1998/07/31 by Yoshiaki Sofue, Akihiko Tomita, Yoshinori Tutui +2 · 2 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Emission spectrum #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy rotation curve #Light curve #Line (geometry) #Rotation (mathematics) #Spiral galaxy #Stellar rotation #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1093/pasj/50.5.427
10 pages Latex, 8 fig. directories, each 22 galaxies ps figures. PASJ Vol. 50, No.5, in press
arxiv created 1998/07/31 · openalex publication_date 1998/10/01 · openalex created_date 2016/06/24 · arxiv updated 2017/01/04 · openalex updated_date 2026/08/05
We have obtained optical CCD spectroscopy along the major axes of 22 nearby spiral galaxies of Sb and Sc types in order to analyze their rotation curves. By subtracting the stellar continuum emission, we have obtained position–velocity (PV) diagrams of the Hα and [N II] lines. We point out that the Hα line is often superposed by a broad stellar absorption feature (Balmer wing) in the nuclear regions, and, therefore, the [N II] line is a better tracer of kinematics in the central few hundred parsec regions. By applying the envelope-tracing technique to the Hα and [N II] PV diagrams, we have derived nucleus-to-disk rotation curves of the observed galaxies. The rotation curves rise steeply within the central few hundred parsecs, indicating a rapidly rotating nuclear disk and mass concentration near the nucleus.