The “red shelf" of the H$\boldmath\beta$ line in the Seyfert 1 galaxies 
RXS J01177+3637 and HS 0328+05

Véron, Philippe; Gonçalves, A. C.; Véron-Cetty, M. P.

doi:10.1051/0004-6361:20020072

Cited by 33 publications

(26 citation statements)

References 39 publications

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“…We have previousy observed a similar complexity in the case of HS 0328+05 (Véron et al 2002). Weak permitted Ti II lines frequently occur in various types of emission line spectra, especially those with strong bright Fe II lines.…”

Section: The Broad Line System L1supporting

confidence: 59%

The unusual emission line spectrum of I Zw 1

Véron-Cetty¹,

Joly

Véron³

2004

A&A

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289

310

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Abstract. Most Seyfert 1 galaxies show strong Fe II lines in their spectrum having the velocity and width of the broad emission lines. To remove the Fe II contribution in these objects, an accurate template is necessary. We used very high signal-to-noise, medium resolution archive optical spectra of I Zw 1 to build such a template. I Zw 1 is a bright narrow-line Seyfert 1 galaxy. As such it is well suited for a detailed analysis of its emission line spectrum. Furthermore it is known to have a very peculiar spectrum with, in addition to the usual broad and narrow line regions, two emission regions emitting broad and blue shifted [O III] lines making it a peculiarly interesting object. While analysing the spectra, we found that the narrow-line region is, unlike the NLR of most Seyfert 1 galaxies, a very low excitation region dominated by both permitted and forbidden Fe II lines. It is very similar to the emission spectrum of a blob in η Carinae which is a low temperature (T e ∼ 6500 K), relatively high density (N e = 10 6 cm −3 ) cloud. The Fe II lines in this cloud are mainly due to pumping via the stellar continuum radiation field (Verner et al. 2002). We did not succeed in modelling the spectrum of the broad-line region, and we suggest that a non radiative heating mechanism increases the temperature in the excited H I region, thus providing the necessary additional excitation of the Fe II lines. For the low-excitation narrow-line region, we are able to apply boundaries to the physical conditions accounting for the forbidden and permitted Fe II lines (10 6 < N e < 10 7 cm −3 ; 10 −6 < U < 10 −5 ).

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Section: The Broad Line System L1supporting

confidence: 59%

The unusual emission line spectrum of I Zw 1

Véron-Cetty¹,

Joly

Véron³

2004

A&A

Self Cite

289

310

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“…A minor fraction of the objects deviate from the sequence by their positive values of ξ 3 . By inspecting the spectra of these objects one by one by eye, we find that the deviations are mainly a result of contamination at the [O iii] red wing caused by the weak low-ionization emission line He i λ5016 (Véron et al 2002). It is interesting to see that the star-forming galaxies with σ > 2σ inst follow the sequence as well, although most of them have Gaussian line profiles.…”

Section: Line Shape Parameters ξ 3 and ξmentioning

confidence: 93%

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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“…In comparison with the list of Fe II lines given by Sigut & Pradhan (2003), the Fe II template used here gives a better fit to the Fe II lines of the present sample of AGNs. (4) We included the He I λλ4921.93, 5015.68 Å lines (Véron et al 2002), assuming that they originate in the same region, i.e. that they have the same redshift and width.…”

Section: Line Profile Analysismentioning

confidence: 99%

“…Hence, each of them has been fitted by only one Gaussian. On the other hand, we include the He Iλ6678.15 Å and SiIIλ6371 lines (Véron et al 2002), and each line has been represented by one Gaussian. Also, one can expect a contribution of Fe II lines in the Hα wavelength region, but on the bases of the calculation given by Sigut & Pradhan (2003) In the fitting procedure we included these lines assuming that they originate from the same region, i.e.…”

Section: Line Profile Analysismentioning

confidence: 99%

Contribution of the disk emission to the broad emission lines in AGNs: Two-component model

Popović

Mediavilla

Bon

et al. 2004

A&A

116

172

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Abstract. We present an investigation of the structure of the emission line region in a sample of 12 single-peaked Active Galactic Nuclei (AGNs). Using the high resolution Hβ and Hα line profiles observed with the Isaac Newton Telescope (La Palma) we study the substructure in the lines (such as shoulders or bumps) which can indicate a disk or disk-like emission in Broad Line Regions (BLRs). Applying Gaussian analysis we found that both kinds of emission regions, BLR and NLR, are complex. In this sample the narrow [OIII] lines are composites of two components; NLR1 which have random velocities from ∼200 to 500 km s −1 and systematic velocities toward the blue from 20 to 350 km s −1 , and NLR2 with smaller random velocities (∼100−200 km s −1 ) and a redshift corresponding to the cosmological one. The BLR also have complex structure and we apply a two-component model assuming that the line wings originate in a very broad line region (VBLR) and the line core in an intermediate line region (ILR). The VBLR is assumed to be an accretion disk and the ILR a spherical emission region. The model fits very well the Hα and Hβ line profiles of the AGNs.

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The “red shelf" of the H$\boldmath\beta$ line in the Seyfert 1 galaxies RXS J01177+3637 and HS 0328+05

Cited by 33 publications

References 39 publications

The unusual emission line spectrum of I Zw 1

The unusual emission line spectrum of I Zw 1

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

Contribution of the disk emission to the broad emission lines in AGNs: Two-component model

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