Narrow line Seyfert 1 galaxies: where are the broad line regions?

Mao, Weiming; Hu, Chen; Wang, Jian-Min; Bian, Wei-Hao; Zhang, Shu; Zhao, Gang

doi:10.1007/s11433-010-4158-z

Cited by 2 publications

(3 citation statements)

References 22 publications

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“…We note a high correlation between FWHM IC and FWHM BC , with a Pearson correlation coefficient of r p = 0.93. We found for our sample that FWHM BC / FWHM IC is in a range of 2.1 − 3 with a mean value of ∼ 2.5, which is somewhat lower than that obtained by Mao et al (2010) of ∼3 for Hβ . We also performed Kolmogorov-Smirnov (K-S) tests to FWHM BC and FWHM IC , and to FWHM NC and FWHM IC , which give probabilities of P < 10 −5 and P < 10 −8 as being drawn from the same parent distribution, respectively.…”

Section: Final Remarkscontrasting

confidence: 78%

“…An OLS bisector fit gives a slope of ∼ 2.4 with a small (<100 km s −1 ) zero point and a remarkable Pearson correlation coefficient of r p =0.93. We calculated the ratio between the two quantities (bottom left panel), and we find a mean value of FWHM BC /FWHM IC ∼ 2.5, which is somewhat lower than that obtained by Mao et al (2010) of ∼3 for Hβ.…”

Section: The Intermediate Component Of Hαmentioning

confidence: 56%

“…In addition, Crenshaw et al (2009) detected ILR emission with width of 680 km s −1 in the spectrum of NGC 5548. Mao et al (2010) studied a sample of 211 narrow line Seyfert 1 galaxies selected from the SDSS, finding that the Hβ profile can be fitted well by three (narrow, intermediate, and broad) Gaussian components with a ratio FWHM BC / FWHM IC ∼ 3 for the entire sample. Also, they suggested that the intermediate components originate from the inner edge of the torus, which is scaled by dust K-band reverberation.…”

Section: Introductionmentioning

confidence: 99%

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Spectral nuclear properties of NLS1 galaxies

Schmidt

Ferreiro

Neme

et al. 2016

A&A

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Context. It is not yet well known whether narrow line Seyfert 1 (NLS1) galaxies follow the M BH − σ relation found for normal galaxies. Emission lines, such as [SII] On the other hand, we study the properties of the IC of Hα found in 14 galaxies of the sample to find a link between this component, the central engine, and the remaining lines. We also compare the emission among the broad component (BC) of Hα and those emitted at the narrow line region (NLR) to detect differences in the ionizing source in each emitting region. Methods. We have obtained and studied medium-resolution spectra (170 km s −1 FWHM at Hα) of 36 NLS1 galaxies in the optical range ∼5800 -6800Å. We performed a Gaussian decomposition of the Hα+[NII]λλ6548,6584 profile to study the distinct components of Hα and [NII] lines. We also measured the [SII] lines. Results. We obtained black hole (BH) masses in the range log (M BH /M ) = 5.4 − 7.5 for our sample. We found that, in general, most of the galaxies lie below the M BH −σ relation when the NC of Hα and [NII] lines are used as a surrogate of σ . The objects are closer to the relation when [SII] lines are used. Nevertheless, the galaxies are still below this relation and we do not see a clear correlation between the BH masses and FWHM [S II] . Besides this, we found that 13 galaxies show an IC, most of which are in the velocity range ∼ 700 − 1500 km s −1 . This is same range as in AGN types and is well correlated with the FWHM of BC and, therefore, with the BH mass. On the other hand, we found that there is a correlation between the luminosity of the BC of Hα and NC, IC, [NII]λ6584, and [SII] lines.

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Section: Final Remarkscontrasting

confidence: 78%

Section: The Intermediate Component Of Hαmentioning

confidence: 56%

Section: Introductionmentioning

confidence: 99%

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Spectral nuclear properties of NLS1 galaxies

Schmidt

Ferreiro

Neme

et al. 2016

A&A

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The analysis of the iron-rich spectra of a sample of narrow-line Seyfert 1 galaxies

Paul

Winkler

Potter

2022

Monthly Notices of the Royal Astronomical Society

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We analyse medium resolution optical spectra of fourteen Narrow-Line Seyfert 1 galaxies with average to strong iron emission. The targets were observed several times over a 2-year period to probe the nature of spectral variations. Parameters determined from fitting the line profiles include relative strength, width, and asymmetry. We explore the applicability of various profile combinations to Hβ. We achieve satisfactory fits using three components: the narrow and broad components characteristic of all Seyfert 1 galaxies and that are reasonably represented by Gaussian profiles, and an intermediate component with width similar to that of the Fe ii lines. This intermediate component accounted for the largest fraction of the Hβ flux in most of our sample, especially when fitted with a Lorentzian instead of a Gaussian profile. This Lorentzian component improves the overall Hβ fits in most cases. In contrast to many other types of AGN, no dramatic spectral changes were detected in our sample over the two-year period spanning this study, even though some of our targets are known for large and rapid X-ray variability. In particular, we find the variability of the Fe ii lines relative to the Hβ intermediate component to be minimal. For the [O iii] lines we identified asymmetries in almost all our targets well represented by two Gaussians: a primary central and a second blueshifted component. These may signify different gas dynamics connected with nuclear outflow. As in several previous studies, we identify a clear correlation between [O iii] asymmetry and its core component width.

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Narrow line Seyfert 1 galaxies: where are the broad line regions?

Cited by 2 publications

References 22 publications

Spectral nuclear properties of NLS1 galaxies

Spectral nuclear properties of NLS1 galaxies

The analysis of the iron-rich spectra of a sample of narrow-line Seyfert 1 galaxies

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