A new determination of the thickness of the galactic disk from H I-observations and a discussion of some consequences for galactic mass models

Details A new determination of the thickness of the galactic disk from H I-observations and a discussion of some consequences for galactic mass models A new determination of the thickness of the galactic disk from H I-observations and a discussion of some consequences for galactic mass models

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....76...24c&link_type=abstract

Astronomy and Astrophysics, vol. 76, no. 1, June 1979, p. 24-34. Deutsche Forschungsgemeinschaft

Astronomy and Astrophysics

Astrophysics

31

Density Distribution, Galactic Mass, Galactic Structure, Gas Density, H Lines, Hydrogen Clouds, Interstellar Gas, Milky Way Galaxy, Disks (Shapes), Least Squares Method, Neutral Gases, Nonlinear Equations, Radial Velocity, Stellar Mass, Stellar Models, Taylor Series, Terminal Velocity, Thickness

Scientific paper

The density distribution of neutral hydrogen perpendicular to the galactic plane has been determined from 21-cm line observations near terminal velocity of the measured line profiles. For this, a general expression for the observed line shape in this velocity range has been derived that permits a unique recognition of terminal velocity in the observed line profiles. The density distribution derived from high-resolution 21-cm line measurements with a 100-m telescope shows a Gaussian core and extended exponential wings. This can be understood as the equilibrium distribution of an isothermal gas in a galactic force function. By a nonlinear least-squares fitting routine the parameters of this density distribution have been derived, and the bias introduced by interstellar clouds disturbing this equilibrium has been estimated. An alternative interpretation of the extended wings of the density distribution by a two-component gas is shown to be contradicted by the observations. Therefore the observed scale-height values can be interpreted in terms of an equivalent thickness of the total mass of the galactic disk in a column perpendicular to the galactic plane resulting in expressions for the variation of the dynamical thickness and the total mass density for z 0 with galactic radius.

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