On the Nature of Seyfert Galaxies with High [O<scp>iii</scp>] λ5007 Blueshifts

Komossa, Stefanie; Xu, Dawei; Zhou, Hongyan; Storchi‐Bergmann, Thaisa; Binette, L.

doi:10.1086/587932

Cited by 187 publications

(327 citation statements)

References 142 publications

(186 reference statements)

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“…Previous studies frequently identified a strong correlation between the [O iii] line widths and the [O iii] blueshifts (e.g., Bian et al 2005;Komossa et al 2008;Zamanov et al 2002). The correlation is commonly explained by the material outflows.…”

Section: Line Shape Parameters ξ 3 and ξmentioning

confidence: 95%

“…The bulk relative velocity shift of the [O iii] emission line is measured relative to the Hβ emission line in each emission-lineisolated spectrum, because the Hβ line can be easily detected and because the line shows a very small velocity shift relative to the galaxy rest frame (e.g., Komossa et al 2008). The velocity shift is calculated as Δυ = δλ/λ 0 c, where λ 0 and c are the rest-frame wavelength of the [O iii] λ5007 emission line and the velocity of light, respectively.…”

Section: Relative Velocity Shiftsmentioning

confidence: 99%

“…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%

“…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: 99%

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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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Section: Line Shape Parameters ξ 3 and ξmentioning

confidence: 95%

Section: Relative Velocity Shiftsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Wang

Mao

Wei

2011

ApJ

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“…The [O III] λ4959 profile is much broader than the CO profile, FWHM = 2200 ± 180 km s −1 , with a single identifiable peak. Such broad line profiles are commonly interpreted as gas stirred up and accelerated by the AGN in the inner narrowline region (e.g., Komossa et al 2008). This line probes warm ionized gas that is highly excited, but low in mass, unlike the CO lines.…”

Section: Gas Dynamicsmentioning

confidence: 99%

Disk, merger, or outflow? Molecular gas kinematics in two powerful obscured QSOs atz ≥ 3.4

Polletta

Nesvadba

Neri

et al. 2011

A&A

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We report on the detection of bright CO(4-3) line emission in two powerful, obscured quasars discovered in the SWIRE survey, SW022513 and SW022550 at z ≥ 3.4. We analyze the line strength and profile to determine the gas mass, dynamical mass, and the gas dynamics for both galaxies. In SW022513 we may have found the first evidence for a molecular, AGN-driven wind in the early Universe. The line profile in SW022513 is broad (FWHM = 1000 km s −1 ) and blueshifted by −200 km s −1 relative to systemic (where the systemic velocity is estimated from the narrow components of ionized gas lines, as is commonly done for AGN at low and high redshifts). SW022550 has a more regular, double-peaked profile, which is marginally spatially resolved in our data, consistent with either a merger or an extended disk. The molecular gas masses, 4×10 10 M , are large and account for <30% of the stellar mass, making these obscured QSOs as gas rich as other powerful CO emitting galaxies at high redshift, i.e., submillimeter galaxies. Our sources exhibit relatively lower star-formation efficiencies compared to other dusty, powerful starburst galaxies at high redshift. We speculate that this could be a consequence of the AGN perturbing the molecular gas.

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Observational Constraints on the Influence of Active Galactic Nuclei on the Evolution of Galaxies

Harrison¹

2016

Springer Theses

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How to cite: HARRISON, CHRISTOPHER,MARK (2014) Observational constraints on the inuence of active galactic nuclei on the evolution of galaxies, Durham The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source• a link is made to the metadata record in Durham E-Theses• the full-text is not changed in any wayThe full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full Durham E-Theses policy for further details. Observational constraints on the influence of active galactic nuclei on the evolution of galaxies Christopher Mark Harrison AbstractAt the centre of every massive galaxy there resides a super-massive black hole that grew during periods of active galactic nuclei (AGN) activity. Current theoretical models of galaxy evolution invoke AGN-driven galaxy-scale feedback processes (e.g., the expulsion of gas through outflows) in order to reproduce many of the fundamental properties of galaxies and the intergalactic medium. This thesis uses observations to test some of the predictions of these feedback processes. I present integral field unit observations of AGN host galaxies to trace their ionised gas kinematics. The targets are eight high-redshift (z = 1.4 −3.4) ultra-luminous infrared galaxies, that are representative of rapidly evolving distant galaxies, and sixteen z < 0.2 luminous AGN, that were selected from a parent sample of ≈24,000 sources to be representative of the overall population. In both samples I identify galaxy-wide outflows (i.e., over kiloparsec scales), calculate their properties (e.g., mass outflow rates and energetics) and show that they are broadly consistent with theoretical predictions. I find that ionised outflows are common in z < 0.2 luminous AGN and are consistently extended over kiloparsec scales (in ≥ 70% of cases). I also use far-infrared Herschel data of X-ray detected z = 1-3 AGN to test the prediction that luminous AGN shut down star formation in their host galaxies. Using stacking techniques I show that, on average, X-ray detected AGN over a wide range of luminosities (i.e., L 2−8keV ≈ 10 42−45 erg s −1 ) have star formation rates that are consistent with non-active galaxies. This may imply that luminous AGN do not impact upon the star formation in their host galaxies. Overall, this thesis demonstrates that energetic galaxy-wide outflows are prevalent in AGN host galaxies; however, it also demonstrates that we still lack direct observational evidence that luminous AGN are suppressing star formation in their host galaxies.

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On the Nature of Seyfert Galaxies with High [Oiii] λ5007 Blueshifts

Cited by 187 publications

References 142 publications

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

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

Disk, merger, or outflow? Molecular gas kinematics in two powerful obscured QSOs atz ≥ 3.4

Observational Constraints on the Influence of Active Galactic Nuclei on the Evolution of Galaxies

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