Abstract

We have obtained radial velocities of 68 planetary nebulae (PNs) surrounding the SB0 galaxy NGC 3384 in the Leo I group, using the CTIO 4 m telescope and the Rutgers Fabry-Perot interferometer. The PN system exhibits a well-ordered rotation field aligned with the photometric axes of the galaxy. The rotation curve is flat from about 2 kpc until at least 7 kpc. We infer a lower limit of 0.7 x 10 11M. for the mass of NGC 3384. Our results imply that at least a third of the dynamical mass of the NGC 3379/3384 system -- estimated by Schneider (1985) to be roughly 6 x 10 11M. -- may be accounted for in the two bright galaxies. (Refer to PDF file for exact formulas).

Publication Date

4-10-1995

Comments

Also archived in: astro-ph/9510098 19 Oct 1995 This work was supported by NSF grant AST-9318617 to DM and by a Grant-in-Aid of Research from the National Academy of Sciences through Sigma Xi. The RFP was developed with support from Rutgers University and the National Science Foundation, under grant AST 83-19344.ISSN:1538-4357 Note: imported from RIT’s Digital Media Library running on DSpace to RIT Scholar Works in February 2014.

Document Type

Article

Department, Program, or Center

School of Physics and Astronomy (COS)

Campus

RIT – Main Campus

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