The galaxy-halo size relation of low-mass galaxies in FIRE. Rohr, E., Feldmann, R., Bullock, J., Çatmabacak, O., Boylan-Kolchin, M., Faucher-Giguère, C., Kereš, D., Liang, L., Moreno, J., & Wetzel, A. arXiv:2112.05159 [astro-ph], December, 2021. arXiv: 2112.05159![The galaxy-halo size relation of low-mass galaxies in FIRE [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex Galaxy sizes correlate closely with the sizes of their parent dark matter haloes, suggesting a link between halo formation and galaxy growth. However, the precise nature of this relation and its scatter remains to be understood fully, especially for low-mass galaxies. We analyse the galaxy-halo size relation for low-mass (\$M_{\textbackslash}star {\textbackslash}sim 10{\textasciicircum}\{7-9\} \{{\textbackslash}rm M_{\textbackslash}odot\}\$) central galaxies over the past 12.5 billion years with the help of cosmological volume simulations (FIREbox) from the Feedback in Realistic Environments (FIRE) project. We find a nearly linear relationship between the half-stellar mass galaxy size \$R_\{1/2\}\$ and the parent dark matter halo virial radius \$R_\{{\textbackslash}rm vir\}\$. This relation evolves only weakly since redshift \$z = 5\$: \$R_\{1/2\} \{{\textbackslash}rm kpc\} = (0.053{\textbackslash}pm0.002)(R_\{{\textbackslash}rm vir\}/35 \{{\textbackslash}rm kpc\}){\textasciicircum}\{0.934{\textbackslash}pm0.054\}\$, with a nearly constant scatter \${\textbackslash}langle {\textbackslash}sigma {\textbackslash}rangle = 0.084 [\{{\textbackslash}rm dex\}]\$. Whilst this ratio is similar to what is expected from models where galaxy disc sizes are set by halo angular momentum, the low-mass galaxies in our sample are not angular momentum supported, with stellar rotational to circular velocity ratios \$v_\{{\textbackslash}rm rot\} / v_\{{\textbackslash}rm circ\} {\textbackslash}sim 0.15\$. Introducing redshift as another parameter to the GHSR does not decrease the scatter. Furthermore, this scatter does not correlate with any of the halo properties we investigate – including spin and concentration – suggesting that baryonic processes and feedback physics are instead critical in setting the scatter in the galaxy-halo size relation. Given the relatively small scatter and the weak dependence of the galaxy-halo size relation on redshift and halo properties for these low-mass central galaxies, we propose using galaxy sizes as an independent method from stellar masses to infer halo masses.
@article{rohr_galaxy-halo_2021,
title = {The galaxy-halo size relation of low-mass galaxies in {FIRE}},
url = {http://arxiv.org/abs/2112.05159},
abstract = {Galaxy sizes correlate closely with the sizes of their parent dark matter haloes, suggesting a link between halo formation and galaxy growth. However, the precise nature of this relation and its scatter remains to be understood fully, especially for low-mass galaxies. We analyse the galaxy-halo size relation for low-mass (\$M\_{\textbackslash}star {\textbackslash}sim 10{\textasciicircum}\{7-9\} \{{\textbackslash}rm M\_{\textbackslash}odot\}\$) central galaxies over the past 12.5 billion years with the help of cosmological volume simulations (FIREbox) from the Feedback in Realistic Environments (FIRE) project. We find a nearly linear relationship between the half-stellar mass galaxy size \$R\_\{1/2\}\$ and the parent dark matter halo virial radius \$R\_\{{\textbackslash}rm vir\}\$. This relation evolves only weakly since redshift \$z = 5\$: \$R\_\{1/2\} \{{\textbackslash}rm kpc\} = (0.053{\textbackslash}pm0.002)(R\_\{{\textbackslash}rm vir\}/35 \{{\textbackslash}rm kpc\}){\textasciicircum}\{0.934{\textbackslash}pm0.054\}\$, with a nearly constant scatter \${\textbackslash}langle {\textbackslash}sigma {\textbackslash}rangle = 0.084 [\{{\textbackslash}rm dex\}]\$. Whilst this ratio is similar to what is expected from models where galaxy disc sizes are set by halo angular momentum, the low-mass galaxies in our sample are not angular momentum supported, with stellar rotational to circular velocity ratios \$v\_\{{\textbackslash}rm rot\} / v\_\{{\textbackslash}rm circ\} {\textbackslash}sim 0.15\$. Introducing redshift as another parameter to the GHSR does not decrease the scatter. Furthermore, this scatter does not correlate with any of the halo properties we investigate -- including spin and concentration -- suggesting that baryonic processes and feedback physics are instead critical in setting the scatter in the galaxy-halo size relation. Given the relatively small scatter and the weak dependence of the galaxy-halo size relation on redshift and halo properties for these low-mass central galaxies, we propose using galaxy sizes as an independent method from stellar masses to infer halo masses.},
urldate = {2021-12-17},
journal = {arXiv:2112.05159 [astro-ph]},
author = {Rohr, Eric and Feldmann, Robert and Bullock, James and Çatmabacak, Onur and Boylan-Kolchin, Michael and Faucher-Giguère, Claude-André and Kereš, Dušan and Liang, Lichen and Moreno, Jorge and Wetzel, Andrew},
month = dec,
year = {2021},
note = {arXiv: 2112.05159},
keywords = {Astrophysics - Astrophysics of Galaxies},
}
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We analyse the galaxy-halo size relation for low-mass (\\$M_{\\textbackslash}star {\\textbackslash}sim 10{\\textasciicircum}\\{7-9\\} \\{{\\textbackslash}rm M_{\\textbackslash}odot\\}\\$) central galaxies over the past 12.5 billion years with the help of cosmological volume simulations (FIREbox) from the Feedback in Realistic Environments (FIRE) project. We find a nearly linear relationship between the half-stellar mass galaxy size \\$R_\\{1/2\\}\\$ and the parent dark matter halo virial radius \\$R_\\{{\\textbackslash}rm vir\\}\\$. This relation evolves only weakly since redshift \\$z = 5\\$: \\$R_\\{1/2\\} \\{{\\textbackslash}rm kpc\\} = (0.053{\\textbackslash}pm0.002)(R_\\{{\\textbackslash}rm vir\\}/35 \\{{\\textbackslash}rm kpc\\}){\\textasciicircum}\\{0.934{\\textbackslash}pm0.054\\}\\$, with a nearly constant scatter \\${\\textbackslash}langle {\\textbackslash}sigma {\\textbackslash}rangle = 0.084 [\\{{\\textbackslash}rm dex\\}]\\$. Whilst this ratio is similar to what is expected from models where galaxy disc sizes are set by halo angular momentum, the low-mass galaxies in our sample are not angular momentum supported, with stellar rotational to circular velocity ratios \\$v_\\{{\\textbackslash}rm rot\\} / v_\\{{\\textbackslash}rm circ\\} {\\textbackslash}sim 0.15\\$. Introducing redshift as another parameter to the GHSR does not decrease the scatter. Furthermore, this scatter does not correlate with any of the halo properties we investigate – including spin and concentration – suggesting that baryonic processes and feedback physics are instead critical in setting the scatter in the galaxy-halo size relation. Given the relatively small scatter and the weak dependence of the galaxy-halo size relation on redshift and halo properties for these low-mass central galaxies, we propose using galaxy sizes as an independent method from stellar masses to infer halo masses.","urldate":"2021-12-17","journal":"arXiv:2112.05159 [astro-ph]","author":[{"propositions":[],"lastnames":["Rohr"],"firstnames":["Eric"],"suffixes":[]},{"propositions":[],"lastnames":["Feldmann"],"firstnames":["Robert"],"suffixes":[]},{"propositions":[],"lastnames":["Bullock"],"firstnames":["James"],"suffixes":[]},{"propositions":[],"lastnames":["Çatmabacak"],"firstnames":["Onur"],"suffixes":[]},{"propositions":[],"lastnames":["Boylan-Kolchin"],"firstnames":["Michael"],"suffixes":[]},{"propositions":[],"lastnames":["Faucher-Giguère"],"firstnames":["Claude-André"],"suffixes":[]},{"propositions":[],"lastnames":["Kereš"],"firstnames":["Dušan"],"suffixes":[]},{"propositions":[],"lastnames":["Liang"],"firstnames":["Lichen"],"suffixes":[]},{"propositions":[],"lastnames":["Moreno"],"firstnames":["Jorge"],"suffixes":[]},{"propositions":[],"lastnames":["Wetzel"],"firstnames":["Andrew"],"suffixes":[]}],"month":"December","year":"2021","note":"arXiv: 2112.05159","keywords":"Astrophysics - Astrophysics of Galaxies","bibtex":"@article{rohr_galaxy-halo_2021,\n\ttitle = {The galaxy-halo size relation of low-mass galaxies in {FIRE}},\n\turl = {http://arxiv.org/abs/2112.05159},\n\tabstract = {Galaxy sizes correlate closely with the sizes of their parent dark matter haloes, suggesting a link between halo formation and galaxy growth. However, the precise nature of this relation and its scatter remains to be understood fully, especially for low-mass galaxies. We analyse the galaxy-halo size relation for low-mass (\\$M\\_{\\textbackslash}star {\\textbackslash}sim 10{\\textasciicircum}\\{7-9\\} \\{{\\textbackslash}rm M\\_{\\textbackslash}odot\\}\\$) central galaxies over the past 12.5 billion years with the help of cosmological volume simulations (FIREbox) from the Feedback in Realistic Environments (FIRE) project. We find a nearly linear relationship between the half-stellar mass galaxy size \\$R\\_\\{1/2\\}\\$ and the parent dark matter halo virial radius \\$R\\_\\{{\\textbackslash}rm vir\\}\\$. This relation evolves only weakly since redshift \\$z = 5\\$: \\$R\\_\\{1/2\\} \\{{\\textbackslash}rm kpc\\} = (0.053{\\textbackslash}pm0.002)(R\\_\\{{\\textbackslash}rm vir\\}/35 \\{{\\textbackslash}rm kpc\\}){\\textasciicircum}\\{0.934{\\textbackslash}pm0.054\\}\\$, with a nearly constant scatter \\${\\textbackslash}langle {\\textbackslash}sigma {\\textbackslash}rangle = 0.084 [\\{{\\textbackslash}rm dex\\}]\\$. Whilst this ratio is similar to what is expected from models where galaxy disc sizes are set by halo angular momentum, the low-mass galaxies in our sample are not angular momentum supported, with stellar rotational to circular velocity ratios \\$v\\_\\{{\\textbackslash}rm rot\\} / v\\_\\{{\\textbackslash}rm circ\\} {\\textbackslash}sim 0.15\\$. Introducing redshift as another parameter to the GHSR does not decrease the scatter. 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Given the relatively small scatter and the weak dependence of the galaxy-halo size relation on redshift and halo properties for these low-mass central galaxies, we propose using galaxy sizes as an independent method from stellar masses to infer halo masses.},\n\turldate = {2021-12-17},\n\tjournal = {arXiv:2112.05159 [astro-ph]},\n\tauthor = {Rohr, Eric and Feldmann, Robert and Bullock, James and Çatmabacak, Onur and Boylan-Kolchin, Michael and Faucher-Giguère, Claude-André and Kereš, Dušan and Liang, Lichen and Moreno, Jorge and Wetzel, Andrew},\n\tmonth = dec,\n\tyear = {2021},\n\tnote = {arXiv: 2112.05159},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n}\n\n","author_short":["Rohr, E.","Feldmann, R.","Bullock, J.","Çatmabacak, O.","Boylan-Kolchin, M.","Faucher-Giguère, C.","Kereš, D.","Liang, L.","Moreno, J.","Wetzel, A."],"key":"rohr_galaxy-halo_2021","id":"rohr_galaxy-halo_2021","bibbaseid":"rohr-feldmann-bullock-atmabacak-boylankolchin-fauchergigure-kere-liang-etal-thegalaxyhalosizerelationoflowmassgalaxiesinfire-2021","role":"author","urls":{"Paper":"http://arxiv.org/abs/2112.05159"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["galaxy","halo","size","relation","low","mass","galaxies","fire","rohr","feldmann","bullock","çatmabacak","boylan-kolchin","faucher-giguère","kereš","liang","moreno","wetzel"],"title":"The galaxy-halo size relation of low-mass galaxies in FIRE","year":2021}