Quasar Host Galaxies and the $M_{SMBH}$ - ${\sigma }_{\ast }$ Relation

Abstract

We analyze the emission line profiles detected in deep optical spectra of quasars to derive the mass of their super-massive black holes (SMBH) following the single-epoch virial method. Our sample consists in 6 radio-loud quasars and 4 radio-quiet quasars. We carefully fit a broad and narrow Gaussian component for each emission line in both the H$\beta$ (10 objects) and H$\alpha$ regions (5 objects). A very good agreement of the derived SMBH masses, $M_{\mathrm{SMBH}}$, is found using the fitted broad H$\beta$ and H$\alpha$ emission lines. We compare our $M_{\mathrm{SMBH}}$ results with those found by previous studies. We study the relationship between the $M_{\mathrm{SMBH}}$ of the quasar and the stellar velocity dispersion, ${\sigma }_{\ast }$, of the host galaxy. We use the measured $M_{\mathrm{SMBH}}$ and ${\sigma }_{\ast }$ to investigate the $M_{\mathrm{SMBH}}$ - ${\sigma }_{\ast }$ relation for both the radio-loud and radio-quiet subsamples. Besides the scatter, we find a good agreement between radio-quiet quasars and AGN+quiescent galaxies and between radio-loud quasars and AGN. Our analysis does not support the hypothesis of using $\sigma$([O III] $\lambda$5007) as a surrogate for stellar velocity dispersions in high-mass, high-luminosity quasars. We also investigate the relationship between the 5 GHz radio-continuum luminosity, $L_{5\mathrm{GHz}}$, of the quasar host galaxy with both $M_{\mathrm{SMBH}}$ and ${\sigma }_{\ast }$. We do not find any correlation between $L_{5\mathrm{GHz}}$ and $M_{\mathrm{SMBH}}$, although we observe a trend that galaxies with larger stellar velocity dispersions have larger $L_{5\mathrm{GHz}}$. Using the results of our fitting for the narrow emission lines of [O III] $\lambda$5007 and [N II] $\lambda$6583 we estimate the gas-phase oxygen abundance of six quasars, being sub-solar in all cases.

Accepted for publication in The Astronomical Journal. 32 pages, 15 figures, 7 tables

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