The unusual emission line spectrum of I Zw 1
By M. Joly, M. Véron-Cetty, P. Véron. Proceedings of the International Astronomical Union, 2003
244 citations recorded by the source corpus.
A detailed analysis of the spectrum of I Zw 1 shows that the Narrow Line Region, unlike that of most Seyfert 1 galaxies, is a very low excitation region dominated by both permitted and forbidden Fe II lines. The physical conditions in this region are discussed.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/b7c02240eaad5977394b51d351f1eb7f9fac0a5f
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Citations in the corpus
- THE LICK AGN MONITORING PROJECT 2011: SPECTROSCOPIC CAMPAIGN AND EMISSION-LINE LIGHT CURVES (2015, methodology): “Fe II: The blends of broad FeII emission were modeled using template spectra, including those described by Boroson & Green (1992), Véron-Cetty et al. (2004), and Kovačevíc et al. (2010).”
- On the Nature of Seyfert Galaxies with High [O III] λ5007 Blueshifts (2008, background): “The presence of a strong [OIII] blueshift on the order of several hundred km s−1 was noticed early in the prototype NLS1 galaxy IZw13 (e.g., Phillips 1976, Véron-Cetty et al. 2004).”
- The Large Sky Area Multi-object Fiber Spectroscopic Telescope (LAMOST) Quasar Survey: The Fourth and Fifth Data Releases (2018, methodology): “The Fe II template from Véron-Cetty et al. (2004) is adopted to model the optical Fe II multiplets.”
- A Systematic Analysis of Fe II Emission in Quasars: Evidence for Inflow to the Central Black Hole (2008, background): “For example, a template of any width can be constructed from the list of Fe lines for I Zw 1 given by Véron-Cetty et al. (2004).”
- A Comprehensive Study of 2000 Narrow Line Seyfert 1 Galaxies from the Sloan Digital Sky Survey. I. The Sample (2006, background): “C(k) denotes the optical Fe ii templates of Véron-Cetty et al. (2004) with the width fixed to that of the broad component of H .”
- A Recoiling Supermassive Black Hole in the Quasar SDSS J092712.65+294344.0? (2008, methodology): “Each emission line was fit by a single Gaussian except the FeII multiplets, which were modeled by templates built from I Zw 1 (λ > 3500 Å, Véron-Cetty et al. 2004; λ < 3500 Å, Tsuzuki et al. 2006).”
- CONSTRAINTS ON BLACK HOLE GROWTH, QUASAR LIFETIMES, AND EDDINGTON RATIO DISTRIBUTIONS FROM THE SDSS BROAD-LINE QUASAR BLACK HOLE MASS FUNCTION (2010, methodology): “Vestergaard et al. (2008) modeled the observed quasar spectra using a power-law continuum, an optical–UV iron line spectrum based on I Zw I (Vestergaard & Wilkes 2001; Véron-Cetty et al. 2004), a Balmer continuum, and host galaxy template (Bruzual & Charlot 2003) for objects at z < 0.5.”
- A Combined Optical and X-ray Study of Unobscured Type 1 AGN. I. Optical Spectra and SED Modeling (2011, background): “1 (one broad-line system, two narrow high-excitation systems and one low-excitation system, Véron-Cetty et al. 2004; Zhou et al. 2006; Mei et al. 2009).”
- Broad-line Balmer decrements in blue active galactic nuclei (2007, methodology): “I ZW1 readily provided by Véron-Cetty et al. (2004), we use two sets of Fe II emission templates in analytical forms constructed from their measurements, one for the broad line system L1 and the other for low-excitation narrow line system N3.”
- ANALYSIS OF OPTICAL Fe ii EMISSION IN A SAMPLE OF ACTIVE GALACTIC NUCLEUS SPECTRA (2010, methodology): “We measured their relative intensities in I Zw 1 which has a wellstudied spectrum (Veron-Cetty et al. 2004), with strong and narrow Fe ii lines.”