Evolution of Disc Thickness in High-Redshift Galaxies. Meng, X. & Gnedin, O. Y. arXiv e-prints, 2006:arXiv:2006.10642, June, 2020. ![Evolution of Disc Thickness in High-Redshift Galaxies [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We study the growth of stellar discs of Milky Way-sized galaxies using a suite of cosmological simulations. We calculate the half-mass axis lengths and axis ratios of stellar populations split by age in isolated galaxies with stellar mass \$M_* = 10{\textasciicircum}7 - 10{\textasciicircum}\{10\} M_\{{\textbackslash}odot\}\$ at redshifts \$z\$ \textgreater 1.5. We find that in our simulations stars always form in relatively thin discs, and at ages below 100 Myr are contained within half-mass height \$z_\{1/2\}\$ \textasciitilde 0.1 kpc and short-to-long axis ratio \$z_\{1/2\}/x_\{1/2\}\$ \textasciitilde 0.15. The disc thickness increases with the age of stellar population, reaching median \$z_\{1/2\}\$ \textasciitilde 0.8 kpc and \$z_\{1/2\}/x_\{1/2\}\$ \textasciitilde 0.6 for stars older than 500 Myr. We trace the same group of stars over the simulation snapshots and show explicitly that their intrinsic shape grows more spheroidal over time. The observed increase in disc thickness is due to the gradual vertical expansion of the originally thin stellar population, combined with the rapidly changing orientation of the galactic plane which mixes the configuration of young stars. The frequently mentioned "upside-down" formation scenario of galactic discs, which posits that young stars form in already thick discs at high redshift, is describing only the final product of this quick disc inflation while missing the actual formation of stars within a fairly thin plane. The location of very young stars in thin discs is due to the correspondingly flat configuration of dense molecular gas that participates in star formation.
@article{meng_evolution_2020,
title = {Evolution of {Disc} {Thickness} in {High}-{Redshift} {Galaxies}},
volume = {2006},
url = {http://adsabs.harvard.edu/abs/2020arXiv200610642M},
abstract = {We study the growth of stellar discs of Milky Way-sized galaxies using a suite of cosmological simulations. We calculate the half-mass axis lengths and axis ratios of stellar populations split by age in isolated galaxies with stellar mass \$M\_* = 10{\textasciicircum}7 - 10{\textasciicircum}\{10\} M\_\{{\textbackslash}odot\}\$ at redshifts \$z\$ {\textgreater} 1.5. We find that in our simulations stars always form in
relatively thin discs, and at ages below 100 Myr are contained within half-mass height \$z\_\{1/2\}\$ {\textasciitilde} 0.1 kpc and short-to-long axis ratio \$z\_\{1/2\}/x\_\{1/2\}\$ {\textasciitilde} 0.15. The disc thickness increases with the age of stellar population, reaching median \$z\_\{1/2\}\$ {\textasciitilde} 0.8 kpc and
\$z\_\{1/2\}/x\_\{1/2\}\$ {\textasciitilde} 0.6 for stars older than 500 Myr. We trace the same group of stars over the simulation snapshots and show explicitly that their intrinsic shape grows more spheroidal over time. The observed increase in disc thickness is due to the gradual vertical expansion of the originally thin stellar population, combined with the rapidly changing orientation of the galactic plane which mixes the configuration of young stars. The frequently mentioned "upside-down" formation scenario of galactic discs, which posits that young stars form in already thick discs at high redshift, is describing only the final product of this quick disc inflation while missing the actual formation of stars within a fairly thin plane. The location of very young stars in thin discs is due to the correspondingly flat configuration of dense molecular gas that participates in star formation.},
urldate = {2020-06-22},
journal = {arXiv e-prints},
author = {Meng, Xi and Gnedin, Oleg Y.},
month = jun,
year = {2020},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {arXiv:2006.10642},
}
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The disc thickness increases with the age of stellar population, reaching median \\$z_\\{1/2\\}\\$ \\textasciitilde 0.8 kpc and \\$z_\\{1/2\\}/x_\\{1/2\\}\\$ \\textasciitilde 0.6 for stars older than 500 Myr. We trace the same group of stars over the simulation snapshots and show explicitly that their intrinsic shape grows more spheroidal over time. The observed increase in disc thickness is due to the gradual vertical expansion of the originally thin stellar population, combined with the rapidly changing orientation of the galactic plane which mixes the configuration of young stars. The frequently mentioned \"upside-down\" formation scenario of galactic discs, which posits that young stars form in already thick discs at high redshift, is describing only the final product of this quick disc inflation while missing the actual formation of stars within a fairly thin plane. 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We calculate the half-mass axis lengths and axis ratios of stellar populations split by age in isolated galaxies with stellar mass \\$M\\_* = 10{\\textasciicircum}7 - 10{\\textasciicircum}\\{10\\} M\\_\\{{\\textbackslash}odot\\}\\$ at redshifts \\$z\\$ {\\textgreater} 1.5. We find that in our simulations stars always form in\nrelatively thin discs, and at ages below 100 Myr are contained within half-mass height \\$z\\_\\{1/2\\}\\$ {\\textasciitilde} 0.1 kpc and short-to-long axis ratio \\$z\\_\\{1/2\\}/x\\_\\{1/2\\}\\$ {\\textasciitilde} 0.15. The disc thickness increases with the age of stellar population, reaching median \\$z\\_\\{1/2\\}\\$ {\\textasciitilde} 0.8 kpc and\n\\$z\\_\\{1/2\\}/x\\_\\{1/2\\}\\$ {\\textasciitilde} 0.6 for stars older than 500 Myr. We trace the same group of stars over the simulation snapshots and show explicitly that their intrinsic shape grows more spheroidal over time. The observed increase in disc thickness is due to the gradual vertical expansion of the originally thin stellar population, combined with the rapidly changing orientation of the galactic plane which mixes the configuration of young stars. The frequently mentioned \"upside-down\" formation scenario of galactic discs, which posits that young stars form in already thick discs at high redshift, is describing only the final product of this quick disc inflation while missing the actual formation of stars within a fairly thin plane. The location of very young stars in thin discs is due to the correspondingly flat configuration of dense molecular gas that participates in star formation.},\n\turldate = {2020-06-22},\n\tjournal = {arXiv e-prints},\n\tauthor = {Meng, Xi and Gnedin, Oleg Y.},\n\tmonth = jun,\n\tyear = {2020},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:2006.10642},\n}\n\n","author_short":["Meng, X.","Gnedin, O. 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