Blueshifted [O<scp>iii</scp>] Emission: Indications of a Dynamic Narrow-Line Region

Boroson, Todd A.

doi:10.1086/431722

Cited by 165 publications

(192 citation statements)

References 18 publications

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“…The discrepancy remains high even when we account for a potential intrinsic offset Δσ = log(σ * )−log(σ [O iii] ) = 0.11 dex as reported by Ho (2009). However, the robustness of σ [O iii] as a surrogate for σ * is strongly debated as the scatter in the relation is much higher for σ [O iii] than for σ * (Shields et al 2003;Boroson 2005;Greene & Ho 2005a).…”

Section: Is He 2158−0107 An Outlier From the Bh-bulge Relations?mentioning

confidence: 96%

The low-metallicity QSO HE 2158 − 0107: a massive galaxy growing by accretion of nearly pristine gas from its environment?

Wisotzki

Jahnke

Sánchez

2011

A&A

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The metallicities of active galactic nuclei (AGN) are usually well above solar in their narrow-line regions, often reaching up to several times solar in their broad-line regions independent of redshift. Low-metallicity AGN are rare objects that have so far always been associated with low-mass galaxies hosting low-mass black holes (M BH 10 6 M ). We present integral field spectroscopy data of the low-redshift (z = 0.212) quasi-stellar object (QSO) HE 2158−0107 for which we find strong evidence of sub-solar NLR metallicities associated with a massive black hole (M BH ∼ 3 × 10 8 M ). The QSO is surrounded by a large extended emission-line region reaching out to 30 kpc from the QSO in a tail-like geometry. We present optical and near-infrared images and investigate the properties of the host galaxy. The host of HE 2158−0107 is most likely a very compact bulge-dominated galaxy with a size of r e ∼ 1.4 kpc. The multi-colour spectral energy distribution (SED) of the host is quite blue, indicative of a significant young age stellar population formed within the last 1 Gyr. A 3σ upper limit of L bulge,H < 4.5 × 10 10 L ,H for the H-band luminosity and a corresponding stellar mass upper limit of M bulge < 3.4 × 10 10 M show that the host is offset from the local black hole-bulge relations. This is independently supported by the kinematics of the gas. Although the stellar mass of the host galaxy is lower than expected, it cannot explain the exceptionally low metallicity of the gas. We suggest that the extended emission-line region and the galaxy growth are caused by the infall of nearly pristine gas from the environment of the QSO host. Minor mergers of low-metallicity dwarf galaxies or the theoretically predicted smooth accretion of cold (∼ 10 4 K) gas are both potential drivers behind that process. Because the metallicity of the gas in the QSO narrow-line region is much lower than expected, we suspect that the external gas has already reached the galaxy centre and may even contribute to the current feeding of the black hole. HE 2158−0107 appears to represent a particular phase of substantial black hole and galaxy growth that can be observationally linked with the accretion of external material from its environment.

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Section: Is He 2158−0107 An Outlier From the Bh-bulge Relations?mentioning

confidence: 96%

The low-metallicity QSO HE 2158 − 0107: a massive galaxy growing by accretion of nearly pristine gas from its environment?

Wisotzki

Jahnke

Sánchez

2011

A&A

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“…Using a sample of ∼ 400 broad emission-line AGNs selected from the first data release of the SDSS, Boroson (2005) Figure 20 (upper panel). These so called "blue outliers" can provide a valuable tool in the study of the dynamics of NLR and its possible connection with other AGN components.…”

Section: Narrow Emission Linesmentioning

confidence: 99%

A Comprehensive Study of 2000 Narrow Line Seyfert 1 Galaxies from the Sloan Digital Sky Survey. I. The Sample

Zhou

Wang

Yuan

et al. 2006

ASTROPHYS J SUPPL S

308

316

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This is the first paper in a series dedicated to the study of the emission-line and continuum properties of narrow line Seyfert 1 galaxies (NLS1s). We carried out a systematic search for NLS1s from objects assigned as "QSOs" or "galaxies" in the spectroscopic sample of the Sloan Digital Sky Survey Data Release 3 (SDSS DR3) by a careful modeling of their emission lines and continua. The result is a uniform sample comprising ∼ 2 000 NLS1. This sample dramatically increases the number of known NLS1 by a factor of ∼ 10 over previous compilations. This paper presents the parameters of the prominent emission lines and continua, which were measured accurately with typical uncertainties < 10%. Taking advantage of such an unprecedented large and uniform sample with accurately measured spectral parameters, we carried out various statistical analysis, some of which were only possible for the first time. The main results found are as follows.(1) Within the overall Seyfert 1 population, the incidence of NLS1s is strongly dependent on the optical, X-ray, and radio luminosities as well as the radioloudness. The fraction of NLS1 peaks around SDSS g-band absolute magnitude M g ∼ −22 m in the optical and ∼ 10 43.2 erg s −1 in the soft X-ray band, and decreases quickly as the radio-loudness increases. (2) On average the relative FeII emission, R 4570 = F eII(4434 − 4684)/Hβ, in NLS1s is about twice that in normal AGNs, and is anti-correlated with the broad component width of the Balmer emission lines. (3) The well-known anti-correlation between the width of broad low-ionization lines and the soft X-ray spectral slope for broad line AGNs extends down to F W HM ∼ 1 000 km s −1 in NLS1s, but the trend appears to

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“…Nelson et al (2004) found a correlation between the blue asymmetry and Eigenvector-I space by studying the [O iii] λ5007 line profiles of the Palomar-Green quasars. The quasars associated with larger blue asymmetries tend to be stronger Fe ii emitters presumably having larger Eddington ratios (L/L Edd , where L Edd = 1.26 × 10 38 (M BH /M ) erg s −1 is the Eddington luminosity; see also Xu et al 2007;Boroson 2005;Greene & Ho 2005;Mathur & Grupe 2005 Bian et al 2005), but the correlation might not be real (e.g., Aoki et al 2005). Marziani et al (2003) pointed out that all the "blue outliers" have small Hβ line widths (<4000 km s −1 ) and high L/L Edd (see also Zamanov et al 2002;Komossa et al 2008).…”

Section: Introductionmentioning

confidence: 98%

“…The spectroscopic monitor revealed a variability timescale from 1 to 10 years for the blue wings of the [O iii] λ5007 lines in two type I AGNs (IZW 1: Wang et al 2005;NGC 5548: Sergeev et al 1997), which means that the blue wings are likely emitted from the intermediate-line region located between the traditional broadline region and the NLR. In addition to the blue asymmetry, the redshifts of the [O iii] doublets are often found to be negative compared with the redshifts measured from both stellar absorption features and Hβ emission lines (i.e., [O iii] blueshifts; e.g., Phillips 1976;Zamanov et al 2002;Marziani et al 2003;Aoki et al 2005;Boroson 2005;Bian et al 2005;Komossa et al 2008). The rare cases of objects with strong [O iii] blueshifts larger than 100 km s −1 are called "blue outliers.…”

Section: Introductionmentioning

confidence: 99%

Evolution of [O Iii] Λ5007 Emission-Line Profiles in Narrow Emission-Line Galaxies

Wang

Mao

Wei

2011

ApJ

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The active galactic nucleus (AGN)-host co-evolution issue is investigated here by focusing on the evolution of the [O iii] λ5007 emission-line profile. A large sample of narrow emission-line galaxies is selected from the Max-Planck Institute for Astrophysics/Johns Hopkins University Sloan Digital Sky Survey DR7 catalog to simultaneously measure both the [O iii] line profile and circumnuclear stellar population in an individual spectrum. By requiring that (1) the [O iii] line signal-to-noise ratio is larger than 30 and (2) the [O iii] line width is larger than the instrumental resolution by a factor of two, our sample is narrowed down to 2333 Seyfert galaxies/LINERs (AGNs), 793 transition galaxies, and 190 star-forming galaxies. In addition to the commonly used profile parameters (i.e., line centroid, relative velocity shift, and velocity dispersion), two dimensionless shape parameters, skewness and kurtosis, are used to quantify the line shape deviation from a pure Gaussian function. We show that the transition galaxies are systematically associated with narrower line widths and weaker [O iii] broad wings than the AGNs, which implies that the kinematics of emission-line gas are different in the two kinds of objects. By combining the measured host properties and line shape parameters, we find that the AGNs with stronger blue asymmetries tend to be associated with younger stellar populations. However, a similar trend is not identified in the transition galaxies. The failure likely results from a selection effect in which the transition galaxies are systematically associated with younger stellar populations than the AGNs. The evolutionary significance revealed here suggests that both narrow-line region kinematics and outflow feedback in AGNs co-evolve with their host galaxies.

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Blueshifted [Oiii] Emission: Indications of a Dynamic Narrow-Line Region

Cited by 165 publications

References 18 publications

The low-metallicity QSO HE 2158 − 0107: a massive galaxy growing by accretion of nearly pristine gas from its environment?

The low-metallicity QSO HE 2158 − 0107: a massive galaxy growing by accretion of nearly pristine gas from its environment?

A Comprehensive Study of 2000 Narrow Line Seyfert 1 Galaxies from the Sloan Digital Sky Survey. I. The Sample

Evolution of [O Iii] Λ5007 Emission-Line Profiles in Narrow Emission-Line Galaxies

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