Black hole mass and cluster mass correlation in cosmological hydro-dynamical simulations

Black hole mass and cluster mass correlation in cosmological hydro-dynamical simulations. Bassini, L., Rasia, E., Borgani, S., Ragone-Figueroa, C., Biffi, V., Dolag, K., Gaspari, M., Granato, G. L., Murante, G., Taffoni, G., & Tornatore, L. arXiv e-prints, 1903:arXiv:1903.03142, March, 2019.

Paper abstract bibtex

Recently, relations connecting the SMBH mass and global properties of the hosting galaxy cluster, such as temperature and mass, were observed. We investigate the correlation between SMBH mass and cluster mass and temperature, their establishment and evolution. We compare their scatter to that of the classical \$M_\{{\textbackslash}rm BH\}-M_\{{\textbackslash}rm BCG\}\$ relation. Moreover, we study how gas accretion and BH-BH mergers contribute to SMBH growth across cosmic time. We employ 135 groups and clusters with a mass range \$1.4{\textbackslash}times 10{\textasciicircum}\{13\}M_\{{\textbackslash}odot\}-2.5{\textbackslash}times 10{\textasciicircum}\{15\} M_\{{\textbackslash}odot\}\$ extracted from a set of 29 zoom-in cosmological hydro-dynamical simulations where the baryonic physics is treated with various sub-grid models, including feedback by active galactic nuclei. In our simulations we find that \$M_\{{\textbackslash}rm BH\}\$ well correlates with \$M_\{500\}\$ and \$T_\{500\}\$, with the scatter around these relations compatible within \$2{\textbackslash}sigma\$ with the scatter around \$M_\{{\textbackslash}rm BH\}-M_\{{\textbackslash}rm BCG\}\$ at \$z=0\$. The \$M_\{p̌hantom{\}}{\textbackslash}rm BHp̌hantom{\{}\}-M_\{500\}\$ relation evolves with time, becoming shallower at lower redshift as a direct consequence of hierarchical structure formation. In our simulations, SMBHs mainly grow by gas accretion at redshift \$z{\textgreater}2\$. At redshift \$z{\textless}1\$ the main growth channel is instead the BH-BH merging. During this last process, substructures hosting BHs are disrupted in the merger process with the BCG and the unbound stars enrich the diffuse stellar component rather than contribute to increase BCG mass. From the results obtained in our simulations with simple sub-grid models we conclude that the scatter around the \$M_\{p̌hantom{\}}{\textbackslash}rm BHp̌hantom{\{}\}-T_\{500\}\$ relation is comparable to the scatter around the \$M_\{p̌hantom{\}}{\textbackslash}rm BHp̌hantom{\{}\}-M_\{{\textbackslash}rm BCG\}\$ relation and that, given the observational difficulties related to the estimation of the BCG mass, clusters temperature and mass can be a useful proxy for the SMBHs mass, especially at high redshift.

@article{bassini_black_2019,
	title = {Black hole mass and cluster mass correlation in cosmological hydro-dynamical simulations},
	volume = {1903},
	url = {http://adsabs.harvard.edu/abs/2019arXiv190303142B},
	abstract = {Recently, relations connecting the SMBH mass and global properties of 
the hosting galaxy cluster, such as temperature and mass, were observed.
We investigate the correlation between SMBH mass and cluster mass and
temperature, their establishment and evolution. We compare their scatter
to that of the classical \$M\_\{{\textbackslash}rm BH\}-M\_\{{\textbackslash}rm BCG\}\$ relation. Moreover, we
study how gas accretion and BH-BH mergers contribute to SMBH growth
across cosmic time. We employ 135 groups and clusters with a mass range
\$1.4{\textbackslash}times 10{\textasciicircum}\{13\}M\_\{{\textbackslash}odot\}-2.5{\textbackslash}times 10{\textasciicircum}\{15\} M\_\{{\textbackslash}odot\}\$ extracted from
a set of 29 zoom-in cosmological hydro-dynamical simulations where the
baryonic physics is treated with various sub-grid models, including
feedback by active galactic nuclei. In our simulations we find that
\$M\_\{{\textbackslash}rm BH\}\$ well correlates with \$M\_\{500\}\$ and \$T\_\{500\}\$, with the
scatter around these relations compatible within \$2{\textbackslash}sigma\$ with the
scatter around \$M\_\{{\textbackslash}rm BH\}-M\_\{{\textbackslash}rm BCG\}\$ at \$z=0\$. The \$M\_\{\vphantom{\}}{\textbackslash}rm
BH\vphantom{\{}\}-M\_\{500\}\$ relation evolves with time, becoming shallower at lower
redshift as a direct consequence of hierarchical structure formation. In
our simulations, SMBHs mainly grow by gas accretion at redshift
\$z{\textgreater}2\$. At redshift \$z{\textless}1\$ the main growth channel is instead the
BH-BH merging. During this last process, substructures hosting BHs are
disrupted in the merger process with the BCG and the unbound stars
enrich the diffuse stellar component rather than contribute to increase
BCG mass. From the results obtained in our simulations with simple
sub-grid models we conclude that the scatter around the \$M\_\{\vphantom{\}}{\textbackslash}rm
BH\vphantom{\{}\}-T\_\{500\}\$ relation is comparable to the scatter around the \$M\_\{\vphantom{\}}{\textbackslash}rm
BH\vphantom{\{}\}-M\_\{{\textbackslash}rm BCG\}\$ relation and that, given the observational difficulties
related to the estimation of the BCG mass, clusters temperature and mass
can be a useful proxy for the SMBHs mass, especially at high redshift.},
	urldate = {2019-03-12},
	journal = {arXiv e-prints},
	author = {Bassini, Luigi and Rasia, Elena and Borgani, Stefano and Ragone-Figueroa, Cinthia and Biffi, Veronica and Dolag, Klaus and Gaspari, Massimo and Granato, Gian Luigi and Murante, Giuseppe and Taffoni, Giuliano and Tornatore, Luca},
	month = mar,
	year = {2019},
	keywords = {Astrophysics - Astrophysics of Galaxies},
	pages = {arXiv:1903.03142},
}

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Moreover, we study how gas accretion and BH-BH mergers contribute to SMBH growth across cosmic time. We employ 135 groups and clusters with a mass range \\$1.4{\\textbackslash}times 10{\\textasciicircum}\\{13\\}M_\\{{\\textbackslash}odot\\}-2.5{\\textbackslash}times 10{\\textasciicircum}\\{15\\} M_\\{{\\textbackslash}odot\\}\\$ extracted from a set of 29 zoom-in cosmological hydro-dynamical simulations where the baryonic physics is treated with various sub-grid models, including feedback by active galactic nuclei. In our simulations we find that \\$M_\\{{\\textbackslash}rm BH\\}\\$ well correlates with \\$M_\\{500\\}\\$ and \\$T_\\{500\\}\\$, with the scatter around these relations compatible within \\$2{\\textbackslash}sigma\\$ with the scatter around \\$M_\\{{\\textbackslash}rm BH\\}-M_\\{{\\textbackslash}rm BCG\\}\\$ at \\$z=0\\$. The \\$M_\\{p̌hantom{\\}}{\\textbackslash}rm BHp̌hantom{\\{}\\}-M_\\{500\\}\\$ relation evolves with time, becoming shallower at lower redshift as a direct consequence of hierarchical structure formation. In our simulations, SMBHs mainly grow by gas accretion at redshift \\$z{\\textgreater}2\\$. At redshift \\$z{\\textless}1\\$ the main growth channel is instead the BH-BH merging. During this last process, substructures hosting BHs are disrupted in the merger process with the BCG and the unbound stars enrich the diffuse stellar component rather than contribute to increase BCG mass. From the results obtained in our simulations with simple sub-grid models we conclude that the scatter around the \\$M_\\{p̌hantom{\\}}{\\textbackslash}rm BHp̌hantom{\\{}\\}-T_\\{500\\}\\$ relation is comparable to the scatter around the \\$M_\\{p̌hantom{\\}}{\\textbackslash}rm BHp̌hantom{\\{}\\}-M_\\{{\\textbackslash}rm BCG\\}\\$ relation and that, given the observational difficulties related to the estimation of the BCG mass, clusters temperature and mass can be a useful proxy for the SMBHs mass, especially at high redshift.","urldate":"2019-03-12","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Bassini"],"firstnames":["Luigi"],"suffixes":[]},{"propositions":[],"lastnames":["Rasia"],"firstnames":["Elena"],"suffixes":[]},{"propositions":[],"lastnames":["Borgani"],"firstnames":["Stefano"],"suffixes":[]},{"propositions":[],"lastnames":["Ragone-Figueroa"],"firstnames":["Cinthia"],"suffixes":[]},{"propositions":[],"lastnames":["Biffi"],"firstnames":["Veronica"],"suffixes":[]},{"propositions":[],"lastnames":["Dolag"],"firstnames":["Klaus"],"suffixes":[]},{"propositions":[],"lastnames":["Gaspari"],"firstnames":["Massimo"],"suffixes":[]},{"propositions":[],"lastnames":["Granato"],"firstnames":["Gian","Luigi"],"suffixes":[]},{"propositions":[],"lastnames":["Murante"],"firstnames":["Giuseppe"],"suffixes":[]},{"propositions":[],"lastnames":["Taffoni"],"firstnames":["Giuliano"],"suffixes":[]},{"propositions":[],"lastnames":["Tornatore"],"firstnames":["Luca"],"suffixes":[]}],"month":"March","year":"2019","keywords":"Astrophysics - Astrophysics of Galaxies","pages":"arXiv:1903.03142","bibtex":"@article{bassini_black_2019,\n\ttitle = {Black hole mass and cluster mass correlation in cosmological hydro-dynamical simulations},\n\tvolume = {1903},\n\turl = {http://adsabs.harvard.edu/abs/2019arXiv190303142B},\n\tabstract = {Recently, relations connecting the SMBH mass and global properties of \nthe hosting galaxy cluster, such as temperature and mass, were observed.\nWe investigate the correlation between SMBH mass and cluster mass and\ntemperature, their establishment and evolution. 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