The black hole mass -- stellar velocity dispersion correlation: bulges versus pseudobulges

Abstract

We investigate the correlation between the supermassive black holes (SMBHs) mass ($M_{\mathrm{bh}}$) and the stellar velocity dispersion (${\sigma }_{\ast }$) in two types of host galaxies: the early-type bulges (disk galaxies with classical bulges or elliptical galaxies) and pseudobulges. In the form $\log (M_{\mathrm{bh}}/{\mathrm{M}}_{\odot })=\alpha +\beta \log ({\sigma }_{\ast }/200\mathrm{km}{\mathrm{s}}^{-1})$, the best-fit results for the 39 early-type bulges are the slope $\beta =4.06\pm 0.28$ and the normalization $\alpha =8.28\pm 0.05$; the best-fit results for the 9 pseudobulges are $\beta =4.5\pm 1.3$, $\alpha =7.50\pm 0.18$. Both relations have intrinsic scatter in $\log M_{\mathrm{bh}}$ of $\lesssim$0.27 dex. The $M_{\mathrm{bh}}$-${\sigma }_{\ast }$ relation for pseudobulges is different from the relation in the early-type bulges over the 3$\sigma$ significance level. The contrasting relations indicate the formation and growth histories of SMBHs depend on their host type. The discrepancy between the slope of the $M_{\mathrm{bh}}$-${\sigma }_{\ast }$ relations using different definition of velocity dispersion vanishes in our sample, a uniform slope will constrain the coevolution theories of the SMBHs and their host galaxies more effectively. We also find the slope for the ``core'' elliptical galaxies at the high mass range of the relation appears steeper ($\beta \simeq$ 5-6), which may be the imprint of their origin of dissipationless mergers.

12 pages, 5 figures, accepted by MNRAS

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