Modeling Fe<scp>ii</scp>Emission and Revised Fe<scp>ii</scp>(UV) Empirical Templates for the Seyfert 1 Galaxy I Zw 1

Bruhweiler, F. C.; Verner, E. M.

doi:10.1086/525557

Cited by 118 publications

(180 citation statements)

References 39 publications

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“…The exact parameters of the best theoretical template (model E) are: model with 735 atomic levels, number density n H = 10 11 cm −3 , turbulent velocity v turb = 20 km s −1 , and Φ = 10 20.5 cm −2 s −1 . Interestingly, Bruhweiler & Verner (2008) came to the same conclusion when analysing the I Zw 1 spectrum. Table 2 for model parameters and Fig.…”

Section: Mean Spectrumsupporting

confidence: 52%

“…However, we obtained very interesting results for the theoretical templates of Fe II from Bruhweiler & Verner (2008), which were recently applied to a large sample of SDSS quasars Table 1 for the model parameters. (Marziani et al 2013).…”

Section: Mean Spectrummentioning

confidence: 97%

“…We start with the Vestergaard & Wilkes (2001) template, based on I Zw 1 with zero contribution underlying the Mg II core, and the template of Tsuzuki et al (2006) also based on I Zw 1 but with some Fe II emission underlying Mg II obtained by subtraction of the two Gaussians modeling the Mg II doublet. Next we experiment with purely theoretical templates of Bruhweiler & Verner (2008), calculated for different values of the density, turbulent velocity, and ionization parameter Φ. We allow for Fe II broadening as well as for the shift with respect to Mg II since Fe II was suggested to come from infalling material (Ferland et al 2009).…”

Section: Modelmentioning

confidence: 99%

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SALT long-slit spectroscopy of LBQS 2113-4538: variability of the Mg II and Fe II component

Hryniewicz

Czerny

Pych

et al. 2014

A&A

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Context. The Mg II line is of extreme importance in intermediate redshift quasars since it allows us to measure the black hole mass in these sources and to use these sources as probes of the distribution of dark energy in the Universe, as a complementary tool to SN Ia. Aims. Reliable use of Mg II requires a good understanding of all the systematic effects involved in the measurement of the line properties, including the contamination by Fe II UV emission. Methods. We performed three spectroscopic observations of a quasar LBQS 2113-4538 (z = 0.956) with the SALT telescope, separated in time by several months and we analyze in detail the mean spectrum and the variability in the spectral shape. Results. We show that even in our good-quality spectra the Mg II doublet is well fit by a single Lorentzian shape. We tested several models of the Fe II pseudo-continuum and showed that one of them well represents all the data. The amplitudes of both components vary in time, but the shapes do not change significantly. The measured line width of LBQS 2113-4538 identifies this object as a class A quasar. The upper limit of 3% for the contribution of the narrow line region (NLR) to Mg II may suggest that the separation of the broad line region and NLR disappears in this class of objects.

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Section: Mean Spectrumsupporting

confidence: 52%

Section: Mean Spectrummentioning

confidence: 97%

Section: Modelmentioning

confidence: 99%

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SALT long-slit spectroscopy of LBQS 2113-4538: variability of the Mg II and Fe II component

Hryniewicz

Czerny

Pych

et al. 2014

A&A

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“…We only mention that emission blends near Mgiiλ2800 are mainly due to Feii, which is modeled with the Feii UV emission template provided by the last model in Table 1 in Brühweiler & Verner (2008). The main results presented in this paper were also tested with an additional empirical template produced by Tsuzuki et al (2006).…”

Section: Hβ and Mgiiλ2800 Spectral Rangementioning

confidence: 99%

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

Marziani

Sulentic

Plauchu-Frayn

et al. 2013

A&A

156

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Context. Broad Mgiiλ2800 and Hβ lines have emerged as the most reliable virial estimators of the black hole mass in quasars. Which is more reliable? Part of the challenge centers on comparing Mgiiλ2800 and Hβ line profiles in order to improve the ±1 dex M BH uncertainties inherent in single-epoch FWHM measures from noisy spectra. Aims. We compare Mgiiλ2800 and Hβ profile measures in the same sources and especially FWHM measures that provide the virial broadening estimator. Methods. We identify 680 bright Sloan Digital Sky Survey Data Release 7 quasars with spectra showing both Mgiiλ2800 and Hβ lines at redshift 0.4 ≤ z ≤ 0.75. The S/N of these spectra are high enough to allow binning in the "four-dimensional (4D) eigenvector 1" optical plane and construction of high S/N composite spectra. Results. We confirm that Mgiiλ2800 shows a profile that is ≈20% narrower as suggested in some previous studies. FWHM measures for Population B sources (i.e., with FWHM of Hβ larger than 4000 km s −1 ) are uncertain because they show complex profiles with at least two broad-line components involving a nearly unshifted broad and redshifted very-broad component. Only the broad component is likely to be a valid virial estimator. If Hβ and Mgiiλ2800 are not corrected for the very broad component then black hole mass M BH values for Population B sources will be systematically overestimated by up to Δ logM BH ≈ 0.3−0.4 dex. We suggest a simple correction that can be applied to the majority of sources. Mgiiλ2800 is the safer virial estimator for Population B sources because the centroid shifts with respect to rest frame are lower than for Hβ. In the broad and very broad component profile interpretation, this is a consequence of the lower very broad to broad component intensity ratio for Mgiiλ2800. Eigenvector-based studies show that effective discrimination of black hole mass and Eddington ratio at fixed redshift is not achieved via luminosity binning but rather by binning in a "4D eigenvector 1" context that reflects different broad line region geometry/kinematics probably driven by the Eddington ratio.

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“…They were simultaneously fit along with the continuum and Feii + Feiii emission (the latter is only relevant in the 1900 blend and for population A). For the UV Feii and Feiii emissions we considered the templates provided by Brühweiler & Verner (2008) and Vestergaard & Wilkes (2001), respectively. The fitting routine scaled and broadened the original templates to reproduce the observed emission.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

GTC spectra ofz≈ 2.3 quasars: comparison with local luminosity analogs

Sulentic¹,

Marziani²,

Olmo³

et al. 2014

A&A

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Context. The advent of 8−10 m class telescopes for the first time makes it possible to compare in detail quasars with similar luminosity and very different redshifts. Aims. We conducted a search for z-dependent gradients in line-emission diagnostics and derived physical properties by comparing, in a narrow bolometric luminosity range (log L ∼ 46.1± 0.4 [erg s −1 ]), some of the most luminous local z < 0.6 quasars with some of the lowest luminosity sources yet found at redshift z = 2.1−2.5. Methods. Moderate signal-to-noise ratio spectra for 22 high-redshift sources were obtained with the 10.4 m Gran Telescopio Canarias (GTC), for which the HST (largely the Faint Object Spectrograph) archive provides a low-redshift control sample. We compared the spectra in the context of the 4D Eigenvector 1 formalism, meaning that we divided both source samples into highly accreting population A and population B sources accreting at a lower rate. Results. Civλ1549, the strongest and most reliable diagnostic line, shows very similar properties at both redshifts, which confirms the Civλ1549 profile differences at high redshift between populations A and B, which are well established in local quasars. The Civλ1549 blueshift that appears quasi-ubiquitous in higher L sources is found in only half (population A) of the quasars observed in the two samples. A Civλ1549 evolutionary Baldwin effect is certainly disfavored. We find evidence for lower metallicity in the GTC sample that may point toward a gradient with z. No evidence for a gradient in M BH or L/L Edd is found. Conclusions. Spectroscopic differences established at low z are also present in much higher redshift quasars. Our results on the Civλ1549 blueshift suggest that it depends both on source luminosity and L/L Edd . Given that our samples involve sources with very similar luminosity, the evidence for a systematic metallicity decrease, if real, points toward an evolutionary effect. Our samples are not large enough to effectively constrain possible changes of M BH or L/L Edd with redshift. The two samples appear representative of a slowly evolving quasar population that is most likely present at all redshifts.

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Modeling FeiiEmission and Revised Feii(UV) Empirical Templates for the Seyfert 1 Galaxy I Zw 1

Cited by 118 publications

References 39 publications

SALT long-slit spectroscopy of LBQS 2113-4538: variability of the Mg II and Fe II component

SALT long-slit spectroscopy of LBQS 2113-4538: variability of the Mg II and Fe II component

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

GTC spectra ofz≈ 2.3 quasars: comparison with local luminosity analogs

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