Hostname: page-component-586b7cd67f-g8jcs Total loading time: 0 Render date: 2024-11-29T13:39:37.344Z Has data issue: false hasContentIssue false

The Starburst in the Nucleus of NGC 6764: The Near-IR/Radio/Optical Connection

Published online by Cambridge University Press:  12 April 2016

Murray Cameron
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany
Andreas Eckart
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany
Reinhard Genzel
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Garching, Germany
Naomasa Nakai
Affiliation:
Nobeyama Radio Observatory, Nagano, Japan
Stefan Wagner
Affiliation:
Landessternwarte, Heidelberg, Germany

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.

Knowledge of the distribution and excitation of gas close to the nuclei of starburst galaxies is an essential element in the construction of models dealing with intense, but short-lived, star forming events. Building a comprehensive picture of the concentrations of various gaseous components in such regions calls for a multi-wavelength approach: the principal cooling lines of cold (T≤200K) molecular gas fall in the millimetre waveband, those of hot (T~1−3×103K) excited molecular material in the near-IR, and those pinpointing starburst activity in the optical. In many cases the extents of the emitting regions are on the order of only a few arcseconds.

As part of such a study into the relationship between various near- and circum- nuclear gaseous components in starburst galaxies, we have obtained data on NGC 6764, a barred spiral classified as a LINER, at resolutions of 1″−4″ across the optical, near-infrared and millimetre wavelength regimes. In a previous paper (Eckart et al. 1991) we discussed extensive single dish millimetre and JHK near-IR measurements of the nucleus and disk of NGC 6764. Here we present new near-IR observations obtained with the MPE FAST instrument (Rotaciuc et al. 1991) at the William Herschel Telescope, along with 2″ resolution 12CO J=1-0 (115 GHz) interferometry measured with the Nobeyama millimeter array and 1″ optical spectroscopy from the 3.5m Calar Alto telescope.

Type
3. Astronomical Results and Prospects
Copyright
Copyright © Astronomical Society of the Pacific 1994

References

Eckart, A., Cameron, M., Jackson, J.M., Genzel, R., Harris, A.I., Wild, W. & Zinnecker, H., 1991, Ap. J., 372, 67.Google Scholar
Rotaciuc, V., Krabbe, A., Cameron, M., Drapatz, S., Genzel, R., Sternberg, A. & Storey, J.W.V., 1991, Ap.J., 370, L23.Google Scholar
Wilson, A.S. & Willis, A.G., 1980, Ap.J., 240, 429.CrossRefGoogle Scholar