We revisit the possibility of redshift evolution in the MBH− * relation with a sample of 22 Seyfert 1 galaxies with black holes (BHs) in the mass range and redshift range 0.03 < z < 0.57 with spectra ...obtained from spatially resolved Keck/Low-resolution Imaging Spectrometer observations. Stellar velocity dispersions were measured directly from the Mg ib region, taking into consideration the effect of Fe ii contamination, active galactic nucleus (AGN) dilution, and host-galaxy morphology on our measurements. BH masses are estimated using the Hβ line width, and the luminosity at 5100 is estimated from surface brightness decomposition of the AGN from the host galaxy using high-resolution imaging from the Hubble Space Telescope. Additionally, we investigate the use of the O iiiλ5007 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 AGNs and lower-mass BHs in the non-local universe than those measured in previous single-epoch studies. We find that any offset in the MBH− * relation up to z ∼ 0.6 is consistent with the scatter of local BH masses, and address the sources of biases and uncertainties that contribute to this scatter.
We present a multiwavelength study of IC 860, a nearby post-starburst galaxy at the early stage of transitioning from blue and star forming to red and quiescent. Optical images reveal a galaxy-wide, ...dusty outflow originating from a compact core. We find evidence for a multiphase outflow in the molecular and neutral gas phase from the CO position-velocity diagram and NaD absorption features. We constrain the neutral mass outflow rate to be ∼0.5 M ⊙ yr−1, and the total hydrogen mass outflow rate to be ∼12 M ⊙ yr−1. Neither outflow component seems able to escape the galaxy. We also find evidence for a recent merger in the optical images, CO spatial distribution, and kinematics, and evidence for a buried active galactic nucleus in the optical emission line ratios, mid-IR properties, and radio spectral shape. The depletion time of the molecular gas reservoir under the current star formation rate is ∼7 Gyr, indicating that the galaxy could stay at the intermediate stage between the blue and red sequence for a long time. Thus the timescales for a significant decline in star formation rate (quenching) and gas depletion are not necessarily the same. Our analysis supports the quenching picture where outflows help suppress star formation by disturbing rather than expelling the gas and shed light on possible ongoing activities in similar quenching galaxies.
Abstract
We revisit the possibility of redshift evolution in the
M
BH
−
σ
*
relation with a sample of 22 Seyfert 1 galaxies with black holes (BHs) in the mass range
and redshift range 0.03 <
z
... < 0.57 with spectra obtained from spatially resolved Keck/Low-resolution Imaging Spectrometer observations. Stellar velocity dispersions were measured directly from the Mg
i
b region, taking into consideration the effect of Fe
ii
contamination, active galactic nucleus (AGN) dilution, and host-galaxy morphology on our measurements. BH masses are estimated using the H
β
line width, and the luminosity at 5100 Å is estimated from surface brightness decomposition of the AGN from the host galaxy using high-resolution imaging from the
Hubble Space Telescope
. Additionally, we investigate the use of the O
iii
λ
5007 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 AGNs 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
BH
−
σ
*
relation up to
z
∼ 0.6 is consistent with the scatter of local BH masses, and address the sources of biases and uncertainties that contribute to this scatter.
Abstract
We present a multiwavelength study of IC 860, a nearby post-starburst galaxy at the early stage of transitioning from blue and star forming to red and quiescent. Optical images reveal a ...galaxy-wide, dusty outflow originating from a compact core. We find evidence for a multiphase outflow in the molecular and neutral gas phase from the CO position–velocity diagram and NaD absorption features. We constrain the neutral mass outflow rate to be ∼0.5
M
⊙
yr
−1
, and the total hydrogen mass outflow rate to be ∼12
M
⊙
yr
−1
. Neither outflow component seems able to escape the galaxy. We also find evidence for a recent merger in the optical images, CO spatial distribution, and kinematics, and evidence for a buried active galactic nucleus in the optical emission line ratios, mid-IR properties, and radio spectral shape. The depletion time of the molecular gas reservoir under the current star formation rate is ∼7 Gyr, indicating that the galaxy could stay at the intermediate stage between the blue and red sequence for a long time. Thus the timescales for a significant decline in star formation rate (
quenching
) and gas depletion are not necessarily the same. Our analysis supports the quenching picture where outflows help suppress star formation by disturbing rather than expelling the gas and shed light on possible ongoing activities in similar quenching galaxies.
We present a multiwavelength study of IC 860, a nearby post-starburst galaxy at the early stage of transitioning from blue and star-forming to red and quiescent. Optical images reveal a galaxy-wide, ...dusty outflow originating from a compact core. We find evidence for a multiphase outflow in the molecular and neutral gas phase from the CO position-velocity diagram and NaD absorption features. We constrain the neutral mass outflow rate to be ~0.5 M\(_{\odot}/\)yr, and the total hydrogen mass outflow rate to be ~12 M\(_{\odot}\)/yr. Neither outflow component seems able to escape the galaxy. We also find evidence for a recent merger in the optical images, CO spatial distribution, and kinematics, and evidence for a buried AGN in the optical emission line ratios, mid-IR properties, and radio spectral shape. The depletion time of the molecular gas reservoir under the current star formation rate is ~7 Gyr, indicating that the galaxy could stay at the intermediate stage between the blue and red sequence for a long time. Thus the timescales for a significant decline in star formation rate ("quenching") and gas depletion are not necessarily the same. Our analysis supports the quenching picture where outflows help suppress star formation by disturbing rather than expelling the gas and shed light on possible ongoing activities in similar quenching galaxies.
We revisit the possibility of redshift evolution in the
$M_{\rm{BH}}-\sigma_*$ 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/Low-Resolution Imaging Spectrometer observations. Stellar velocity
dispersions were measured directly from the Mg Ib region, taking into
consideration the effect of Fe II contamination, active galactic nucleus (AGN)
dilution, and host-galaxy morphology on our measurements. BH masses are
estimated using the H$\beta$ line width, and the luminosity at 5100
$\overset{\lower.5em\circ}{\mathrm{A}}$ is estimated from surface brightness
decomposition of the AGN from the host galaxy using high-resolution imaging
from the Hubble Space Telescope. Additionally, we investigate the use of the 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 AGNs 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 $z\sim0.6$ is consistent with the
scatter of local BH masses, and address the sources of biases and uncertainties
that contribute to this scatter.
We revisit the possibility of redshift evolution in the \(M_{\rm{BH}}-\sigma_*\) 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/Low-Resolution Imaging Spectrometer observations. Stellar velocity dispersions were measured directly from the Mg Ib region, taking into consideration the effect of Fe II contamination, active galactic nucleus (AGN) dilution, and host-galaxy morphology on our measurements. BH masses are estimated using the H\(\beta\) line width, and the luminosity at 5100 \(\overset{\lower.5em\circ}{\mathrm{A}}\) is estimated from surface brightness decomposition of the AGN from the host galaxy using high-resolution imaging from the Hubble Space Telescope. Additionally, we investigate the use of the 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 AGNs 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 \(z\sim0.6\) is consistent with the scatter of local BH masses, and address the sources of biases and uncertainties that contribute to this scatter.
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