An Optical Spectroscopic Atlas of Low-Redshift Active Galactic Nuclei

By P. Marziani, J. Sulentic, R. Zamanov, M. Calvani, D. Dultzin-Hacyan, R. Bachev, T. Zwitter. 2003

165 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f5004c2e6dac9e6490fba339523244f062b1f472

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Citations in the corpus

Comparing and Calibrating Black Hole Mass Estimators for Distant Active Galactic Nuclei (2007, background): “The line ratio Hβnarrow / [O III]λ5007 was allowed to range between 1/20 and the maximum value consistent with the absence of “dips” in the broad component (typically 1/10-1/7; e.g. Marziani et al. 2003).”
C IV λ1549 as an Eigenvector 1 Parameter for Active Galactic Nuclei (2007, methodology): “…with references indicated as ESO (unpublished European Southern Observatory spectra), SPM (unpublished spectra obtained with the 2.2 m telescope at San Pedro Martir), M03 (Marziani et al. 2003a),M96 (Marziani et al. 1996), SDSS (spectra retrieved from SDSS Web site), and G99 (Grupe et al. 1999).”
A Systematic Analysis of Fe II Emission in Quasars: Evidence for Inflow to the Central Black Hole (2008, methodology): “…statistical measures of AGN correlations, such as the so-called eigenvector 1 derived from principal component analysis, which is believed to be driven by some fundamental property such as mass accretion rate (e.g., Boroson & Green 1992; Sulentic et al. 2000a, 2000b;Marziani et al. 2001, 2003a).”
A Catalog of Broad Absorption Line Quasars from the Sloan Digital Sky Survey Early Data Release (2003, background): “Most quasars have broadly similar ultraviolet/optical spectra (e.g., Richards et al. 2001, Vanden Berk et al. 2001), but there are several basic trends which lead to considerable variation among quasar spectra (Marziani et al. 2003).”
Central Masses and Broad-Line Region Sizes of Active Galactic Nuclei. II. A Homogeneous Analysis of a Large Reverberation-Mapping Database (2004, unknown): “Most of these values are from Marziani et al. (2003), although in few cases we used our own determinations.”
The Relationship between Luminosity and Broad-Line Region Size in Active Galactic Nuclei (2005, methodology): “The contribution of the narrow component of H was calculated using the H (narrow component)/ [O iii]k5007 line ratio from Marziani et al. (2003), multiplied by the [O iii] k5007 line flux we measured in the data sets in hand.”
Broad-line Balmer decrements in blue active galactic nuclei (2007, background): “…to fit and subtract the AGN continuum and then Fe II multiplets (or the opposite) and finally to fit emission lines (e.g., Boroson & Green 1992, Marziani et al. 2003); or first to fit and subtract simultaneously the continuum and the Fe II emission multiplets (socalled “pseudo-continuum”) and…”
Dust covering factor, silicate emission, and star formation in luminous QSOs (2007, methodology): “9 the latter correlation in terms of PAH(7.7µm) luminosity versus L5100 by using the PAH luminosities from the sample of Schweitzer et al. (2006) and the corresponding optical datafrom Marziani et al. (2003).”
The cosmological evolution of quasar black hole masses (2003, methodology): “For the modelling of the Hβ emission line we have used the optical FeII emission template derived by Marziani et al. (2003), which is made freely available by the authors.”
REVERBERATION MEASUREMENTS OF THE INNER RADIUS OF THE DUST TORUS IN 17 SEYFERT GALAXIES (2014, methodology): “The flux of [O III]λ5007 was compiled from previous research (Boroson & Meyers 1992; Whittle 1992; Kaspi et al. 1996; Marziani et al. 2003; Schmitt et al. 2003; Kaspi et al. 2005), and the flux of [O III]λ4959 was calculated by assuming a theoretical line ratio of [O III]λ5007/[O III]λ4959 = 3.01…”
BAT AGN Spectroscopic Survey. I. Spectral Measurements, Derived Quantities, and AGN Demographics (2017, methodology): “For 18 spectra, we used the low redshift AGN atlas of Marziani et al. (2003), which was obtained using several 2m-class telescopes.”
Black Hole Growth to z = 2 - I: Improved Virial Methods for Measuring M_BH and L/L_Edd (2012, methodology): “We chose 90 sources for which Hβ was reliably measured, by applying our fitting procedure to spectra obtained either from the SDSS or from the catalog of Marziani et al. (2003).”