies. Under the assumption that the threshold is constant with time, such a low value of \\${\\textbackslash}sigma_\\{{\\textbackslash}log M{\\textbackslash}ast\\}\\$ rules out all of these models with the exception of quenching by a stellar mass treshold. Most physical quantities, such as metallicity, will increase scatter if they are uncorrelated with halo formation history. Thus, to decrease the scatter of a given model, galaxy properties would correlate tightly with formation history, creating testable predictions for their clustering. Understanding why \\${\\textbackslash}sigma_\\{{\\textbackslash}log M{\\textbackslash}ast\\}\\$ is so small may be key to understanding the physics of galaxy formation.","urldate":"2016-09-09","journal":"arXiv:1607.06099 [astro-ph]","author":[{"propositions":[],"lastnames":["Tinker"],"firstnames":["Jeremy","L."],"suffixes":[]}],"month":"July","year":"2016","note":"arXiv: 1607.06099","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics","bibtex":"@article{tinker_testing_2016,\n\ttitle = {Testing {Galaxy} {Quenching} {Theories} with {Scatter} in the {Stellar} to {Halo} {Mass} {Relation}},\n\turl = {http://arxiv.org/abs/1607.06099},\n\tabstract = {We use the scatter in the stellar-to-halo mass relation to constrain galaxy evolution models. If the efficiency of converting accreted baryons into stars varies with time, halos of the same present-day mass but different formation histories will have different z=0 galaxy stellar mass. This is one of the sources of scatter in stellar mass at fixed halo mass, \\${\\textbackslash}sigma\\_\\{{\\textbackslash}log M{\\textbackslash}ast\\}\\$. For massive halos that undergo rapid quenching of star formation at z{\\textasciitilde}2, different mechanisms that trigger this quenching yield different values of \\${\\textbackslash}sigma\\_\\{{\\textbackslash}log M{\\textbackslash}ast\\}\\$. We use this framework to test various models in which quenching begins after a galaxy crosses a threshold in one of the following physical quantities: redshift, halo mass, stellar mass, and stellar-to-halo mass ratio. Our model is highly idealized, with other sources of scatter likely to arise as more physics is included. Thus, our test is whether a model can produce scatter lower than observational bounds, leaving room for other sources. Recent measurements find \\${\\textbackslash}sigma\\_\\{{\\textbackslash}log M{\\textbackslash}ast\\}=0.16\\$ dex for 10{\\textasciicircum}11 Msol galaxies. Under the assumption that the threshold is constant with time, such a low value of \\${\\textbackslash}sigma\\_\\{{\\textbackslash}log M{\\textbackslash}ast\\}\\$ rules out all of these models with the exception of quenching by a stellar mass treshold. Most physical quantities, such as metallicity, will increase scatter if they are uncorrelated with halo formation history. Thus, to decrease the scatter of a given model, galaxy properties would correlate tightly with formation history, creating testable predictions for their clustering. Understanding why \\${\\textbackslash}sigma\\_\\{{\\textbackslash}log M{\\textbackslash}ast\\}\\$ is so small may be key to understanding the physics of galaxy formation.},\n\turldate = {2016-09-09},\n\tjournal = {arXiv:1607.06099 [astro-ph]},\n\tauthor = {Tinker, Jeremy L.},\n\tmonth = jul,\n\tyear = {2016},\n\tnote = {arXiv: 1607.06099},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},\n}\n\n","author_short":["Tinker, J. L."],"key":"tinker_testing_2016","id":"tinker_testing_2016","bibbaseid":"tinker-testinggalaxyquenchingtheorieswithscatterinthestellartohalomassrelation-2016","role":"author","urls":{"Paper":"http://arxiv.org/abs/1607.06099"},"keyword":["Astrophysics - Astrophysics of Galaxies","Astrophysics - Cosmology and Nongalactic Astrophysics"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies","astrophysics - cosmology and nongalactic astrophysics"],"search_terms":["testing","galaxy","quenching","theories","scatter","stellar","halo","mass","relation","tinker"],"title":"Testing Galaxy Quenching Theories with Scatter in the Stellar to Halo Mass Relation","year":2016}