A Sample of<i>IRAS</i>Infrared‐selected Seyfert 1.5 Galaxies: Infrared Color α(60, 25)‐dominated Eigenvector 1

Wang, J.; Wei, J. Y.; He, X. T.

doi:10.1086/498667

Cited by 40 publications

(35 citation statements)

References 80 publications

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“…A sources shows a significant Mgiiλ2800 blueshift (Paper I) making FWHM Hβ a safer virial estimator. These sources can be described as the youngest leastevolved quasars with strong ongoing star formation among all quasars in the present sample (e.g., Sulentic et al 2000a;Mathur 2000;Wang et al 2006;Sani et al 2010). Extreme values of R FeII appear to be an empirical signature of quasar youth perhaps reflecting extreme low ionization and metal enrichment as well (cf.…”

Section: Introductionmentioning

confidence: 76%

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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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Section: Introductionmentioning

confidence: 76%

“…Variants of E1 were later found in several studies (e.g. Marziani et al 1996;Boroson 2002;Grupe 2004;Kuraszkiewicz et al 2002;Sulentic et al 2000bSulentic et al , 2002Yip et al 2004;Kovačević et al 2010;Kruczek et al 2011;Tang et al 2012;Wang et al 2006).…”

Section: Introductionmentioning

confidence: 83%

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

Marziani

Sulentic

Plauchu-Frayn

et al. 2013

A&A

156

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“…The E1 space extends also to the optical variability of quasars [55], the far-IR luminosity [127]. Even the Baldwin Effect -hailed as the most important luminosity effect -is at least in part due to the HIL equivalent width correlations associated with E1 [4,7,57,63].…”

Section: Organizing Quasar Diversity: the 4de1 Approachmentioning

confidence: 99%

Low- and High-zHighly Accreting Quasars in the 4D Eigenvector 1 Context

Marziani¹,

Sulentic²,

Negrete³

et al. 2014

Astronomical Review

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Highly accreting quasars are characterized by distinguishing properties in the 4D eigenvector 1 parameter space that make them easily recognizable over a broad range range of redshift and luminosity. The 4D eigenvector 1 approach allows us to define selection criteria that go beyond the restriction to Narrow Line Seyfert 1s identified at low redshift. These criteria are probably able to isolate sources with a defined physical structure i.e., a geometrically thick, optically thick advectiondominated accretion disk (a "slim" disk). We stress that the importance of highly accreting quasars goes beyond the understanding of the details of their physics: their Eddington ratio is expected to saturate toward values of order unity, making them possible cosmological probes.

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“…We reprocessed the EPIC PN and MOS Observation Data Files (ODFs) to obtain new calibrated and concatenated event (Verma et al 2002), IRAS 14026+4321 (Wang et al 2006) and IRAS 18216+6418 (Véron-Cetty & Véron 2006). IRAS 00182-7112 has been classified as type 2 source using the optical emission lines from Armus et al (1989) and the diagnostic diagrams from Osterbrock (1989, chap.…”

Section: Data Reductionmentioning

confidence: 99%

An XMM-Newtonstudy of hyper-luminous infrared galaxies

Ruiz

Carrera²,

Panessa

2007

A&A

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Aims. Hyper-Luminous Infrared Galaxies (HLIRGs) are the most luminous persistent objects in the Universe. They exhibit extremely high star formation rates, and most of them seem to harbor an Active Galactic Nucleus (AGN). They are unique laboratories to investigate ultimate star formation, and its connection to super-massive black hole growth. X-ray studies of HLIRGs have the potential to unravel the AGN contribution to the bolometric output from these bright objects. Methods. We have selected a sample of 14 HLIRGs observed by XMM-Newton (type 1, type 2 AGN and starburst), 5 of which are candidates to be Compton-thick objects. This is the first time that a systematic study of this type of objects has been carried out in the X-ray spectral band. Their X-ray spectral properties have been correlated with their infrared luminosities, estimated by IRAS, ISO and sub-millimeter observations. Results. The X-ray spectra of HLIRGs present heterogeneous properties. All our X-ray detected HLIRGs (10) have AGN-dominated X-ray spectra. The hard X-ray luminosity of 8 of them is consistent with a pure AGN contribution, while in the remaining 2 sources, both an AGN and a starburst seem to contribute to the overall emission. We found soft excess emission in 5 sources. In one of them it is consistent with a pure starburst origin, while in the other 4 sources it is consistent with an AGN origin. The observed X-ray emission is systematically below that expected for a standard local QSO of the same IR luminosity, suggesting the possible presence of absorption in type 2 objects and/or a departure from a standard spectral energy distribution of QSO. The X-ray-to-IR-luminosity ratio is constant with redshift, indicating similar evolutions for the AGN and starburst component, and that their respective power sources could be physically related.

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A Sample ofIRASInfrared‐selected Seyfert 1.5 Galaxies: Infrared Color α(60, 25)‐dominated Eigenvector 1

Cited by 40 publications

References 80 publications

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

Low- and High-zHighly Accreting Quasars in the 4D Eigenvector 1 Context

An XMM-Newtonstudy of hyper-luminous infrared galaxies

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