The Taurus-Auriga-Perseus complex of dark clouds. I - Density structure

Details The Taurus-Auriga-Perseus complex of dark clouds. I - Density structure The Taurus-Auriga-Perseus complex of dark clouds. I - Density structure

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...149..273c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 149, no. 2, Aug. 1985, p. 273-282.

Astronomy and Astrophysics

Astronomy

111

Galactic Structure, Interstellar Matter, Milky Way Galaxy, Molecular Clouds, Nebulae, Space Density, Colorimetry, Density Distribution, Interstellar Extinction, Sky Surveys (Astronomy), Star Distribution

Scientific paper

Star counts covering all the dark clouds of A(v) greater than 1 mag in the Taurus-Auriga-Perseus complex have been carried out on the red prints of the Palomar Observatory Sky Survey with an about 2.5 arcmin resolution. They facilitate the sketch of a high resolution picture of the local interstellar medium within 200 pc from the sun from l exponent II = 160 to 180 deg and from b exponent II = -10 to -20 deg. The distance of the complex is discussed. The mass of the Perseus complex is about 7000 solar masses. For the Taurus complex a mass of 6500 to 9500 solar masses is derived and most of the mass is an extended halo. The star counts are used to study the density, mass and column density distribution in dark clouds. It is found that n(r) varies inversely with r exponent -1/3 fitting well the observed visual extinction maps. Visual extinction towards other local dark clouds are also fitted by the same density law, suggesting a similarity in the formation and evolution mechanisms of dark clouds. Larson's (1981) relation between velocity dispersion and radius arises as a consequence of the gas density distribution in molecular clouds, if they are in virial equilibrium.

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