2005/09/30 by G. Battaglia, F. Fraternali, T. Oosterloo +1 · 76 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Dark matter #Dark matter halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy rotation curve #Halo #Irregular galaxy #Rotation (mathematics) #Spiral galaxy #astro-ph
paper · pdf · doi:10.1051/0004-6361:20053210
published in Astronomy and Astrophysics 447(1), 49-62 (EDP Sciences) · Accepted for publication in A&A. Minor corrections
arxiv created 2005/10/20 · openalex publication_date 2006/01/27 · arxiv updated 2009/12/01 · openalex created_date 2017/01/06 · openalex updated_date 2026/07/31
We present a study of the distribution and dynamics of the nearby spiral galaxy NGC 5055 based on observations with the Westerbork Synthesis Radio Telescope. The gaseous disk of NGC 5055 extends out to about 40 kpc, equal to 3.5 R25, and shows a pronounced warp that starts at the end of the bright optical disk ( kpc). This very extended warp has large-scale symmetry, which along with the rotation period of its outer parts (1.5 Gyr at 40 kpc), suggests a long-lived phenomenon. The rotation curve rises steeply in the central parts up to the maximum velocity ( km s-1). Beyond the bright stellar disk (R25), it shows a decline of about 25 km s-1 and then remains flat out to the last measured point. The standard analysis with luminous and dark matter components shows the dynamical importance of the disk. The best fit to the rotation curve is obtained with a “maximum disk”. Less satisfactory fits with lighter disks help to set a firm lower limit of 1.4 to the mass-to-light ratio in F band of the disk. Such a “minimum disk” contributes about 60% of the observed maximum rotational velocity. NGC 5055 shows remarkable overall regularity and symmetry. A mild lopsidedness is noticeable, however, both in the distribution and kinematics of the gas. The tilted ring analysis of the velocity field led us to adopt different values for the kinematical centre and for the systemic velocity for the inner and the outer parts of the system. This has produced a remarkable result: the kinematical and geometrical asymmetries disappear, both at the same time. These results point at two different dynamical regimes: an inner region dominated by the stellar disk and an outer one, dominated by a dark matter halo offset with respect to the disk.