next previous
Up: Abstract

A&A Supplement series, Vol. 122, April II 1997, 255-266

Received April 25; accepted July 7, 1996

Results of the ESO-SEST key programme: CO in the Magellanic Clouds

VI. The 30 Dor Complexgif

M.L. Kutner tex2html_wrap1175 - M. Rubio tex2html_wrap1177 - R.S. Booth tex2html_wrap1179 - F. Boulanger tex2html_wrap1181 - Th. de Graauw tex2html_wrap1183 - G. Garay tex2html_wrap1185 - F.P. Israel tex2html_wrap1187 - L.E.B. Johansson tex2html_wrap1189 - J. Lequeux tex2html_wrap1191 - L.-Å. Nymantex2html_wrap1193

Send offprint request: M.L. Kutner

tex2html_wrap1195  NRAO, 949 N. Cherry Av., Campus Building 65, Tucson , Arizona 85721-0655, U.S.A.
tex2html_wrap1197  Department of Physics, Rensselaer Polytechnic Institute, Troy, NY 12180, U.S.A.
tex2html_wrap1199  Departamento de Astronomía , Universidad de Chile, Casilla 36-D, Santiago, Chile
tex2html_wrap1201  Onsala Space Observatory, S-43900 Onsala, Sweden
tex2html_wrap1203  Radioastronomie, Ecole Normale Superieure, 24 Rue Lhomond, 75231 Paris Cedex 05, France
tex2html_wrap1205  Institut d'Astrophysique Spatiale, Bat. 120, Université de Paris-XI, 91045 Orsay Cedex, France
tex2html_wrap1207  Laboratorium voor Ruimteonderzoek, SRON, Postbus 800, NL-9700 AV Groningen, The Netherlandis
tex2html_wrap1209  Sterrewacht, Postbus 9513, NL-2300 Leiden, The Netherlands
tex2html_wrap1211  DEMIRM, Observatoire de Paris, 61 Av. de l'Observatoire, 75014 Paris, France
tex2html_wrap1213  European Southern Observatory, Casilla 19001, Santiago 19, Chile


We report observations of tex2html_wrap_inline1155 emission from molecular clouds in a complex extending tex2html_wrap_inline11572 kpc south of 30 Dor in the Large Magellanic Cloud. The observations were taken on the Swedish-ESO Submillimetre Telescope (SEST) as part of the Key Programme: CO in the Magellanic Clouds. This paper presents observations of the emission from the Central and Southern parts of that complex. In both parts, the strongest emission has tex2html_wrap_inline1159. This is a factor of tex2html_wrap_inline1161 to 5 weaker than we would expect for Milky Way GMCs observed at a distance of 50 kpc. In the Central region, the emission is dominated by a 600 pc long, slightly curved feature, which is clearly seen in peak and integrated intensity maps. When we look at this emission in 5 km stex2html_wrap_inline1163 velocity ranges, it breaks into 22 clouds whose sizes and line profiles look like that from Milky Way molecular clouds. The Southern region is clearly separated from the Central region, and its emission can be broken into 5 clouds.

keywords: Galaxy: Magellanic Clouds -- interstellar medium: molecules -- interstellar medium: clouds -- interstellar medium: molecules, millimeter lines -- radio lines: molecular

next previous
Up: Abstract

Copyright by the European Southern Observatory (ESO)