Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...494..236w&link_type=abstract
Astrophysical Journal v.494, p.236
Astronomy and Astrophysics
Astronomy
20
Galaxies: Individual Ngc Number: Ngc 4321, Galaxies: Ism, Galaxies: Kinematics And Dynamics, Galaxies: Spiral, Hydrodynamics, Methods: Numerical
Scientific paper
Hydrodynamic simulations have been compared with high-resolution CO (J = 1-0) observations of the central region (R < 1.5 kpc) of NGC 4321. In the simulations, the evolution of a self-gravitating gas disk in gravitational potentials that suitably match the nuclear bar of NGC 4321 has been followed. Postulating that the nuclear bar of R ~ 16" governs nearby gas dynamics, we determine a set of parameters to reproduce the observed gas structure, which includes two trailing spirals and a dense nuclear concentration. The pattern speed of the nuclear bar is 65 km s-1 kpc-1, and the total gas mass in the central region is ~1.0-1.3 (Tg/104 K)1/2 x 109 M&sun;, where Tg is the gas kinematic temperature. In addition, the observed molecular spirals have been found to be short-lived but recurrent. It has been found that the observed gas features cannot be reproduced from the gravitational potential derived from a K'-band image if a constant mass-to-luminosity ratio is assumed. From the K'-band image and the gravitational potential of the best-fit analytical model, a two-dimensional map of the mass-to-K luminosity ratio (M/LK) has been obtained. This ratio ranges from 0.2 to 1.2 (M/L)&sun; in the central region; the smallest value occurs at star-forming regions located at each end of the nuclear bar. Our numerical approach is an effective way to estimate the mass distribution and the pattern speed in spiral galaxies.
Minezaki Takeo
Sakamoto Kazushi
Wada Keiichi
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