Stronger Constraints on the Evolution of the $M_{rm{BH}}-sigma_*$ Relation up to $zsim0.6$. (arXiv:1905.05780v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Sexton_R/0/1/0/all/0/1">Remington O. Sexton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Canalizo_G/0/1/0/all/0/1">Gabriela Canalizo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hiner_K/0/1/0/all/0/1">Kyle D. Hiner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Komossa_S/0/1/0/all/0/1">Stefanie Komossa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Woo_J/0/1/0/all/0/1">Jong-Hak Woo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Treister_E/0/1/0/all/0/1">Ezequiel Treister</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dimassimo_S/0/1/0/all/0/1">Sabrina Lyn Hiner Dimassimo</a>
We revisit the possibility of redshift evolution in the We revisit the possibility of redshift evolution in the http://arxiv.org/icons/sfx.gif
$M_{rm{BH}}-sigma_*$ relation with a sample of 22 Seyfert 1 galaxies with
black holes (BHs) in the mass range $10^{6.3}-10^{8.3}~M_odot$ and redshift
range $0.03
$M_{rm{BH}}-sigma_*$ relation with a sample of 22 Seyfert 1 galaxies with
black holes (BHs) in the mass range $10^{6.3}-10^{8.3}~M_odot$ and redshift
range $0.03<z<0.57$ with spectra obtained from spatially-resolved Keck/LRIS
observations. Stellar velocity dispersions were measured directly from the Mg
Ib region, taking into consideration the effect of Fe II contamination, AGN
dilution, and host-galaxy morphology on our measurements. Black hole masses are
estimated using the H$beta$ line width, and the luminosity at 5100
$overset{lower.5emcirc}{mathrm{A}}$ is estimated from surface brightness
decomposition of the active-galactic nucleus (AGN) from the host galaxy using
high-resolution imaging from Hubble Space Telescope. Additionally, we
investigate the use of [O III]$lambda5007$ emission line width as a surrogate
for stellar velocity dispersion, finding better correlation once corrected for
Fe II contamination and any possible blueshifted wing components. Our selection
criteria allowed us to probe lower-luminosity AGN and lower-mass BHs in the
non-local universe than those measured in previous single-epoch studies. We
find that any offset in the $M_{rm{BH}}-sigma_*$ relation up to $zsim0.6$ is
consistent with the scatter of local BH masses, and address the sources of
biases and uncertainties that contribute to this scatter.
