Hostname: page-component-76fb5796d-25wd4 Total loading time: 0 Render date: 2024-04-25T08:08:23.522Z Has data issue: false hasContentIssue false
  • English
  • Français

The HST Sample of Radio-Loud Quasars: Fe II and Other Correlations

Published online by Cambridge University Press:  12 April 2016

D. Wills ,
K.L. Thompson ,
M.S. Brotherton ,
Beverley J. Wills ,
J. A. Baldwin ,
R. F. Carswell ,
I. W.A. Browne  and
H. Netzer
D. Wills
Affiliation:
McDonald Observatory and Department of Astronomy, RLM 15.308, University of Texas at Austin, TX 78712, USA
K.L. Thompson
Affiliation:
McDonald Observatory and Department of Astronomy, RLM 15.308, University of Texas at Austin, TX 78712, USA
M.S. Brotherton
Affiliation:
McDonald Observatory and Department of Astronomy, RLM 15.308, University of Texas at Austin, TX 78712, USA
Beverley J. Wills
Affiliation:
McDonald Observatory and Department of Astronomy, RLM 15.308, University of Texas at Austin, TX 78712, USA
J. A. Baldwin
Affiliation:
CTIO, Casilla 603, La Serena, Chile
R. F. Carswell
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge, CB3 OHA, UK
I. W.A. Browne
Affiliation:
Nuffield Radio Astronomy Laboratories, Jodrell Bank, Cheshire SK11 9DL, UK
H. Netzer
Affiliation:
Tel-Aviv University, Tel-Aviv, Israel

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We are analyzing the emission lines and continuum spectra of a sample of ~61 radio-loud quasars to investigate dependences amongst various spectral, radio, and X-ray parameters, in particular to look for dependences of spectral properties on inclination of the the radio-jet axis (Wills et al. 1997).

We have carried out conventional correlation analyses, as well as spectral principal-component analyses (SPCA) as described in the previous paper (Wills et al. 1997). We found that the single largest contribution to the spectrum-tospectrum variations was from a component — the ‘first principal component’ (PC1) — that has a more UV (or less red) continuum than the mean spectrum, and a weaker narrow-line (NLR) spectrum. The ‘second principal component’ (PC2) accounts for only 8–12% of the spectrum-to-spectrum variation, contributing a weaker UV, and stronger red continuum, and showing stronger narrow emission lines. There is also a tendency for the broad (BLR) lines in the second principal component spectrum to be narrower (note the sharper He II λ1640 and [O III] λ1663 features redward of the stronger C IV λ1549 emission line, and perhaps a narrow component of the N V λ1240 line redward of Lyα).

Type
II. Broad Emission Lines
Information
International Astronomical Union Colloquium , Volume 159: Emission Lines in Active Galaxies: New Methods and Techniques , 1997 , pp. 106 - 107
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Baker, J.C., Hunstead, R.W., Kapahi, V.K., & Subrahmanya, C.R. 1994, in The First Stromlo Symposium: The Physics of Active Galaxies, ed. Bicknell, G.V., Dopita, M.A., & Quinn, P.J. (San Francisco: Astronomical Society of the Pacific), 195.Google Scholar
Brotherton, M.S. 1997, this volume.Google Scholar
Hes, R., Fosbury, R.A.E., & Barthel, P.D. 1994, in The First Stromlo Symposium: The Physics of Active Galaxies, ed. Bicknell, G.V., Dopita, M.A., & Quinn, P.J. (San Francisco: Astronomical Society of the Pacific), 367.Google Scholar
Wills, B.J., et al. 1997, this volume.Google Scholar