Relativistic beaming and quasar emission lines

Wills, Beverley J.; Browne, I. W. A.

doi:10.1086/163973

Cited by 277 publications

(310 citation statements)

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“…In bin B1 we are probably considering a subsample of FRII that show narrower profile than the majority of the population. If the FWHM is affected by orientation as expected (e.g., Wills & Browne 1986;Sulentic et al 2003;Rokaki et al 2003;Runnoe et al 2013;Zamfir et al 2008), we are observing sources that tend to be seen at a smaller viewing angle than the general FRII population. If the wind flow follows a bent path over the accretion disk (Elvis 2000) or if the flow is constrained closer to the disk plane, the absence of a blueshift might therefore be related more to orientation than to full suppression of disk winds in RL sources by the pressure of a cocoon associated with the relativistic ejections (Norman & Miley 1984).…”

Section: Radio Quiet and Radio Loudmentioning

confidence: 54%

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: Radio Quiet and Radio Loudmentioning

confidence: 54%

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

Marziani

Sulentic

Plauchu-Frayn

et al. 2013

A&A

156

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“…Note that this BH mass is a factor of 3 lower than the lowest BH mass of the radio-loud quasars in the PG sample and the accretion rate is much higher than predicted by the relation between L=L Edd and the radio loudness of Ho (2002). However, if the broad-line region is flat, the small line width can be due to inclination effects (Wills & Browne 1986). In this case, the BH mass could be severely underestimated.…”

Section: Discussionmentioning

confidence: 76%

SDSS J094857.3+002225: A Very Radio Loud, Narrow‐Line Quasar with Relativistic Jets?

Zhou

Wang

Dong

et al. 2003

ApJ

163

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We report the identification of a very radio loud, narrow-line quasar, SDSS J094857.3+002225, discovered in the Sloan Digital Sky Survey (SDSS) early data release (EDR). With FWHM ðH Þ % 1500 km s À1 and undetected [O iii] 4959, 5007 SDSS J094857.3+002225 is consistent with the conventional definition of narrow-line Seyfert 1 galaxies (NLS1s). Its strong optical Fe ii emission [R 4570 f ðFe ii 4570Þ= f ðH Þ % 1:59] is also typical of NLS1s. With a radio loudness RL ð f ;4:85 GHz =f ;B Þe1000 and radio power of P 4:85 GHz $ ð3:6 5:2Þ Â 10 26 W Hz À1 , it is the first bona fide, very radio loud NLS1. The inverted radio spectrum and very high brightness temperature (e10 13 K) derived from variation of the radio flux suggest the presence of a relativistic jet beaming toward the observer in this NLS1.

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“…We again see a preferred thick disk geometry in 3C 120 and the inclination angle of the system is well-constrained at θ i = 17.6 +5.4 −3.3 relative to the observer. 3C 120 is of particular interest because there are external indicators of inclination angle in the system obtained from radio jet orientation, which has shown to be linked to the BLR rotation axis (e.g., Wills & Browne 1986;Marscher et al 2002;Jorstad et al 2005;Agudo et al 2012). Marscher et al (2002) first determined the upper limit on the jet viewing angle to be 20 degrees, and further work by Jorstad et al (2005) measured a viewing angle of 20.5 ± 1.8 degrees.…”

Section: Mrk 1501mentioning

confidence: 99%

The Structure of the Broad-line Region in Active Galactic Nuclei. II. Dynamical Modeling of Data From the AGN10 Reverberation Mapping Campaign

Grier

Pancoast

Barth

et al. 2017

ApJ

144

171

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We present inferences on the geometry and kinematics of the broad-Hβ line-emitting region in four active galactic nuclei monitored as a part of the fall 2010 reverberation mapping campaign at MDM Observatory led by the Ohio State University. From modeling the continuum variability and response in emission-line profile changes as a function of time, we infer the geometry of the Hβ-emitting broad line regions to be thick disks that are close to face-on to the observer with kinematics that are well-described by either elliptical orbits or inflowing gas. We measure the black hole mass to be log 10 (M BH ) = 7.25 −0.23 for PG 2130+099. These black hole mass measurements are not based on a particular assumed value of the virial scale factor f , allowing us to compute individual f factors for each target. Our results nearly double the number of targets that have been modeled in this manner, and investigate the properties of a more diverse sample by including previously modeled objects. We measure an average scale factor f in the entire sample to be log 10f = 0.54 ± 0.17 when the line dispersion is used to characterize the line width, which is consistent with values derived using the normalization of the M BH -σ relation. We find that the scale factor f for individual targets is likely correlated with the black hole mass, inclination angle, and opening angle of the broad line region but we do not find any correlation with the luminosity.

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Relativistic beaming and quasar emission lines

Cited by 277 publications

References 0 publications

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

SDSS J094857.3+002225: A Very Radio Loud, Narrow‐Line Quasar with Relativistic Jets?

The Structure of the Broad-line Region in Active Galactic Nuclei. II. Dynamical Modeling of Data From the AGN10 Reverberation Mapping Campaign

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