What does Civ{\lambda}1549 tell us about the physical driver of the Eigenvector Quasar Sequence?

J. W. Sulentic; A. del Olmo; P. Marziani; M. A. Martínez-Carballo; M. D'Onofrio; D. Dultzin; J. Perea; M. L. Martínez-Aldama; C. A. Negrete; G. M. Stirpe; S. Zamfir

doi:10.1051/0004-6361/201630309

arXiv · 1708.03187

What does Civ{\lambda}1549 tell us about the physical driver of the Eigenvector Quasar Sequence?

J. W. Sulentic·A. del Olmo·P. Marziani·M. A. Martínez-Carballo·M. D'Onofrio·D. Dultzin·J. Perea·M. L. Martínez-Aldama·C. A. Negrete·G. M. Stirpe·S. Zamfir

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Abstract

Broad emission lines in quasars enable us to "resolve" structure and kinematics of the broad line emitting region (BLR) thought to in- volve 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. H{\beta} serves as an estimator of black hole mass, Eddington ratio and source rest frame, the latter a valuable input for Civ{\lambda}1549 studies which allow us to isolate the blueshifted wind component. Optical and HST-UV spectra yield H{\beta} and Civ{\lambda}1549 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 H{\beta} and Civ{\lambda}1549 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 Civ{\lambda}1549 blueshift and source Eddington ratio, with a weaker trend with source luminosity (similar amplitude outflows are seen over 4 of the 5 dex luminosity range 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.

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J. W. Sulentic, A. del Olmo, P. Marziani, M. A. Martínez-Carballo, M. D'Onofrio, D. Dultzin, J. Perea, M. L. Martínez-Aldama, C. A. Negrete, G. M. Stirpe, S. Zamfir. 2017-08-10. What does Civ{\lambda}1549 tell us about the physical driver of the Eigenvector Quasar Sequence?. https://doi.org/10.1051/0004-6361%2F201630309

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