A universal relation between the properties of supermassive black holes, galaxies, and dark matter halos. Marasco, A., Cresci, G., Posti, L., Fraternali, F., Mannucci, F., Marconi, A., Belfiore, F., & Fall, S. M. arXiv e-prints, 2105:arXiv:2105.10508, May, 2021. ![A universal relation between the properties of supermassive black holes, galaxies, and dark matter halos [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex We study the relations between the mass of the central black hole (BH) \$M_\{{\textbackslash}rm BH\}\$, the dark matter halo mass \$M_\{{\textbackslash}rm h\}\$, and the stellar-to-halo mass fraction \$f_{\textbackslash}star{\textbackslash}propto M_{\textbackslash}star/M_\{{\textbackslash}rm h\}\$ in a sample of \$55\$ nearby galaxies with dynamically measured \$M_\{p̌hantom{\}}{\textbackslash}rm BHp̌hantom{\{}\}{\textgreater}10{\textasciicircum}6{\textbackslash},\{{\textbackslash}rm M\}_{\textbackslash}odot\$ and \$M_\{{\textbackslash}rm h\}{\textgreater}5{\textbackslash}times10{\textasciicircum}\{11\}{\textbackslash},\{p̌hantom{\}}{\textbackslash}rm Mp̌hantom{\{}\}_{\textbackslash}odot\$. The main improvement with respect to previous studies is that we consider both early- and late-type systems for which \$M_\{{\textbackslash}rm h\}\$ is determined either from globular cluster dynamics or from spatially resolved rotation curves. Independently of their structural properties, galaxies in our sample build a well defined sequence in the \$M_\{p̌hantom{\}}{\textbackslash}rm BHp̌hantom{\{}\}\$-\$M_\{{\textbackslash}rm h\}\$-\$f_{\textbackslash}star\$ space. We find that: (i) \$M_\{{\textbackslash}rm h\}\$ and \$M_\{{\textbackslash}rm BH\}\$ strongly correlate with each other and anti-correlate with \$f_{\textbackslash}star\$; (ii) there is a break in the slope of the \$M_\{p̌hantom{\}}{\textbackslash}rm BHp̌hantom{\{}\}\$-\$M_\{{\textbackslash}rm h\}\$ relation at \$M_\{{\textbackslash}rm h\}\$ of \$10{\textasciicircum}\{12\}{\textbackslash},\{{\textbackslash}rm M\}_{\textbackslash}odot\$, and in the \$f_{\textbackslash}star\$-\$M_\{{\textbackslash}rm BH\}\$ relation at \$M_\{{\textbackslash}rm BH\}\$ of \${\textbackslash}sim10{\textasciicircum}7{\textbackslash}!-{\textbackslash}!10{\textasciicircum}8{\textbackslash},\{{\textbackslash}rm M\}_{\textbackslash}odot\$; (iii) at a fixed \$M_\{{\textbackslash}rm BH\}\$, galaxies with a larger \$f_{\textbackslash}star\$ tend to occupy lighter halos and to have later morphological types. We show that the observed trends can be reproduced by a simple equilibrium model in the \${\textbackslash}Lambda\$CDM framework where galaxies smoothly accrete dark and baryonic matter at a cosmological rate, having their stellar and black hole build-up regulated both by the cooling of the available gas reservoir and by the negative feedback from star formation and active galactic nuclei (AGN). Feature (ii) arises as the BH population transits from a rapidly accreting phase to a more gentle and self-regulated growth, while scatter in the AGN feedback efficiency can account for feature (iii).
@article{marasco_universal_2021,
title = {A universal relation between the properties of supermassive black holes, galaxies, and dark matter halos},
volume = {2105},
url = {http://adsabs.harvard.edu/abs/2021arXiv210510508M},
abstract = {We study the relations between the mass of the central black hole (BH)
\$M\_\{{\textbackslash}rm BH\}\$, the dark matter halo mass \$M\_\{{\textbackslash}rm h\}\$, and the
stellar-to-halo mass fraction \$f\_{\textbackslash}star{\textbackslash}propto M\_{\textbackslash}star/M\_\{{\textbackslash}rm h\}\$ in a
sample of \$55\$ nearby galaxies with dynamically measured \$M\_\{\vphantom{\}}{\textbackslash}rm
BH\vphantom{\{}\}{\textgreater}10{\textasciicircum}6{\textbackslash},\{{\textbackslash}rm M\}\_{\textbackslash}odot\$ and \$M\_\{{\textbackslash}rm h\}{\textgreater}5{\textbackslash}times10{\textasciicircum}\{11\}{\textbackslash},\{\vphantom{\}}{\textbackslash}rm
M\vphantom{\{}\}\_{\textbackslash}odot\$. The main improvement with respect to previous studies is that
we consider both early- and late-type systems for which \$M\_\{{\textbackslash}rm h\}\$ is
determined either from globular cluster dynamics or from spatially
resolved rotation curves. Independently of their structural properties,
galaxies in our sample build a well defined sequence in the \$M\_\{\vphantom{\}}{\textbackslash}rm
BH\vphantom{\{}\}\$-\$M\_\{{\textbackslash}rm h\}\$-\$f\_{\textbackslash}star\$ space. We find that: (i) \$M\_\{{\textbackslash}rm h\}\$ and
\$M\_\{{\textbackslash}rm BH\}\$ strongly correlate with each other and anti-correlate with
\$f\_{\textbackslash}star\$; (ii) there is a break in the slope of the \$M\_\{\vphantom{\}}{\textbackslash}rm
BH\vphantom{\{}\}\$-\$M\_\{{\textbackslash}rm h\}\$ relation at \$M\_\{{\textbackslash}rm h\}\$ of \$10{\textasciicircum}\{12\}{\textbackslash},\{{\textbackslash}rm M\}\_{\textbackslash}odot\$,
and in the \$f\_{\textbackslash}star\$-\$M\_\{{\textbackslash}rm BH\}\$ relation at \$M\_\{{\textbackslash}rm BH\}\$ of
\${\textbackslash}sim10{\textasciicircum}7{\textbackslash}!-{\textbackslash}!10{\textasciicircum}8{\textbackslash},\{{\textbackslash}rm M\}\_{\textbackslash}odot\$; (iii) at a fixed \$M\_\{{\textbackslash}rm BH\}\$,
galaxies with a larger \$f\_{\textbackslash}star\$ tend to occupy lighter halos and to
have later morphological types. We show that the observed trends can be
reproduced by a simple equilibrium model in the \${\textbackslash}Lambda\$CDM framework
where galaxies smoothly accrete dark and baryonic matter at a
cosmological rate, having their stellar and black hole build-up
regulated both by the cooling of the available gas reservoir and by the
negative feedback from star formation and active galactic nuclei (AGN).
Feature (ii) arises as the BH population transits from a rapidly
accreting phase to a more gentle and self-regulated growth, while
scatter in the AGN feedback efficiency can account for feature (iii).},
urldate = {2021-06-04},
journal = {arXiv e-prints},
author = {Marasco, A. and Cresci, G. and Posti, L. and Fraternali, F. and Mannucci, F. and Marconi, A. and Belfiore, F. and Fall, S. M.},
month = may,
year = {2021},
keywords = {Astrophysics - Astrophysics of Galaxies},
pages = {arXiv:2105.10508},
}
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M."],"bibdata":{"bibtype":"article","type":"article","title":"A universal relation between the properties of supermassive black holes, galaxies, and dark matter halos","volume":"2105","url":"http://adsabs.harvard.edu/abs/2021arXiv210510508M","abstract":"We study the relations between the mass of the central black hole (BH) \\$M_\\{{\\textbackslash}rm BH\\}\\$, the dark matter halo mass \\$M_\\{{\\textbackslash}rm h\\}\\$, and the stellar-to-halo mass fraction \\$f_{\\textbackslash}star{\\textbackslash}propto M_{\\textbackslash}star/M_\\{{\\textbackslash}rm h\\}\\$ in a sample of \\$55\\$ nearby galaxies with dynamically measured \\$M_\\{p̌hantom{\\}}{\\textbackslash}rm BHp̌hantom{\\{}\\}{\\textgreater}10{\\textasciicircum}6{\\textbackslash},\\{{\\textbackslash}rm M\\}_{\\textbackslash}odot\\$ and \\$M_\\{{\\textbackslash}rm h\\}{\\textgreater}5{\\textbackslash}times10{\\textasciicircum}\\{11\\}{\\textbackslash},\\{p̌hantom{\\}}{\\textbackslash}rm Mp̌hantom{\\{}\\}_{\\textbackslash}odot\\$. The main improvement with respect to previous studies is that we consider both early- and late-type systems for which \\$M_\\{{\\textbackslash}rm h\\}\\$ is determined either from globular cluster dynamics or from spatially resolved rotation curves. Independently of their structural properties, galaxies in our sample build a well defined sequence in the \\$M_\\{p̌hantom{\\}}{\\textbackslash}rm BHp̌hantom{\\{}\\}\\$-\\$M_\\{{\\textbackslash}rm h\\}\\$-\\$f_{\\textbackslash}star\\$ space. We find that: (i) \\$M_\\{{\\textbackslash}rm h\\}\\$ and \\$M_\\{{\\textbackslash}rm BH\\}\\$ strongly correlate with each other and anti-correlate with \\$f_{\\textbackslash}star\\$; (ii) there is a break in the slope of the \\$M_\\{p̌hantom{\\}}{\\textbackslash}rm BHp̌hantom{\\{}\\}\\$-\\$M_\\{{\\textbackslash}rm h\\}\\$ relation at \\$M_\\{{\\textbackslash}rm h\\}\\$ of \\$10{\\textasciicircum}\\{12\\}{\\textbackslash},\\{{\\textbackslash}rm M\\}_{\\textbackslash}odot\\$, and in the \\$f_{\\textbackslash}star\\$-\\$M_\\{{\\textbackslash}rm BH\\}\\$ relation at \\$M_\\{{\\textbackslash}rm BH\\}\\$ of \\${\\textbackslash}sim10{\\textasciicircum}7{\\textbackslash}!-{\\textbackslash}!10{\\textasciicircum}8{\\textbackslash},\\{{\\textbackslash}rm M\\}_{\\textbackslash}odot\\$; (iii) at a fixed \\$M_\\{{\\textbackslash}rm BH\\}\\$, galaxies with a larger \\$f_{\\textbackslash}star\\$ tend to occupy lighter halos and to have later morphological types. We show that the observed trends can be reproduced by a simple equilibrium model in the \\${\\textbackslash}Lambda\\$CDM framework where galaxies smoothly accrete dark and baryonic matter at a cosmological rate, having their stellar and black hole build-up regulated both by the cooling of the available gas reservoir and by the negative feedback from star formation and active galactic nuclei (AGN). Feature (ii) arises as the BH population transits from a rapidly accreting phase to a more gentle and self-regulated growth, while scatter in the AGN feedback efficiency can account for feature (iii).","urldate":"2021-06-04","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Marasco"],"firstnames":["A."],"suffixes":[]},{"propositions":[],"lastnames":["Cresci"],"firstnames":["G."],"suffixes":[]},{"propositions":[],"lastnames":["Posti"],"firstnames":["L."],"suffixes":[]},{"propositions":[],"lastnames":["Fraternali"],"firstnames":["F."],"suffixes":[]},{"propositions":[],"lastnames":["Mannucci"],"firstnames":["F."],"suffixes":[]},{"propositions":[],"lastnames":["Marconi"],"firstnames":["A."],"suffixes":[]},{"propositions":[],"lastnames":["Belfiore"],"firstnames":["F."],"suffixes":[]},{"propositions":[],"lastnames":["Fall"],"firstnames":["S.","M."],"suffixes":[]}],"month":"May","year":"2021","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:2105.10508","bibtex":"@article{marasco_universal_2021,\n\ttitle = {A universal relation between the properties of supermassive black holes, galaxies, and dark matter halos},\n\tvolume = {2105},\n\turl = {http://adsabs.harvard.edu/abs/2021arXiv210510508M},\n\tabstract = {We study the relations between the mass of the central black hole (BH) \n\\$M\\_\\{{\\textbackslash}rm BH\\}\\$, the dark matter halo mass \\$M\\_\\{{\\textbackslash}rm h\\}\\$, and the\nstellar-to-halo mass fraction \\$f\\_{\\textbackslash}star{\\textbackslash}propto M\\_{\\textbackslash}star/M\\_\\{{\\textbackslash}rm h\\}\\$ in a\nsample of \\$55\\$ nearby galaxies with dynamically measured \\$M\\_\\{\\vphantom{\\}}{\\textbackslash}rm\nBH\\vphantom{\\{}\\}{\\textgreater}10{\\textasciicircum}6{\\textbackslash},\\{{\\textbackslash}rm M\\}\\_{\\textbackslash}odot\\$ and \\$M\\_\\{{\\textbackslash}rm h\\}{\\textgreater}5{\\textbackslash}times10{\\textasciicircum}\\{11\\}{\\textbackslash},\\{\\vphantom{\\}}{\\textbackslash}rm\nM\\vphantom{\\{}\\}\\_{\\textbackslash}odot\\$. The main improvement with respect to previous studies is that\nwe consider both early- and late-type systems for which \\$M\\_\\{{\\textbackslash}rm h\\}\\$ is\ndetermined either from globular cluster dynamics or from spatially\nresolved rotation curves. Independently of their structural properties,\ngalaxies in our sample build a well defined sequence in the \\$M\\_\\{\\vphantom{\\}}{\\textbackslash}rm\nBH\\vphantom{\\{}\\}\\$-\\$M\\_\\{{\\textbackslash}rm h\\}\\$-\\$f\\_{\\textbackslash}star\\$ space. We find that: (i) \\$M\\_\\{{\\textbackslash}rm h\\}\\$ and\n\\$M\\_\\{{\\textbackslash}rm BH\\}\\$ strongly correlate with each other and anti-correlate with\n\\$f\\_{\\textbackslash}star\\$; (ii) there is a break in the slope of the \\$M\\_\\{\\vphantom{\\}}{\\textbackslash}rm\nBH\\vphantom{\\{}\\}\\$-\\$M\\_\\{{\\textbackslash}rm h\\}\\$ relation at \\$M\\_\\{{\\textbackslash}rm h\\}\\$ of \\$10{\\textasciicircum}\\{12\\}{\\textbackslash},\\{{\\textbackslash}rm M\\}\\_{\\textbackslash}odot\\$,\nand in the \\$f\\_{\\textbackslash}star\\$-\\$M\\_\\{{\\textbackslash}rm BH\\}\\$ relation at \\$M\\_\\{{\\textbackslash}rm BH\\}\\$ of\n\\${\\textbackslash}sim10{\\textasciicircum}7{\\textbackslash}!-{\\textbackslash}!10{\\textasciicircum}8{\\textbackslash},\\{{\\textbackslash}rm M\\}\\_{\\textbackslash}odot\\$; (iii) at a fixed \\$M\\_\\{{\\textbackslash}rm BH\\}\\$,\ngalaxies with a larger \\$f\\_{\\textbackslash}star\\$ tend to occupy lighter halos and to\nhave later morphological types. We show that the observed trends can be\nreproduced by a simple equilibrium model in the \\${\\textbackslash}Lambda\\$CDM framework\nwhere galaxies smoothly accrete dark and baryonic matter at a\ncosmological rate, having their stellar and black hole build-up\nregulated both by the cooling of the available gas reservoir and by the\nnegative feedback from star formation and active galactic nuclei (AGN).\nFeature (ii) arises as the BH population transits from a rapidly\naccreting phase to a more gentle and self-regulated growth, while\nscatter in the AGN feedback efficiency can account for feature (iii).},\n\turldate = {2021-06-04},\n\tjournal = {arXiv e-prints},\n\tauthor = {Marasco, A. and Cresci, G. and Posti, L. and Fraternali, F. and Mannucci, F. and Marconi, A. and Belfiore, F. and Fall, S. M.},\n\tmonth = may,\n\tyear = {2021},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies},\n\tpages = {arXiv:2105.10508},\n}\n\n","author_short":["Marasco, A.","Cresci, G.","Posti, L.","Fraternali, F.","Mannucci, F.","Marconi, A.","Belfiore, F.","Fall, S. 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