Volume 608, December 2017
|Number of page(s)||18|
|Published online||14 December 2017|
1 Instituto de Astrofisíca de Andalucía, IAA-CSIC, 18008 Granada, Spain
2 INAF, Osservatorio Astronomico di Padova, IT 35122 Padova, Italy
3 Dipartimento di Fisica & Astronomia “Galileo Galilei”, Univ. of Padova, 35121 Padova, Italy
4 Instituto de Astronomía, UNAM, Mexico DF 04510, Mexico
5 INAF, Osservatorio Astronomico di Bologna, 40129 Bologna, Italy
6 Dept. of Physics & Astronomy, University of Wisconsin, Stevens Points, WI 54481, USA
Received: 21 December 2016
Accepted: 7 August 2017
Broad emission lines in quasars enable us to “resolve” structure and kinematics of the broad-line emitting region (BLR) thought to involve an accretion disk feeding a supermassive black hole. Interpretation of broad line measures within the 4DE1 formalism simplifies the apparent confusion among such data by contrasting and unifying properties of so-called high and low accreting Population A and B sources. Hβ serves as an estimator of black hole mass, Eddington ratio and source rest frame; the latter being a valuable input for Civλ1549 studies which allow us to isolate the blueshifted wind component. Optical and HST-UV spectra yield Hβ and Civλ1549 spectra for low-luminosity sources while VLT-ISAAC and FORS and TNG-LRS provide spectra for high-luminosity sources. New high-S/N data for Civ in high-luminosity quasars are presented here for comparison with the other previously published data. Comparison of Hβ and Civλ1549 profile widths/shifts indicates that much of the emission from the two lines arise in regions with different structure and kinematics. Covering a wide range of luminosity and redshift shows evidence for a correlation between Civλ1549 blueshift and source Eddington ratio, with a weaker trend with source luminosity (similar amplitude outflows are seen over four of the five dex luminosity ranges in our combined samples). At low luminosity (z ≲ 0.7) only Population A sources show evidence for a significant outflow while at high luminosity the outflow signature begins to appear in Population B quasars as well.
Key words: quasars: general / quasars: emission lines / quasars: supermassive black holes
Based on observations made with ESO telescopes at the La Silla Paranal Observatory under programme ID082.B-0572(A) and with the Italian Telescopio Nazionale Galileo (TNG) operated by the Fundación Galileo Galilei (INAF) at the Observatorio del Roque de los Muchachos.
The reduced spectra are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/608/A122
© ESO, 2017
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