scholarly journals Spectroscopic study of the [O iii]λ5007 profile in Seyfert 1 galaxies

2021 ◽  
Vol 502 (3) ◽  
pp. 3312-3328
Author(s):  
Eduardo O Schmidt ◽  
Laura D Baravalle ◽  
Adriana R Rodríguez-Kamenetzky
Keyword(s):  
Black Hole ◽  
Radial Velocity ◽  
Spectroscopic Study ◽  
Gaussian Function ◽  
Blue Emission ◽  
Emission Lines ◽  
Black Hole Mass ◽  
Velocity Difference ◽  
Full Extension ◽  
Emission Parameter

ABSTRACT The spectra of active galactic nuclei usually exhibit wings in some emission lines, such as [O iii]λλ5007, 4959, with these wings generally being blueshifted and related to strong winds and outflows. The aim of this work was to analyse the [O iii] emission lines in broad-line Seyfert 1 (BLS1) galaxies in order to detect the presence of wings, and to study the [O iii] line properties and their possible connection with the central engine. In addition, we attempted to compare the black hole mass distribution in both BLS1 galaxies with symmetric and blue-asymmetric [O iii] profiles. For this purpose, we carried out a spectroscopic study of a sample of 45 nearby southern BLS1 galaxies from the Six Degree Field Galaxy survey. The [O iii] emission lines were well-fitted using a single Gaussian function in 23 galaxies, while 22 objects presented a wing component and required a double-Gaussian decomposition. By computing the radial velocity difference between the wing and core centroids (i.e. Δv), we found 18 galaxies exhibiting blueshifted wings, 2 objects presenting red wings, and 2 galaxies showing symmetric wings (Δv = 0). Moreover, Δv was slightly correlated with the black hole mass. In addition, we computed the radial velocity difference of the blue-side full extension of the wing relative to the centroid of the core component through the blue emission parameter, which revealed a correlation with black hole mass, in agreement with previous results reported for narrow-line galaxies. Finally, in our sample, similar black hole mass distributions were observed in both BLS1 galaxies with symmetric and blueshifted asymmetric [O iii] profiles.

scholarly journals Asymmetric emission of the [OIII]λ5007 profile in narrow-line Seyfert 1 galaxies

2018 ◽  
Vol 615 ◽  
pp. A13 ◽  
Author(s):  
E. O. Schmidt ◽  
G. A. Oio ◽  
D. Ferreiro ◽  
L. Vega ◽  
W. Weidmann
Keyword(s):  
Black Hole ◽  
Radial Velocity ◽  
Narrow Line ◽  
Black Hole Mass ◽  
Core Component ◽  
Velocity Difference ◽  
Narrow Component ◽  
The Core ◽  
Central Engine ◽  
Blue Wing

Context. Many active galactic nuclei (AGN) and particularly narrow-line Seyfert 1 (NLS1) galaxies, usually exhibit blueshifts and blue wings in several emission lines, which are mainly associated with outflows and strong winds. Although there is no clear evidence of the physical origin of the [OIII] blue wings, it has been suggested that they could be emitted from the inner parts of the narrow-line region (NLR). Aims. In order to study the radial velocity difference between the narrow component of Hβ and the core component of [OIII]λ5007 and the asymmetric emission of this forbidden line, we investigate a sample of NLS1 galaxies. One of the aims of this paper is to analyze the blue wings of the [OIII] 5007 profiles and their relation with the central engine. Methods. We have obtained and studied medium-resolution spectra (190 km s−1 FWHM at Hβ) of a sample of 28 NLS1 galaxies in the optical range 4300–5200 Å. We performed Gaussian decomposition to the Hβ and [OIII]λλ 4959,5007 emission profiles in order to study the distinct components of these lines. Results. A new blue outlier galaxy is found, in which the center of the core component of [OIII] is blueshifted by 405 km s−1 relative to the center of the narrow component of Hβ line. We confirmed a previously known correlation between the blueshift and the full width half maximum (FWHM) of the core component of [OIII]λ5007 line. We also corroborated the correlation between the latter and the velocity of the centroid of the blue wing. On the other hand, by studying the radial velocity difference between the blue end of the asymmetric emission and the centroid of the core component of [OIII], we found a correlation between it and the central black hole mass and, therefore, with the luminosity of the broad component of Hβ. Finally, we found a moderate correlation between the luminosity of the [OIII] blue wing and the black hole mass. Conclusions. These results suggest that the asymmetric emission of the [OIII] lines is related to the central engine, not only through the black hole but also in the intensity of the AGN, which is in agreement with previous results.

scholarly journals An improved test of the binary black hole hypothesis for quasars with double-peaked broad Balmer lines

2019 ◽  
Vol 491 (1) ◽  
pp. 1104-1126 ◽  
Author(s):  
Anh Doan ◽  
Michael Eracleous ◽  
Jessie C Runnoe ◽  
Jia Liu ◽  
Gavin Mathes ◽  
...  
Keyword(s):  
Black Hole ◽  
Radial Velocity ◽  
Measurement Errors ◽  
Process Models ◽  
Emission Lines ◽  
Orbital Parameter ◽  
Physical Parameters ◽  
Orbital Inclination ◽  
Broad Emission ◽  
Balmer Lines

ABSTRACT Velocity offsets in the broad Balmer lines of quasars and their temporal variations serve as indirect evidence for bound supermassive black hole binaries (SBHBs) at sub-parsec separations. In this work, we test the SBHB hypothesis for 14 quasars with double-peaked broad emission lines using their long-term (14–41 yr) radial velocity curves. We improve on the previous work by (i) using elliptical instead of circular orbits for the SBHBs, (ii) adopting a statistical model for radial velocity jitter, (iii) employing a Markov chain Monte Carlo method to explore the orbital parameter space efficiently and build posterior distributions of physical parameters, and (iv) incorporating new observations. We determine empirically that jitter comprises approximately Gaussian distributed fluctuations about the smooth radial velocity curves that are larger than the measurement errors by factors of a few. We initially treat jitter by enlarging the effective error bars and then verify this approach via a variety of Gaussian process models for it. We find lower mass limits for the hypothesized SBHBs in the range 108–1011 M⊙. For seven objects, the SBHB scenario appears unlikely based on goodness-of-fit tests. For two additional objects, the minimum SBHB masses are unreasonably large (>1010 M⊙), strongly disfavouring the SBHB scenario. Using constraints on the orbital inclination angle (which requires some assumptions) makes the minimum masses of four more objects unreasonably large. We also cite physical and observational arguments against the SBHB hypothesis for nine objects. We conclude that the SBHB explanation is not the favoured explanation of double-peaked broad emission lines.

scholarly journals Black hole mass measurement using ALMA observations of [CI] and CO emissions in the Seyfert 1 galaxy NGC 7469

2021 ◽  
Author(s):  
Dieu D Nguyen ◽  
Takuma Izumi ◽  
Sabine Thater ◽  
Masatoshi Imanishi ◽  
Taiki Kawamuro ◽  
...  
Keyword(s):  
Black Hole ◽  
Mass Measurement ◽  
Emission Lines ◽  
Black Hole Mass ◽  
X Ray ◽  
Carbon Abundance ◽  
Line Region ◽  
Order Of Magnitude ◽  
Ngc 7469 ◽  
Co Emission

Abstract We present a supermassive black hole (SMBH) mass measurement in the Seyfert 1 galaxy NGC 7469 using Atacama Large Millimeter/submillimeter Array (ALMA) observations of the atomic-[CI](1-0) and molecular-12CO(1-0) emission lines at the spatial resolution of ≈0${_{.}^{\prime\prime}}$3 (or ≈ 100 pc). These emissions reveal that NGC 7469 hosts a circumnuclear gas disc (CND) with a ring-like structure and a two-arm/bi-symmetric spiral pattern within it, surrounded by a starbursting ring. The CND has a relatively low σgas/V ≈ 0.35 (r ≲ 0${_{.}^{\prime\prime}}$5) and ≈0.19 (r > 0${_{.}^{\prime\prime}}$5), suggesting that the gas is dynamically settled and suitable for dynamically deriving the mass of its central source. As is expected from X-ray dominated region (XDR) effects that dramatically increase an atomic carbon abundance by dissociating CO molecules, we suggest that the atomic [CI](1-0) emission is a better probe of SMBH masses than CO emission in AGNs. Our dynamical model using the [CI](1-0) kinematics yields a $M_{\rm BH}=1.78^{+2.69}_{-1.10}\times 10^7$ M⊙ and $M/L_{\rm F547M}=2.25^{+0.40}_{-0.43}$ (M⊙/L⊙). The model using the 12CO(1-0) kinematics also gives a consistent MBH with a larger uncertainty, up to an order of magnitude, i.e. $M_{\rm BH}=1.60^{+11.52}_{-1.45}\times 10^7$ M⊙. This newly dynamical MBH is ≈ 2 times higher than the mass determined from the reverberation mapped (RM) method using emissions arising in the unresolved broad-line region (BLR). Given this new MBH, we are able to constrain the specific RM dimensionless scaling factor of $f=7.2^{+4.2}_{-3.4}$ for the AGN BLR in NGC 7469. The gas within the unresolved BLR thus has a Keplerian virial velocity component and the inclination of i ≈ 11.0○$_{-2.5}^{+2.2}$, confirming its face-on orientation in a Seyfert 1 AGN by assuming a geometrically thin BLR model.

scholarly journals Active galactic nuclei atz∼ 1.5 – II. Black hole mass estimation by means of broad emission lines

2016 ◽  
Vol 460 (1) ◽  
pp. 187-211 ◽  
Author(s):  
J. E. Mejía-Restrepo ◽  
B. Trakhtenbrot ◽  
P. Lira ◽  
H. Netzer ◽  
D. M. Capellupo
Keyword(s):  
Black Hole ◽  
Active Galactic Nuclei ◽  
Galactic Nuclei ◽  
Emission Lines ◽  
Black Hole Mass ◽  
Mass Estimation ◽  
Broad Emission
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