Host Galaxies and Circumgalactic Environment of “Narrow Line” Seyfert 1 Nuclei

Krongold, Y.; Dultzin‐Hacyan, D.; Marziani, Paola

doi:10.1086/318768

Cited by 58 publications

(54 citation statements)

References 24 publications

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“…We find no significant evidence that NLS1 offset from the M BH − σ * relation of active and inactive galaxies, suggesting that NLS1s and BL AGNs are similar in terms of the current black hole growth. In the case of the host galaxies of NLS1s, there seems no strong difference between the environments of NLS1s and BL AGNs (Krongold et al 2001). Also, NLS1s are not preferentially hosted by merging galaxies (Ryan et al 2007).…”

Section: Nls1s Versus Bl Agnsmentioning

confidence: 90%

The Black Hole Mass–stellar Velocity Dispersion Relation of Narrow-Line Seyfert 1 Galaxies

Woo

Yoon

Park

et al. 2015

ApJ

250

311

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Narrow-line Seyfert 1 galaxies (NLS1s) are arguably one of the key AGN subclasses in investigating the origin of the black hole mass -stellar velocity dispersion (M BH − σ * ) relation because of their high accretion rate and significantly low M BH . Currently, it is under discussion whether present-day NLS1s offset from the M BH − σ * relation. Using the directly measured stellar velocity dispersion of 93 NLS1s at z<0.1, and M BH estimates based on the updated mass estimators, we investigate the M BH − σ * relation of NLS1s in comparison with broad-line AGNs. We find no strong evidence that the NLS1s deviates from the M BH − σ * relation, which is defined by reverberation-mapped type 1 AGNs and quiescent galaxies. However, there is a clear trend of the offset with the host galaxy morphology, i.e., more inclined galaxies toward the line-of-sight have higher stellar velocity dispersion, suggesting that the rotational broadening plays a role in measuring stellar velocity dispersion based on the single-aperture spectra from the Sloan Digital Sky Survey. In addition, we provide the virial factor log f = 0.05 ± 0.12 (f = 1.12), for M BH estimators based on the FWHM of Hβ, by jointly fitting the M BH − σ * relation using quiescent galaxies and reverberation-mapped AGNs.

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Section: Nls1s Versus Bl Agnsmentioning

confidence: 90%

The Black Hole Mass–stellar Velocity Dispersion Relation of Narrow-Line Seyfert 1 Galaxies

Woo

Yoon

Park

et al. 2015

ApJ

250

311

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“…In contrast, the morphology of NLSy1 hosts (i.e., in many ways the "extreme Pop. A" sources) in the local Universe often involves high surface brightness star-forming galaxies (Krongold et al 2001;Ohta et al 2007). They are often barred and/or remarkably perturbed suggesting that they may be young systems sustained by a strong flow of matter toward their central black holes (see e.g.…”

Section: Black Hole Mass and Eddington Ratiomentioning

confidence: 99%

VLT/ISAAC spectra of the Hβ region in intermediate-redshift quasars

Marziani¹,

Sulentic²,

Stirpe³

et al. 2009

A&A

Self Cite

108

187

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Aims. We present new VLT ISAAC spectra for 30 quasars, which we combine with previous data to yield a sample of 53 intermediateredshift (z ≈ 0.9-3.0) sources. The sample is used to explore properties of prominent lines in the hβ spectral region of these very luminous quasars. Methods. We compare this data with two large low-redshift (z < 0.8) samples in a search for trends over almost 6dex in source luminosity.Results. We find two major trends: (1) a systematic increase in minimum FWHM hβ with luminosity (discussed in a previous paper).This lower FWHM envelope is best fit by assuming that the narrowest sources radiate near the Eddington limit, show line emission from a virialized cloud distribution, and obey a well-defined broad line region size vs. luminosity relation. (2) A systematic decrease in equivalent width of [oiii]λλ4959, 5007 (from W ≈ 15 to ∼1 Å) with increasing source bolometric luminosity (from log L bol ≈ 43 to log L bol ≈ 49). Other identified trends require differntiating between so-called Population A and Bsources. We generate median composite spectra in six luminosity bins to maximize S /N. Population A sources show reasonably symmetric Lorentzian hβ profiles at all luminosities, while Pop. B sources require two component fits involving an unshifted broad and a redshifted very broad component.Very broad hβ increases in strength with increasing log L bol , while the broad component remains constant, resulting in an apparent "Baldwin effect" with equivalent width decreasing from W ∼ 80 to ∼20 Å over our sample luminosity range. The roughly constant equivalent width shown by the hβ very broad component implies production in optically-thick, photoionized gas. The onset of the redshifted very broad component appears to be a critical change that occurs near the Pop. A-B boundary at FWHM hβ ≈ 4000 km s −1 , which we relate to a critical Eddington ratio (≈0.2 ± 0.1).

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“…There are indications that the host galaxies of NLS1 and BLS1 galaxies differ, particularly in the sense that large-scale bars are more common in NLS1 galaxies (Crenshaw et al 2003;Ohta et al 2007) and that NLS1 galaxies have more grand-design dust spirals and a higher fraction of nuclear star-forming rings (Deo et al 2006). Moreover, Krongold et al (2001) examined the host galaxies and found that NLS1 galaxies reside in galaxies with smaller diameters than BLS1 galaxies. Previous studies on massYluminosity/sigma relation led to conflicting possibilities; i.e., NLS1 galaxies are hosted by less luminous galaxies (e.g., Wang & Lu 2001;Botte et al 2004Botte et al , 2005, or on the contrary, more luminous galaxies for a given black hole mass (e.g., Mathur et al 2001;Grupe & Mathur 2004;Bian & Zhao 2004;Ryan et al 2007).…”

Section: Ism Of the Host Galaxymentioning

confidence: 99%

The Narrow‐Line Region of Narrow‐Line and Broad‐Line Type 1 Active Galactic Nuclei. I. A Zone of Avoidance in Density

Komossa

Zhou

et al. 2007

ApJ

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The properties of narrow-line Seyfert 1 (NLS1) galaxies, the links and correlations between them, and the physics behind them, are still not well understood. Apart from accretion rates and black hole masses, density and outflows were speculated to be among the main drivers of the NLS1 phenomenon. Here we utilize the diagnostic power of the [S ii] kk6716,6731 intensity ratio to measure the density of the narrow-line region (NLR) systematically and homogeneously for a large sample of NLS1 galaxies, and we perform a comparison with a sample of broad-line type 1 active galactic nuclei (AGNs). We report the discovery of a ''zone of avoidance'' in density in the sense that AGNs with broad lines [FWHM(H ) > 2000 km s À1] avoid low densities, while NLS1 galaxies show a wider distribution in the NLR density, including a significant number of objects with low densities. A correlation analysis further shows that the Eddington ratio L/L Edd anticorrelates with density. We investigate a number of different models for the zone of avoidance in density. Supersolar metallicities and temperature effects, a strong starburst contribution in NLS1 galaxies, different NLR extents, and selective obscuration are considered unlikely. Possible differences in the fraction of matter-bounded clouds, and differences in the interstellar media of the host galaxies of NLS1 galaxies and broad-line Seyfert 1 ( BLS1) galaxies, can only be tested further with future observations. We tentatively favor the effects of winds/outflows, stronger in NLS1 galaxies than in BLS1 galaxies, to explain the observations.

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Host Galaxies and Circumgalactic Environment of “Narrow Line” Seyfert 1 Nuclei

Cited by 58 publications

References 24 publications

The Black Hole Mass–stellar Velocity Dispersion Relation of Narrow-Line Seyfert 1 Galaxies

The Black Hole Mass–stellar Velocity Dispersion Relation of Narrow-Line Seyfert 1 Galaxies

VLT/ISAAC spectra of the Hβ region in intermediate-redshift quasars

The Narrow‐Line Region of Narrow‐Line and Broad‐Line Type 1 Active Galactic Nuclei. I. A Zone of Avoidance in Density

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