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Date and Time of the Query: 2019-06-17 T16:04:35 PDT
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For refcode 2002AJ....123..729O:
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2002AJ....123..729O EXTENDED H I DISKS IN DUST LANE ELLIPTICAL GALAXIES THOMAS A. OOSTERLOO AND RAFFAELLA MORGANTI ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands; oosterloo@astron.nl, morganti@astron.nl ELAINE M. SADLER School of Physics, University of Sydney, NSW 2006, Australia; ems@physics.usyd.edu.au DANIELA VERGANI Dipartimento di Astronomia, Universita di Bologna, via Zamboni 33, I-40126 Bologna, Italy AND NELSON CALDWELL Smithsonian Astrophysical Observatory and Steward Observatory, 949 North Cherry Avenue, Tucson, AZ 85719; caldwell@flwo99.sao.arizona.edu Received 2001 August 11; accepted 2001 October 22 ABSTRACT We present the results of H I observations of five dust lane elliptical galaxies with the Australia Telescope Compact Array. Two galaxies (NGC 3108 and NGC 1947) are detected, and sensitive upper limits are obtained for the other three. In the two detected galaxies, the H I is distributed in a regular, extended, and warped disklike structure of low surface brightness. Adding data from the literature, we find that several more dust lane elliptical galaxies have regular H I structures. This H I is likely to be a remnant of accretions and/or mergers that took place a considerable time ago and in which a significant fraction of the gas survived to form a disk. The presence of regular H I structures suggests that some mergers lead to galaxies with extended low surface brightness density gas disks. These gas disks will evolve very slowly, and these elliptical galaxies will remain gas-rich for a long period of time. One of the galaxies we observed (NGC 3108) has a very large amount of neutral hydrogen (M_H I_ = 4.5 x 10^9^ M_sun_; M_H I_/L_B_ ~ 0.09), which is very regularly distributed in an annulus extending to a radius of ~6 R_eff_. The kinematics of the H I distribution suggest that the rotation curve of NGC 3108 is flat out to at least the last observed point. We estimate a mass-to-light ratio of M/L_B_ ~ 18 M_sun_/L_B,sun_ at a radius of ~6 R_eff_ from the center. Several of the galaxies we observed have an unusually low gas-to-dust ratio M_H I_/M_dust_, suggesting that their cold interstellar medium, if present as expected from the presence of dust, may be mainly in molecular rather than atomic form. Key words: galaxies: individual (NGC 1947, NGC 3108, NGC 7049, NGC 7070A, ESO 263-G48) - galaxies: ISM - galaxies: kinematics and dynamics
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