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



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


Department, Program, or Center

School of Physics and Astronomy (COS)


RIT – Main Campus