Hostname: page-component-8448b6f56d-dnltx Total loading time: 0 Render date: 2024-04-18T02:23:16.293Z Has data issue: false hasContentIssue false
  • English
  • Français

Fe II Emission in the NLS1 galaxy I Zw 1: Results from NIR Spectroscopy

Published online by Cambridge University Press:  03 June 2010

Alberto Rodríguez-Ardila  and
Aurea Garcia Rissmann
Alberto Rodríguez-Ardila
Affiliation:
Laboratório Nacioal de Astrofísica/MCT, Brazil Email: aardila@lna.br
Aurea Garcia Rissmann
Affiliation:
Gemini Observatory, Chile Email: arissmann@gemini.edu
Rights & Permissions [Opens in a new window]

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.

Fe ii comprises up to one third of the line emission in AGNs. For that reason it is an important coolant that needs to be taken into account to fully understand the energetics of the broad line region (BLR). As such, Fe+ is a potential diagnostic of gas density, column density, turbulence, temperature and continuum shape. However, understanding Fe ii is complicated because of the energy level configuration and different mechanisms that may contribute to the line emission.

Keywords

galaxies: Seyfertinfrared: galaxiestechniques: spectroscopic
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S267: Co-Evolution of Central Black Holes and Galaxies , August 2009 , pp. 136
Copyright
Copyright © International Astronomical Union 2010

References

Rodríguez-Ardila, A., Viegas, S. M., Pastoriza, M. G., & Prato, L. 2002, ApJ, 565, 140CrossRefGoogle Scholar
Sigut, T. A. A. & Pradhan, A. K. 2003, ApJS, 145, 15CrossRefGoogle Scholar
Wills, B. J., Netzer, H., & Wills, D. 1985, ApJ, 288, 94CrossRefGoogle Scholar