2010/04/27 by О. К. Сильченко, Olga K. Sil'chenko, A. A. Smirnova +1
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Barred spiral galaxy #Bulge #Galactic Center #Galaxies: Formation, Evolution, Phenomena #Galaxy #Hubble sequence #Lenticular galaxy #Milky Way #Physics #Population #RADIUS #Spiral galaxy #Star formation #Stellar kinematics #Stellar population #Stellar, planetary, and galactic studies #astro-ph.CO
paper · pdf · doi:10.1134/s1063773710050026
published as Astronomy Letters, 2010, Vol.36, No.5, pp.319-328 · 9 pages, 7 figures, accepted to "Astronomy Letters"
arxiv created 2010/04/27 · arxiv updated 2010/04/28 · openalex publication_date 2010/05/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Using the method of two-dimensional spectroscopy, we have investigated the kinematics and distribution of the gas and stars at the center of the early-type spiral galaxy NGC 7177 with a mediumscale bar as well as the change in the mean age of the stellar population along the radius. A classical picture of radial gas inflow to the galactic center along the shock fronts delineated by dust concentration at the leading edges of the bar has been revealed. The gas inflow is observed down to a radius R = 1″.5−2″, where the gas flows at the inner Lindblad resonance concentrate in an azimuthally highly inhomogeneous nuclear star formation ring. The bar in NGC 7177 is shown to be thick in z coordinate—basically, it has already turned into a pseudo-bulge as a result of secular dynamical evolution. The mean stellar age inside the star formation ring, in the galactic nucleus, is old, ∼10 Gyr.Outside, at a distance R = 6″−8″ from the nucleus, the mean age of the stellar population is ∼2 Gyr. If we agree that the bar in NGC 7177 is old, then, obviously, the star formation ring has migrated radially inward in the last 1–2 Gyr, in accordance with the predictions of some dynamical models.