Hostname: page-component-76fb5796d-skm99 Total loading time: 0 Render date: 2024-04-26T00:44:59.299Z Has data issue: false hasContentIssue false
  • English
  • Français

Keck High-Resolution Spectroscopy of Mrk 335: Constraints on the Number of Emitting Clouds in the BLR

Published online by Cambridge University Press:  12 April 2016

Nahun Arav ,
Tom A. Barlow ,
Roger D. Blandford  and
Ari Laor
Nahun Arav
Affiliation:
Theoretical Astrophysics, Caltech 130-33, Pasadena, CA 91125, USA
Tom A. Barlow
Affiliation:
Theoretical Astrophysics, Caltech 130-33, Pasadena, CA 91125, USA
Roger D. Blandford
Affiliation:
Theoretical Astrophysics, Caltech 130-33, Pasadena, CA 91125, USA
Ari Laor
Affiliation:
Physics Department, Technion, Haifa 3200, Israel

Abstract

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.

By applying cross-correlation (CC) techniques to high-resolution (~ 6km s−1), high S/N (~ 400 at Hα line center) spectra of Mrk 335, we are able to put a lower limit of ~ 3 × 106 on the number of emitting clouds in this objects. This limit is applicable for clouds with T = 2 × 104 K and an optical depth of a few hundred in their Hα line. Current BEL models based on stellar atmospheres of bloated stars can be ruled out based on this lower limit.

Type
IV. Physics of the Broad-Line Region
Information
International Astronomical Union Colloquium , Volume 159: Emission Lines in Active Galaxies: New Methods and Techniques , 1997 , pp. 211 - 212
Copyright
Copyright © Astronomical Society of the Pacific 1997

References

Alexander, T., & Netzer, H. 1994, MNRAS, 270, 803.Google Scholar
Atwood, B., Baldwin, J.A., & Carswell, R.F. 1982, ApJ, 257, 559.Google Scholar
Kazanas, D. 1989, ApJ, 347, 74.Google Scholar
Scoville, N., & Norman, C. 1989, ApJ, 332, 162.Google Scholar