On the influence of halo mass accretion history on galaxy properties and assembly bias. Montero-Dorta, A. D., Chaves-Montero, J., Artale, M. C., & Favole, G. arXiv e-prints, 2105:arXiv:2105.05274, May, 2021. Paper abstract bibtex Halo assembly bias is the secondary dependence of the clustering of dark-matter haloes on their assembly histories at fixed halo mass. This established dependence is expected to manifest itself on the clustering of the galaxy population, a potential effect commonly known as galaxy assembly bias. Using the IllustrisTNG300 magnetohydrodynamical simulation, we analyse the dependence of the properties and clustering of galaxies on the shape of the specific mass accretion history of their hosting haloes (sMAH). We first show that several halo and galaxy properties strongly correlate with the slope of the sMAH (\${\textbackslash}beta\$) at fixed halo mass. Namely, haloes with increasingly steeper \${\textbackslash}beta\$ increment their halo masses faster at early times, and their hosted galaxies present larger stellar-to-halo mass ratios, lose their gas faster, reach the peak of their star formation histories at higher redshift, and become quenched earlier. We also demonstrate that \${\textbackslash}beta\$ is more directly connected to these key galaxy formation properties than other broadly employed halo proxies, such as formation time. Finally, we measure the secondary dependence of galaxy clustering on \${\textbackslash}beta\$ at fixed halo mass as a function of redshift. By tracing back the evolution of individual haloes, we show that the amplitude of the galaxy assembly bias signal for the progenitors of \$z=0\$ galaxies increases with redshift, reaching a factor of 2 at \$z = 1\$ for haloes of \$M_{\textbackslash}mathrm\{halo\}=10{\textasciicircum}\{11.5\}-10{\textasciicircum}\{12\}\$ \$h{\textasciicircum}\{-1\}{\textbackslash}mathrm\{M\}_{\textbackslash}odot\$. The measurement of the evolution of assembly bias along the merger tree provides a new theoretical perspective to the study of secondary bias. Our findings, which show a tight relationship between halo accretion and both the clustering and the observational properties of the galaxy population, have also important implications for the generation of mock catalogues for upcoming cosmological surveys.
@article{montero-dorta_influence_2021,
title = {On the influence of halo mass accretion history on galaxy properties and assembly bias},
volume = {2105},
url = {http://adsabs.harvard.edu/abs/2021arXiv210505274M},
abstract = {Halo assembly bias is the secondary dependence of the clustering of
dark-matter haloes on their assembly histories at fixed halo mass. This
established dependence is expected to manifest itself on the clustering
of the galaxy population, a potential effect commonly known as galaxy
assembly bias. Using the IllustrisTNG300 magnetohydrodynamical
simulation, we analyse the dependence of the properties and clustering
of galaxies on the shape of the specific mass accretion history of their
hosting haloes (sMAH). We first show that several halo and galaxy
properties strongly correlate with the slope of the sMAH (\${\textbackslash}beta\$) at
fixed halo mass. Namely, haloes with increasingly steeper \${\textbackslash}beta\$
increment their halo masses faster at early times, and their hosted
galaxies present larger stellar-to-halo mass ratios, lose their gas
faster, reach the peak of their star formation histories at higher
redshift, and become quenched earlier. We also demonstrate that \${\textbackslash}beta\$
is more directly connected to these key galaxy formation properties than
other broadly employed halo proxies, such as formation time. Finally, we
measure the secondary dependence of galaxy clustering on \${\textbackslash}beta\$ at
fixed halo mass as a function of redshift. By tracing back the evolution
of individual haloes, we show that the amplitude of the galaxy assembly
bias signal for the progenitors of \$z=0\$ galaxies increases with
redshift, reaching a factor of 2 at \$z = 1\$ for haloes of
\$M\_{\textbackslash}mathrm\{halo\}=10{\textasciicircum}\{11.5\}-10{\textasciicircum}\{12\}\$ \$h{\textasciicircum}\{-1\}{\textbackslash}mathrm\{M\}\_{\textbackslash}odot\$. The
measurement of the evolution of assembly bias along the merger tree
provides a new theoretical perspective to the study of secondary bias.
Our findings, which show a tight relationship between halo accretion and
both the clustering and the observational properties of the galaxy
population, have also important implications for the generation of mock
catalogues for upcoming cosmological surveys.},
urldate = {2021-05-16},
journal = {arXiv e-prints},
author = {Montero-Dorta, Antonio D. and Chaves-Montero, Jonás and Artale, M. Celeste and Favole, Ginevra},
month = may,
year = {2021},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {arXiv:2105.05274},
}
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We first show that several halo and galaxy properties strongly correlate with the slope of the sMAH (\\${\\textbackslash}beta\\$) at fixed halo mass. Namely, haloes with increasingly steeper \\${\\textbackslash}beta\\$ increment their halo masses faster at early times, and their hosted galaxies present larger stellar-to-halo mass ratios, lose their gas faster, reach the peak of their star formation histories at higher redshift, and become quenched earlier. We also demonstrate that \\${\\textbackslash}beta\\$ is more directly connected to these key galaxy formation properties than other broadly employed halo proxies, such as formation time. Finally, we measure the secondary dependence of galaxy clustering on \\${\\textbackslash}beta\\$ at fixed halo mass as a function of redshift. By tracing back the evolution of individual haloes, we show that the amplitude of the galaxy assembly bias signal for the progenitors of \\$z=0\\$ galaxies increases with redshift, reaching a factor of 2 at \\$z = 1\\$ for haloes of \\$M_{\\textbackslash}mathrm\\{halo\\}=10{\\textasciicircum}\\{11.5\\}-10{\\textasciicircum}\\{12\\}\\$ \\$h{\\textasciicircum}\\{-1\\}{\\textbackslash}mathrm\\{M\\}_{\\textbackslash}odot\\$. The measurement of the evolution of assembly bias along the merger tree provides a new theoretical perspective to the study of secondary bias. Our findings, which show a tight relationship between halo accretion and both the clustering and the observational properties of the galaxy population, have also important implications for the generation of mock catalogues for upcoming cosmological surveys.","urldate":"2021-05-16","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Montero-Dorta"],"firstnames":["Antonio","D."],"suffixes":[]},{"propositions":[],"lastnames":["Chaves-Montero"],"firstnames":["Jonás"],"suffixes":[]},{"propositions":[],"lastnames":["Artale"],"firstnames":["M.","Celeste"],"suffixes":[]},{"propositions":[],"lastnames":["Favole"],"firstnames":["Ginevra"],"suffixes":[]}],"month":"May","year":"2021","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics","pages":"arXiv:2105.05274","bibtex":"@article{montero-dorta_influence_2021,\n\ttitle = {On the influence of halo mass accretion history on galaxy properties and assembly bias},\n\tvolume = {2105},\n\turl = {http://adsabs.harvard.edu/abs/2021arXiv210505274M},\n\tabstract = {Halo assembly bias is the secondary dependence of the clustering of \ndark-matter haloes on their assembly histories at fixed halo mass. This\nestablished dependence is expected to manifest itself on the clustering\nof the galaxy population, a potential effect commonly known as galaxy\nassembly bias. Using the IllustrisTNG300 magnetohydrodynamical\nsimulation, we analyse the dependence of the properties and clustering\nof galaxies on the shape of the specific mass accretion history of their\nhosting haloes (sMAH). We first show that several halo and galaxy\nproperties strongly correlate with the slope of the sMAH (\\${\\textbackslash}beta\\$) at\nfixed halo mass. Namely, haloes with increasingly steeper \\${\\textbackslash}beta\\$\nincrement their halo masses faster at early times, and their hosted\ngalaxies present larger stellar-to-halo mass ratios, lose their gas\nfaster, reach the peak of their star formation histories at higher\nredshift, and become quenched earlier. We also demonstrate that \\${\\textbackslash}beta\\$\nis more directly connected to these key galaxy formation properties than\nother broadly employed halo proxies, such as formation time. Finally, we\nmeasure the secondary dependence of galaxy clustering on \\${\\textbackslash}beta\\$ at\nfixed halo mass as a function of redshift. By tracing back the evolution\nof individual haloes, we show that the amplitude of the galaxy assembly\nbias signal for the progenitors of \\$z=0\\$ galaxies increases with\nredshift, reaching a factor of 2 at \\$z = 1\\$ for haloes of\n\\$M\\_{\\textbackslash}mathrm\\{halo\\}=10{\\textasciicircum}\\{11.5\\}-10{\\textasciicircum}\\{12\\}\\$ \\$h{\\textasciicircum}\\{-1\\}{\\textbackslash}mathrm\\{M\\}\\_{\\textbackslash}odot\\$. The\nmeasurement of the evolution of assembly bias along the merger tree\nprovides a new theoretical perspective to the study of secondary bias.\nOur findings, which show a tight relationship between halo accretion and\nboth the clustering and the observational properties of the galaxy\npopulation, have also important implications for the generation of mock\ncatalogues for upcoming cosmological surveys.},\n\turldate = {2021-05-16},\n\tjournal = {arXiv e-prints},\n\tauthor = {Montero-Dorta, Antonio D. and Chaves-Montero, Jonás and Artale, M. Celeste and Favole, Ginevra},\n\tmonth = may,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},\n\tpages = {arXiv:2105.05274},\n}\n\n","author_short":["Montero-Dorta, A. D.","Chaves-Montero, J.","Artale, M. 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