@article{bogdan_correlation_2017,
	title = {Correlation {Between} the {Total} {Gravitating} {Mass} of {Groups} and {Clusters} and the {Supermassive} {Black} {Hole} {Mass} of {Brightest} {Galaxies}},
	volume = {1711},
	url = {http://adsabs.harvard.edu/abs/2017arXiv171109900B},
	abstract = {Supermassive black holes (BHs) residing in the brightest cluster 
galaxies are over-massive relative to the stellar bulge mass or central
stellar velocity dispersion of their host galaxy. Since BHs residing at
the bottom of the galaxy cluster's potential well may undergo physical
processes that are driven by the large-scale characteristics of the
galaxy clusters, it is possible that the growth of these BHs is
(indirectly) governed by the properties of their host clusters. In this
work, we explore the connection between the mass of BHs residing in the
brightest group/cluster galaxies (BGGs/BCGs) and the virial temperature,
and hence total gravitating mass, of galaxy groups/clusters. To this
end, we investigate a sample of 17 BGGs/BCGs with dynamical BH mass
measurements, and utilize XMM-Newton X-ray observations to measure the
virial temperatures and infer the \$M\_\{{\textbackslash}rm 500\}\$ mass of the galaxy
groups/clusters. We find that the \$M\_\{{\textbackslash}rm BH\} - kT\$ relation is
significantly tighter and exhibits smaller scatter than the \$M\_\{{\textbackslash}rm BH\}
- M\_\{{\textbackslash}rm bulge\}\$ relations. The best-fitting power law relations are \$
{\textbackslash}log\_\{10\} (M\_\{{\textbackslash}rm BH\}/10{\textasciicircum}\{9\} {\textbackslash} {\textbackslash}rm\{M\_\{{\textbackslash}odot\}\}) = 0.22 + 1.91 {\textbackslash}log\_\{10\}
(kT/1 {\textbackslash} {\textbackslash}rm\{keV\}) \$ and \$ {\textbackslash}log\_\{10\} (M\_\{{\textbackslash}rm BH\}/10{\textasciicircum}\{9\} {\textbackslash} {\textbackslash}rm\{M\_\{{\textbackslash}odot\}\})
= -0.75 + 1.65 {\textbackslash}log\_\{10\} (M\_\{{\textbackslash}rm bulge\}/10{\textasciicircum}\{11\} {\textbackslash} M\_\{{\textbackslash}odot\})\$. Thus, the
BH mass of BGGs/BCGs may be set by physical processes that are governed
by the properties of the host galaxy group/cluster. These results are
confronted with the Horizon-AGN simulation, which reproduces the
observed relations well, albeit the simulated relations exhibit notably
smaller scatter.},
	urldate = {2018-01-03},
	journal = {ArXiv e-prints},
	author = {Bogdan, Akos and Lovisari, Lorenzo and Volonteri, Marta and Dubois, Yohan},
	month = nov,
	year = {2017},
	keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena},
	pages = {arXiv:1711.09900},
}

{"_id":"7YXQkyCCBnZ7BoAPy","bibbaseid":"bogdan-lovisari-volonteri-dubois-correlationbetweenthetotalgravitatingmassofgroupsandclustersandthesupermassiveblackholemassofbrightestgalaxies-2017","author_short":["Bogdan, A.","Lovisari, L.","Volonteri, M.","Dubois, Y."],"bibdata":{"bibtype":"article","type":"article","title":"Correlation Between the Total Gravitating Mass of Groups and Clusters and the Supermassive Black Hole Mass of Brightest Galaxies","volume":"1711","url":"http://adsabs.harvard.edu/abs/2017arXiv171109900B","abstract":"Supermassive black holes (BHs) residing in the brightest cluster galaxies are over-massive relative to the stellar bulge mass or central stellar velocity dispersion of their host galaxy. Since BHs residing at the bottom of the galaxy cluster's potential well may undergo physical processes that are driven by the large-scale characteristics of the galaxy clusters, it is possible that the growth of these BHs is (indirectly) governed by the properties of their host clusters. In this work, we explore the connection between the mass of BHs residing in the brightest group/cluster galaxies (BGGs/BCGs) and the virial temperature, and hence total gravitating mass, of galaxy groups/clusters. To this end, we investigate a sample of 17 BGGs/BCGs with dynamical BH mass measurements, and utilize XMM-Newton X-ray observations to measure the virial temperatures and infer the \\$M_\\{{\\textbackslash}rm 500\\}\\$ mass of the galaxy groups/clusters. We find that the \\$M_\\{{\\textbackslash}rm BH\\} - kT\\$ relation is significantly tighter and exhibits smaller scatter than the \\$M_\\{{\\textbackslash}rm BH\\} - M_\\{{\\textbackslash}rm bulge\\}\\$ relations. The best-fitting power law relations are \\$ {\\textbackslash}log_\\{10\\} (M_\\{{\\textbackslash}rm BH\\}/10{\\textasciicircum}\\{9\\} {\\textbackslash} {\\textbackslash}rm\\{M_\\{{\\textbackslash}odot\\}\\}) = 0.22 + 1.91 {\\textbackslash}log_\\{10\\} (kT/1 {\\textbackslash} {\\textbackslash}rm\\{keV\\}) \\$ and \\$ {\\textbackslash}log_\\{10\\} (M_\\{{\\textbackslash}rm BH\\}/10{\\textasciicircum}\\{9\\} {\\textbackslash} {\\textbackslash}rm\\{M_\\{{\\textbackslash}odot\\}\\}) = -0.75 + 1.65 {\\textbackslash}log_\\{10\\} (M_\\{{\\textbackslash}rm bulge\\}/10{\\textasciicircum}\\{11\\} {\\textbackslash} M_\\{{\\textbackslash}odot\\})\\$. Thus, the BH mass of BGGs/BCGs may be set by physical processes that are governed by the properties of the host galaxy group/cluster. These results are confronted with the Horizon-AGN simulation, which reproduces the observed relations well, albeit the simulated relations exhibit notably smaller scatter.","urldate":"2018-01-03","journal":"ArXiv e-prints","author":[{"propositions":[],"lastnames":["Bogdan"],"firstnames":["Akos"],"suffixes":[]},{"propositions":[],"lastnames":["Lovisari"],"firstnames":["Lorenzo"],"suffixes":[]},{"propositions":[],"lastnames":["Volonteri"],"firstnames":["Marta"],"suffixes":[]},{"propositions":[],"lastnames":["Dubois"],"firstnames":["Yohan"],"suffixes":[]}],"month":"November","year":"2017","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena","pages":"arXiv:1711.09900","bibtex":"@article{bogdan_correlation_2017,\n\ttitle = {Correlation {Between} the {Total} {Gravitating} {Mass} of {Groups} and {Clusters} and the {Supermassive} {Black} {Hole} {Mass} of {Brightest} {Galaxies}},\n\tvolume = {1711},\n\turl = {http://adsabs.harvard.edu/abs/2017arXiv171109900B},\n\tabstract = {Supermassive black holes (BHs) residing in the brightest cluster \ngalaxies are over-massive relative to the stellar bulge mass or central\nstellar velocity dispersion of their host galaxy. Since BHs residing at\nthe bottom of the galaxy cluster's potential well may undergo physical\nprocesses that are driven by the large-scale characteristics of the\ngalaxy clusters, it is possible that the growth of these BHs is\n(indirectly) governed by the properties of their host clusters. In this\nwork, we explore the connection between the mass of BHs residing in the\nbrightest group/cluster galaxies (BGGs/BCGs) and the virial temperature,\nand hence total gravitating mass, of galaxy groups/clusters. To this\nend, we investigate a sample of 17 BGGs/BCGs with dynamical BH mass\nmeasurements, and utilize XMM-Newton X-ray observations to measure the\nvirial temperatures and infer the \\$M\\_\\{{\\textbackslash}rm 500\\}\\$ mass of the galaxy\ngroups/clusters. We find that the \\$M\\_\\{{\\textbackslash}rm BH\\} - kT\\$ relation is\nsignificantly tighter and exhibits smaller scatter than the \\$M\\_\\{{\\textbackslash}rm BH\\}\n- M\\_\\{{\\textbackslash}rm bulge\\}\\$ relations. The best-fitting power law relations are \\$\n{\\textbackslash}log\\_\\{10\\} (M\\_\\{{\\textbackslash}rm BH\\}/10{\\textasciicircum}\\{9\\} {\\textbackslash} {\\textbackslash}rm\\{M\\_\\{{\\textbackslash}odot\\}\\}) = 0.22 + 1.91 {\\textbackslash}log\\_\\{10\\}\n(kT/1 {\\textbackslash} {\\textbackslash}rm\\{keV\\}) \\$ and \\$ {\\textbackslash}log\\_\\{10\\} (M\\_\\{{\\textbackslash}rm BH\\}/10{\\textasciicircum}\\{9\\} {\\textbackslash} {\\textbackslash}rm\\{M\\_\\{{\\textbackslash}odot\\}\\})\n= -0.75 + 1.65 {\\textbackslash}log\\_\\{10\\} (M\\_\\{{\\textbackslash}rm bulge\\}/10{\\textasciicircum}\\{11\\} {\\textbackslash} M\\_\\{{\\textbackslash}odot\\})\\$. Thus, the\nBH mass of BGGs/BCGs may be set by physical processes that are governed\nby the properties of the host galaxy group/cluster. These results are\nconfronted with the Horizon-AGN simulation, which reproduces the\nobserved relations well, albeit the simulated relations exhibit notably\nsmaller scatter.},\n\turldate = {2018-01-03},\n\tjournal = {ArXiv e-prints},\n\tauthor = {Bogdan, Akos and Lovisari, Lorenzo and Volonteri, Marta and Dubois, Yohan},\n\tmonth = nov,\n\tyear = {2017},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena},\n\tpages = {arXiv:1711.09900},\n}\n\n","author_short":["Bogdan, A.","Lovisari, L.","Volonteri, M.","Dubois, Y."],"key":"bogdan_correlation_2017","id":"bogdan_correlation_2017","bibbaseid":"bogdan-lovisari-volonteri-dubois-correlationbetweenthetotalgravitatingmassofgroupsandclustersandthesupermassiveblackholemassofbrightestgalaxies-2017","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2017arXiv171109900B"},"keyword":["Astrophysics - Astrophysics of Galaxies","Astrophysics - High Energy Astrophysical Phenomena"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies","astrophysics - high energy astrophysical phenomena"],"search_terms":["correlation","between","total","gravitating","mass","groups","clusters","supermassive","black","hole","mass","brightest","galaxies","bogdan","lovisari","volonteri","dubois"],"title":"Correlation Between the Total Gravitating Mass of Groups and Clusters and the Supermassive Black Hole Mass of Brightest Galaxies","year":2017}