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Date and Time of the Query: 2019-07-20 T23:53:56 PDT
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For refcode 1995A&AS..114..147B:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
1995A&AS..114..147B Observations of CO lines in southern spiral galaxies* E. Bajaja, A. Wielebinski, H.-P. Reuter, J.I. Harnett and E. Hummel Instituto Argentino de Radioastronomia, C.C. 5, 1894 Villa Elisa (Prov. de Bs.As.), Argentina Max-Planck-Institut fur Radioastronomie, Auf dem Hugel 69, D-53121 Bonn, Germany IRAM, Avenida Divina Pastora 7, Nucleo Central, 18012 Granada, Spain School of Physics, University of Sydney, Sydney NSW 2006, Australia Goudvink 7,7827 DK Emmen, The Netherlands Received October 26, 1994; accepted May 23,1995 Abstract. - Six southern spiral galaxies, with diameters between 5' and 8', were mapped with the SEST in the 12^CO^(1-0) line. CO emission was detected in five of the galaxies. The 43" beam of the SEST, at 115 GHz, was small enough for determining the general distribution of the gas, which is centrally peaked in all the cases, and the velocity field from which we could derive the major axis position angle and the rotation curve. The latter is, in general, very steep at the centre and quite flat after the turn-over point. It was used to estimate the total mass of the galaxy up to the farthest measured point. The gas mass was estimated from the CO and HI global velocity profiles. On three of the galaxies the ^12^CO(2-1) and ^13^CO(1-0) lines were also observed on their centres, the first one on a 10" grid, covering a region of 20" x 20", and the second on one point towards the centre. The average ratio between the intensities of the ^12^CO(2-1) and ^12^CO(1-0) spectra is 1.3 in the three cases. The detections of the ^13^CO(1-0) were only marginal. A good correlation has been found between the CO and the continuum emission at 843 MHz. Key words: galaxies: ISM; spiral - radio lines: galaxies
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