Balmer lines emission region in NGC 3516: Kinematical and physical properties

Mediavilla, E.; Kubičela, A.; Jovanović, P.

doi:10.1051/0004-6361:20020724

Cited by 39 publications

(48 citation statements)

References 32 publications

(56 reference statements)

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“…We took the relative strength of these lines from Korista (1992) (Korista 1992;Popović et al 2001Popović et al , 2002Popović et al , 2003. 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.…”

Section: Line Profile Analysismentioning

confidence: 99%

“…The starting point for the inclination can be the relative displacement of redand blue-shifted Gaussians, ∆z. We use the empirical relation given by Smak (1981) (see also Popović et al 2002Popović et al , 2003. If we assume that a disk (or a disk-like) region exists, we can roughly estimate the parameters of the disk using the results of Gaussian analysis and the relationship (see Popović et al 2002 for more details) sin i ≈ ∆z √ 2 · R out , where i is the inclination of the disk, and R out is the outer radius given in gravitational radii.…”

Section: Fitting Proceduresmentioning

confidence: 99%

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

Popović

Mediavilla

Bon

et al. 2004

A&A

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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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Section: Line Profile Analysismentioning

confidence: 99%

Section: Fitting Proceduresmentioning

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

Self Cite

116

172

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“…However, there is the problem that the broad emission lines are complex and that they are probably coming from at least two regions with different kinematical and physical conditions. Furthermore, the broad-emission-line profiles of some AGNs may be explained with a two-component model (see, e.g., Popović et al 2002Popović et al , 2003Popović et al , 2004Ilić et al 2006;Bon et al 2006). …”

Section: Introductionmentioning

confidence: 99%

Detailed Analysis of Balmer Lines in a Sloan Digital Sky Survey Sample of 90 Broad‐Line Active Galactic Nuclei

Mura

Ciroi

Rafanelli

et al. 2007

ApJ

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In order to contribute to the general effort aiming at the improvement of our knowledge about the physical conditions within the broad-line regions ( BLRs) of active galactic nuclei (AGNs), here we present the results achieved by our analysis of the spectral properties of a sample of 90 broad-line-emitting sources, collected from the Sloan Digital Sky Survey database. By focusing our attention mainly on the Balmer series of hydrogen emission lines, which is the dominant feature in the optical wavelength range of many BLR spectra, we extracted several flux and profile measurements, which we related to other source properties, such as optical continuum luminosity, inferred black hole mass, and accretion rate. Using the Boltzmann plot method to investigate the Balmer-line flux ratios as a function of the line profiles, we found that AGNs that emit broader lines typically have larger H/H and smaller H/H and H/H line ratios. With the help of some recent investigations, we model the structure of the BLR, and we study the influence of the accretion process on the properties of BLR plasma.

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“…To limit the number of free parameters in the fit we have set some a priori constraints (see e.g. Popović et al 2002, Popović 2003, taking that all lines have the same red-shift and full widths proportional to their wavelengths. Also, we have linked the intensity ratio of two [OIII] and [NII] lines according to the atomic values (see e.g.…”

Section: Resultsmentioning

confidence: 99%

H II emission line region in LEDA 212995, a small neighboring galaxy of Mrk 1040

et al. 2004

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Abstract. We present here new spectroscopic observations of Mrk 1040 and LEDA 212995 (Mrk 1040 companion) obtained with the Isaac Newton Telescope (INT). The intensity ratios and widths for the narrow emission lines found in LEDA 212995 are typical of H II regions. The red-shift (0.0169±0.00015) of the object derived from these emission lines is very close to the red-shift of Mrk 1040 (z=0.01665). The weak narrow and broad absorption lines were detected in the Hα wavelength band of LEDA 212995 spectra. These absorptions indicate that the companion might be at least partly obscured by Mrk 1040. Using this and previous observations we discuss the possible physical relationship between these two galaxies.

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Balmer lines emission region in NGC 3516: Kinematical and physical properties

Cited by 39 publications

References 32 publications

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

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

Detailed Analysis of Balmer Lines in a Sloan Digital Sky Survey Sample of 90 Broad‐Line Active Galactic Nuclei

H II emission line region in LEDA 212995, a small neighboring galaxy of Mrk 1040

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