@article{munshi_quantifying_2021,
	title = {Quantifying scatter in galaxy formation at the lowest masses},
	volume = {2101},
	url = {http://adsabs.harvard.edu/abs/2021arXiv210105822M},
	abstract = {We predict the stellar mass -- halo mass (SMHM) relationship for dwarf galaxies, using simulated galaxies with peak halo masses of M\$\_\{{\textbackslash}rm peak\} = 10{\textasciicircum}\{11\}\$ M\$\_\{{\textbackslash}odot\}\$ down into the ultra-faint dwarf range to M\$\_\{{\textbackslash}rm peak\} =\$ 10\${\textasciicircum}7\$ M\$\_\{{\textbackslash}odot\}\$. Our simulated dwarfs have stellar masses of M\$\_\{{\textbackslash}rm star\} = \$ 790 M\$\_\{{\textbackslash}odot\}\$ to \$8.2 {\textbackslash}times 10{\textasciicircum}8\$ M\$\_\{{\textbackslash}odot\}\$, with corresponding \$V\$-band magnitudes from \$-2\$ to \$-18.5\$. For M\$\_\{{\textbackslash}rm peak\} {\textgreater} 10{\textasciicircum}\{10\}\$ M\$\_\{{\textbackslash}odot\}\$, the simulated SMHM relationship agrees with literature determinations, including exhibiting a small scatter of 0.3 dex. However, the scatter in the SMHM relation increases for lower-mass halos. We first present results for
well-resolved halos that contain a simulated stellar population, but recognize that whether a halo hosts a galaxy is inherently mass
resolution dependent. We thus adopt a probabilistic model to populate "dark" halos below our resolution limit to predict an "intrinsic" slope and scatter for the SMHM relation. We fit linearly growing log-normal scatter in stellar mass, which grows to more than 1 dex at M\$\_\{{\textbackslash}rm peak\}\$ \$=\$ 10\${\textasciicircum}8\$ M\$\_\{{\textbackslash}odot\}\$. At the faintest end of the SMHM relation probed by our simulations, a galaxy cannot be assigned a unique halo mass based solely on its luminosity. Instead, we provide a formula to stochastically populate low-mass halos following our results. Finally, we show that our growing log-normal scatter steepens the faint-end slope of the predicted stellar mass function.},
	urldate = {2021-02-03},
	journal = {arXiv e-prints},
	author = {Munshi, Ferah and Brooks, Alyson and Applebaum, Elaad and Christensen, Charlotte and Sligh, Jordan P. and Quinn, T.},
	month = jan,
	year = {2021},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {arXiv:2101.05822},
}

{"_id":"BgR9FuvJsR6arAugz","bibbaseid":"munshi-brooks-applebaum-christensen-sligh-quinn-quantifyingscatteringalaxyformationatthelowestmasses-2021","author_short":["Munshi, F.","Brooks, A.","Applebaum, E.","Christensen, C.","Sligh, J. P.","Quinn, T."],"bibdata":{"bibtype":"article","type":"article","title":"Quantifying scatter in galaxy formation at the lowest masses","volume":"2101","url":"http://adsabs.harvard.edu/abs/2021arXiv210105822M","abstract":"We predict the stellar mass – halo mass (SMHM) relationship for dwarf galaxies, using simulated galaxies with peak halo masses of M\\$_\\{{\\textbackslash}rm peak\\} = 10{\\textasciicircum}\\{11\\}\\$ M\\$_\\{{\\textbackslash}odot\\}\\$ down into the ultra-faint dwarf range to M\\$_\\{{\\textbackslash}rm peak\\} =\\$ 10\\${\\textasciicircum}7\\$ M\\$_\\{{\\textbackslash}odot\\}\\$. Our simulated dwarfs have stellar masses of M\\$_\\{{\\textbackslash}rm star\\} = \\$ 790 M\\$_\\{{\\textbackslash}odot\\}\\$ to \\$8.2 {\\textbackslash}times 10{\\textasciicircum}8\\$ M\\$_\\{{\\textbackslash}odot\\}\\$, with corresponding \\$V\\$-band magnitudes from \\$-2\\$ to \\$-18.5\\$. For M\\$_\\{{\\textbackslash}rm peak\\} {\\textgreater} 10{\\textasciicircum}\\{10\\}\\$ M\\$_\\{{\\textbackslash}odot\\}\\$, the simulated SMHM relationship agrees with literature determinations, including exhibiting a small scatter of 0.3 dex. However, the scatter in the SMHM relation increases for lower-mass halos. We first present results for well-resolved halos that contain a simulated stellar population, but recognize that whether a halo hosts a galaxy is inherently mass resolution dependent. We thus adopt a probabilistic model to populate \"dark\" halos below our resolution limit to predict an \"intrinsic\" slope and scatter for the SMHM relation. We fit linearly growing log-normal scatter in stellar mass, which grows to more than 1 dex at M\\$_\\{{\\textbackslash}rm peak\\}\\$ \\$=\\$ 10\\${\\textasciicircum}8\\$ M\\$_\\{{\\textbackslash}odot\\}\\$. At the faintest end of the SMHM relation probed by our simulations, a galaxy cannot be assigned a unique halo mass based solely on its luminosity. Instead, we provide a formula to stochastically populate low-mass halos following our results. Finally, we show that our growing log-normal scatter steepens the faint-end slope of the predicted stellar mass function.","urldate":"2021-02-03","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Munshi"],"firstnames":["Ferah"],"suffixes":[]},{"propositions":[],"lastnames":["Brooks"],"firstnames":["Alyson"],"suffixes":[]},{"propositions":[],"lastnames":["Applebaum"],"firstnames":["Elaad"],"suffixes":[]},{"propositions":[],"lastnames":["Christensen"],"firstnames":["Charlotte"],"suffixes":[]},{"propositions":[],"lastnames":["Sligh"],"firstnames":["Jordan","P."],"suffixes":[]},{"propositions":[],"lastnames":["Quinn"],"firstnames":["T."],"suffixes":[]}],"month":"January","year":"2021","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:2101.05822","bibtex":"@article{munshi_quantifying_2021,\n\ttitle = {Quantifying scatter in galaxy formation at the lowest masses},\n\tvolume = {2101},\n\turl = {http://adsabs.harvard.edu/abs/2021arXiv210105822M},\n\tabstract = {We predict the stellar mass -- halo mass (SMHM) relationship for dwarf galaxies, using simulated galaxies with peak halo masses of M\\$\\_\\{{\\textbackslash}rm peak\\} = 10{\\textasciicircum}\\{11\\}\\$ M\\$\\_\\{{\\textbackslash}odot\\}\\$ down into the ultra-faint dwarf range to M\\$\\_\\{{\\textbackslash}rm peak\\} =\\$ 10\\${\\textasciicircum}7\\$ M\\$\\_\\{{\\textbackslash}odot\\}\\$. Our simulated dwarfs have stellar masses of M\\$\\_\\{{\\textbackslash}rm star\\} = \\$ 790 M\\$\\_\\{{\\textbackslash}odot\\}\\$ to \\$8.2 {\\textbackslash}times 10{\\textasciicircum}8\\$ M\\$\\_\\{{\\textbackslash}odot\\}\\$, with corresponding \\$V\\$-band magnitudes from \\$-2\\$ to \\$-18.5\\$. For M\\$\\_\\{{\\textbackslash}rm peak\\} {\\textgreater} 10{\\textasciicircum}\\{10\\}\\$ M\\$\\_\\{{\\textbackslash}odot\\}\\$, the simulated SMHM relationship agrees with literature determinations, including exhibiting a small scatter of 0.3 dex. However, the scatter in the SMHM relation increases for lower-mass halos. We first present results for\nwell-resolved halos that contain a simulated stellar population, but recognize that whether a halo hosts a galaxy is inherently mass\nresolution dependent. We thus adopt a probabilistic model to populate \"dark\" halos below our resolution limit to predict an \"intrinsic\" slope and scatter for the SMHM relation. We fit linearly growing log-normal scatter in stellar mass, which grows to more than 1 dex at M\\$\\_\\{{\\textbackslash}rm peak\\}\\$ \\$=\\$ 10\\${\\textasciicircum}8\\$ M\\$\\_\\{{\\textbackslash}odot\\}\\$. At the faintest end of the SMHM relation probed by our simulations, a galaxy cannot be assigned a unique halo mass based solely on its luminosity. Instead, we provide a formula to stochastically populate low-mass halos following our results. Finally, we show that our growing log-normal scatter steepens the faint-end slope of the predicted stellar mass function.},\n\turldate = {2021-02-03},\n\tjournal = {arXiv e-prints},\n\tauthor = {Munshi, Ferah and Brooks, Alyson and Applebaum, Elaad and Christensen, Charlotte and Sligh, Jordan P. and Quinn, T.},\n\tmonth = jan,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:2101.05822},\n}\n\n","author_short":["Munshi, F.","Brooks, A.","Applebaum, E.","Christensen, C.","Sligh, J. P.","Quinn, T."],"key":"munshi_quantifying_2021","id":"munshi_quantifying_2021","bibbaseid":"munshi-brooks-applebaum-christensen-sligh-quinn-quantifyingscatteringalaxyformationatthelowestmasses-2021","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2021arXiv210105822M"},"keyword":["Astrophysics - Astrophysics of Galaxies"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies"],"search_terms":["quantifying","scatter","galaxy","formation","lowest","masses","munshi","brooks","applebaum","christensen","sligh","quinn"],"title":"Quantifying scatter in galaxy formation at the lowest masses","year":2021}