Dark matter halos and the M-σrelation for supermassive black holes

Abstract

We develop models of two-component spherical galaxies to establish scaling relations linking the properties of spheroids at $z=0$ (total stellar masses, effective radii $R_e$ and velocity dispersions within $R_e$) to the properties of their dark-matter halos at both $z=0$ and higher redshifts. . Our main motivation is the widely accepted idea that the accretion-driven growth of supermassive black holes (SMBHs) in protogalaxies is limited by quasar-mode feedback and gas blow-out. The SMBH masses, $M_{\mathrm{BH}}$, should then be connected to the dark-matter potential wells at the redshift $z_{\mathrm{qso}}$ of the blow-out. We specifically consider the example of a power-law dependence on the maximum circular speed in a protogalactic dark-matter halo: $M_{\mathrm{BH}}\propto V_{\mathrm{d},\mathrm{pk}}^4$, as could be expected if quasar-mode feedback were momentum-driven. For halos with a given $V_{\mathrm{d},\mathrm{pk}}$ at a given $z_{\mathrm{qso}}\ge 0$, our model scaling relations give a typical stellar velocity dispersion ${\sigma }_{\mathrm{ap}}(R_e)$ at $z=0$. Thus, they transform a theoretical $M_{\mathrm{BH}}$-$V_{\mathrm{d},\mathrm{pk}}$ relation into a prediction for an observable $M_{\mathrm{BH}}$-${\sigma }_{\mathrm{ap}}(R_e)$ relation. We find the latter to be distinctly non-linear in log-log space. Its shape depends on the generic redshift-evolution of halos in a {$\Lambda$}CDM cosmology and the systematic variation of stellar-to-dark matter mass fraction at $z=0$, in addition to any assumptions about the physics underlying the $M_{\mathrm{BH}}$-$V_{\mathrm{d},\mathrm{pk}}$ relation. Despite some clear limitations of the form we use for $M_{\mathrm{BH}}$ versus $V_{\mathrm{d},\mathrm{pk}}$, and even though we do not include any SMBH growth through dry mergers at low redshift, our results for $M_{\mathrm{BH}}$-${\sigma }_{\mathrm{ap}}(R_e)$ compare well to data for local early types if we take $z_{\mathrm{qso}}\sim$ 2-4.

arXiv commentAccepted by MNRAS. 20 pages, 6 figures

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