BASS XXXV. The $M_{\mathrm{B}\mathrm{H}}$-${\sigma }_{\star }$ Relation of 105-Month Swift-BAT Type 1 AGNs

We present two independent measurements of stellar velocity dispersions ( ${\sigma }_{\star }$ ) from the Ca,H+K & Mg,$\text{textsc}i$ region (3880–5550~Å) and the Calcium Triplet region (CaT, 8350–8750~Å) for 173 hard X-ray-selected Type 1 AGNs ($z\le$ 0.08) from the 105-month Swift-BAT catalog. We construct one of the largest samples of local Type 1 AGNs that have both single-epoch (SE) ‘virial’ black hole mass ($M_{\mathrm{B}\mathrm{H}}$) estimates and ${\sigma }_{\star }$ measurements obtained from high spectral resolution data, allowing us to test the usage of such methods for SMBH studies. We find that the two independent ${\sigma }_{\star }$ measurements are highly consistent with each other, with an average offset of only $0.002\pm 0.001$ dex. Comparing $M_{\mathrm{B}\mathrm{H}}$ estimates based on broad emission lines and stellar velocity dispersion measurements, we find that the former is systematically lower by $\approx$0.12 dex. Consequently, Eddington ratios estimated through broad-line $M_{\mathrm{B}\mathrm{H}}$ determinations are similarly biased (but in the opposite way). We argue that the discrepancy is driven by extinction in the broad-line region (BLR). We also find an anti-correlation between the offset from the $M_{\mathrm{B}\mathrm{H}}$ - ${\sigma }_{\star }$ relation and the Eddington ratio. Our sample of Type 1 AGNs shows a shallower $M_{\mathrm{B}\mathrm{H}}$ - ${\sigma }_{\star }$ relation (with a power law exponent of $\approx$3.5) compared with that of inactive galaxies (with a power-law exponent of $\approx$4.5), confirming earlier results obtained from smaller samples.