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

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.

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

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab167 ◽

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.

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Observations of the γ-ray emitting narrow-line Seyfert 1, SBS 0846+513, and its host galaxy

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stab1046 ◽

2021 ◽

Author(s):

Timothy S Hamilton ◽

Marco Berton ◽

Sonia Antón ◽

Lorenzo Busoni ◽

Alessandro Caccianiga ◽

...

Keyword(s):

Black Hole ◽

Adaptive Optics ◽

Host Galaxy ◽

Narrow Line ◽

Black Hole Mass ◽

Residual Structure ◽

Line Region ◽

Resolution Imaging ◽

Γ Ray ◽

Adaptive Optics System

Abstract The γ-ray emitting galaxy SBS 0846 + 513 has been classified as a Narrow-Line Seyfert 1 (NLS1) from its spectroscopy, and on that basis would be thought likely to have a small central black hole hosted in a spiral galaxy. But very few of the γ-ray NLS1 have high-resolution imaging of their hosts, so it is unknown how the morphology expectation holds up for the γ-emitting class. We have observed this galaxy in the J-band with the Large Binocular Telescope’s LUCI1 camera and the ARGOS adaptive optics system. We estimate its black hole mass to lie between $4.2\times 10^7 \le \frac{\text{M}}{\text{M}_\odot } \le 9.7\times 10^7$, using the correlation with bulge luminosity, or $1.9\times 10^7 \le \frac{\text{M}}{\text{M}_\odot } \le 2.4\times 10^7$ using the correlation with Sérsic index. Our favoured estimate is 4.2 × 107M⊙, putting its mass at the high end of the NLS1 range in general but consistent with others that are γ-ray emitters. These estimates are independent of the Broad Line Region viewing geometry and avoid any underestimates due to looking down the jet axis. Its host shows evidence of a bulge + disc structure, from the isophote shape and residual structure in the nuclear-subtracted image. This supports the idea that γ-ray NLS1 may be spiral galaxies, like their non-jetted counterparts.

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Independent Estimation of Black Hole Mass for the γ-ray-detected Archetypal Narrow-line Seyfert 1 Galaxy 1H 0323+342 from X-Ray Variability

The Astrophysical Journal ◽

10.3847/1538-4357/aadd4a ◽

2018 ◽

Vol 866 (1) ◽

pp. 69 ◽

Cited By ~ 7

Author(s):

Hai-Wu Pan ◽

Weimin Yuan ◽

Su Yao ◽

S. Komossa ◽

Chichuan Jin

Keyword(s):

Black Hole ◽

Narrow Line ◽

Black Hole Mass ◽

X Ray ◽

Γ Ray

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Linking the central engine to the jet properties in radio loud AGN

Proceedings of the International Astronomical Union ◽

10.1017/s1743921315002446 ◽

2014 ◽

Vol 10 (S313) ◽

pp. 329-330

Author(s):

A. Olguín-Iglesias ◽

J. León-Tavares ◽

V. Chavushyan ◽

E. Valtaoja ◽

C. Añorve ◽

...

Keyword(s):

Black Hole ◽

Host Galaxy ◽

Base Line ◽

Black Hole Mass ◽

Host Galaxies ◽

Optical Telescope ◽

Central Engine ◽

Early Results ◽

Relativistic Jet ◽

Line Array

AbstractWe explore the connection between the black hole mass and its relativistic jet for a sample of radio-loud AGN (z < 1), in which the relativistic jet parameters are well estimated by means of long term monitoring with the 14m Metsähovi millimeter wave telescope and the Very Long Base-line Array (VLBA). NIR host galaxy images taken with the NOTCam on the Nordic Optical Telescope (NOT) and retrieved from the 2MASS all-sky survey allowed us to perform a detailed surface brightness decomposition of the host galaxies in our sample and to estimate reliable black hole masses via their bulge luminosities. We present early results on the correlations between black hole mass and the relativistic jet parameters. Our preliminary results suggest that the more massive the black hole is, the faster and the more luminous jet it produces.

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Black hole mass and velocity dispersion of narrow line region in active galactic nuclei and narrow line Seyfert 1 galaxies

Astronomy and Astrophysics ◽

10.1051/0004-6361:20011071 ◽

2001 ◽

Vol 377 (1) ◽

pp. 52-59 ◽

Cited By ~ 97

Author(s):

T. Wang ◽

Y. Lu

Keyword(s):

Black Hole ◽

Active Galactic Nuclei ◽

Velocity Dispersion ◽

Galactic Nuclei ◽

Narrow Line ◽

Black Hole Mass ◽

Line Region ◽

Narrow Line Region

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ASCA Observations of Narrow-Line Seyfert 1 Galaxies

International Astronomical Union Colloquium ◽

10.1017/s0252921100039592 ◽

1997 ◽

Vol 159 ◽

pp. 40-43 ◽

Cited By ~ 2

Author(s):

K. Hayashida

Keyword(s):

Black Hole ◽

Narrow Line ◽

Black Hole Mass ◽

Central Black Hole ◽

X Ray ◽

Eddington Limit

AbstractASCA observations of four narrow-line Seyfert 1 galaxies are presented. Among the four sources, two show X-ray spectra consisting of soft and hard components. Rapid X-ray variability is observed in all four sources. We estimate the central black-hole mass of these sources and find indications that the apparent luminosities exceed the Eddington limit under some assumptions.

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Revisiting the Fraction of Radio-Loud Narrow Line Seyfert 1 Galaxies with LoTSS DR1

Universe ◽

10.3390/universe6030045 ◽

2020 ◽

Vol 6 (3) ◽

pp. 45 ◽

Cited By ~ 2

Author(s):

Xu-Liang Fan

Keyword(s):

Black Hole ◽

Detection Rate ◽

Narrow Line ◽

Black Hole Mass ◽

Radio Flux ◽

Central Black Hole ◽

Radio Detection ◽

Lower Redshift

Radio-Loud narrow-line Seyfert 1 galaxies (NLS1s), especially the extremely radio-loud ones, are widely accepted as the jetted versions of NLS1s. We explore the radio-loud fraction for NLS1s with recently released LoTSS DR1 at 150 MHz. The radio detection rate is about 28% for LoTSS DR1. The radio detected NLS1s have lower redshift than the non-detected ones. Moreover, the 150 MHz radio luminosities of NLS1s detected by LoTSS are about two orders of magnitude weaker than those of the previous samples. By defining the radio loudness with the ratio between 150 MHz radio flux and SDSS r band flux, the radio-loud fraction is about 1% with the critical radio loudness equalling 100. Radio loudness shows no dependence on central black hole mass, while weak correlations are found between radio loudness and disk luminosity, as well as Eddington ratio.

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