Early-type disk galaxies: Structure and kinematics

• Published in: Astronomy reports Vol. 52; no. 2; pp. 79 - 93
• Main Authors: Zasov, A. V., Moiseev, A. V., Khoperskov, A. V., Sidorova, E. A.
• Format: Journal Article
• Language: English
• Published: Dordrecht SP MAIK Nauka/Interperiodica 01.02.2008
• Subjects: Astronomy; Observations and Techniques; Physics; Physics and Astronomy; 98.62.Hr; 98.62.Dm; 98.62.Ck; 98.52.Lp; 98.52.Nr
• ISSN: 1063-7729; 1562-6881
• DOI: 10.1134/S1063772908020017

Spectroscopic observations of three lenticular (S0) galaxies (NGC 1167, NGC 4150, and NGC 6340) and one SBa galaxy (NGC 2273) have been taken with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences aimed to study the structure and kinematic properties of early-type disk galaxies. The radial profiles of the stellar radial velocities and the velocity dispersion are measured. N -body simulations are used to construct dynamical models of galaxies containing a stellar disk, bulge, and halo. The masses of individual components are estimated formaximum-mass disk models. A comparison of models with estimated rotational velocities and the stellar velocity dispersion suggests that the stellar disks in lenticular galaxies are “overheated”; i.e., there is a significant excess velocity dispersion over the minimum level required to maintain the stability of the disk. This supports the hypothesis that the stellar disks of S0 galaxies were subject to strong gravitational perturbations. The relative thickness of the stellar disks in the S0 galaxies considered substantially exceed the typical disk thickness of spiral galaxies.