Hostname: page-component-586b7cd67f-2plfb Total loading time: 0 Render date: 2024-11-29T14:46:43.220Z Has data issue: false hasContentIssue false
  • English
  • Français

A Basic Step Toward the CO-Line Tully-Fisher Relation

Published online by Cambridge University Press:  12 April 2016

Yoshiaki Sofue  and
Franz Schöniger
Yoshiaki Sofue
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181
Franz Schöniger
Affiliation:
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181

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.

The Tully-Fisher relation makes use of the correlation between the HI linewidth and the luminosity of a galaxy and is one of the most powerful tools to estimate distances of galaxies. Because of the smaller beam the CO line might be an alternative to HI for distant galaxies which so far can not be examined even by the largest telescopes (Dickey and Kazes 1992).

In order to consider the question whether the CO lineprofile could be used as an alternative or a supplement for HI in the Tullly-Fisher relation, we compared the total CO (J=2-1) line profiles of ten galaxies with the corresponding HI profiles. Four almost perfect edge-on galaxies (NGC 891, NGC 4565, NGC 4631 and NGC 3079) and the Seyfert galaxy NGC 1808 have been observed in CO using the Nobeyama 45-m telescope. The HI profiles and the data of the other galaxies has been taken from the literature.

Type
3. Astronomical Results and Prospects
Information
International Astronomical Union Colloquium , Volume 140: Astronomy with Millimeter and Submillimeter Wave Interferometry , 1994 , pp. 368 - 369
Copyright
Copyright © Astronomical Society of the Pacific 1994

References

Dickey, J., and Kazes, I. 1992, ApJ, 393, 530.Google Scholar
Newton, K. 1980, MNRAS, 191, 169 CrossRefGoogle Scholar
Weliachew, L., Sancisi, R., and Guelin, M. 1978, A&A, 65, 37.Google Scholar