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Date and Time of the Query: 2019-06-18 T06:33:26 PDT
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For refcode 2002A&A...381L..29O:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2002A&A...381L..29O VLA detection of OH absorption from the elliptical galaxy NGC 1052 A. Omar, K. R. Anantharamaiah, M. Rupen and J. Rigby Raman Research Institute, C.V. Raman Avenue, Bangalore, 560 080, India National Radio Astronomy Observatory, Socorro, NM, USA; e-mail: mrupen@aoc.nrao.edu Steward Observatory, University of Arizona, 933 N. Cherry Ave, Tucson, AZ 85721, USA; e-mail: jrigby@as.arizona.edu Received 3 September 2001/Accepted 12 November 2001 Abstract. VLA observations of OH absorption towards the elliptical galaxy NGC 1052 are presented. Both OH lines, at 1665 and 1667 MHz, were detected in absorption towards the center of NGC 1052. The hyperfine ratio of the two OH lines ({tau}_1667_/{tau}_1665_) is 2.6 +/- 0.8 as compared to 1.8 expected for the excitation under LTE conditions for an optically thin cloud. The column density of OH is estimated to be 2.73(+/-0.26) x 10^14^ cm^-2^ assuming T_ex_ ~ 10 K. The centers of both the OH lines are redshifted from the systemic velocity of the galaxy by ~173 km s^-1^. The velocity of OH line coincides with the velocity corresponding to the strongest HI absorption. We suggest that OH absorption is arising from a molecular cloud falling towards the nucleus. The OH line, though narrower, is found to be within the much broader and smoother H_2_O megamaser emission. The possible link between OH/HI and H_2_O emission is discussed. Key words: galaxies: active - galaxies: individual: NGC 1052 - galaxies: ISM - radio lines: galaxies
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