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Kinematics of the Scorpius-Centaurus OB association

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Abstract

A fine structure related to the kinematic peculiarities of three components of the Scorpius-Centaurus association (LCC, UCL, and US) has been revealed in the UV-velocity distribution of Gould Belt stars. We have been able to identify the most likely members of these groups by applying the method of analyzing the two-dimensional probability density function of stellar UV velocities that we developed. A kinematic analysis of the identified structural components has shown that, in general, the center-of-mass motion of the LCC, UCL, and US groups follows the motion characteristic of the Gould Belt, notably its expansion. The entire Scorpius-Centaurus complex is shown to possess a proper expansion with an angular velocity parameter of 46 ± 8 km s−1 kpc−1 for the kinematic center with l 0 = −40° and R 0 = 110 pc found. Based on this velocity, we have estimated the characteristic expansion time of the complex to be 21 ± 4 Myr. The proper rotation velocity of the Scorpius-Centaurus complex is lower in magnitude, is determined less reliably, and depends markedly on the data quality.

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Authors and Affiliations

  1. Pulkovo Astronomical Observatory, Russian Academy of Sciences, Pulkovskoe sh. 65, St. Petersburg, 196140, Russia

    V. V. Bobylev & A. T. Bajkova

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  1. V. V. Bobylev
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  2. A. T. Bajkova
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Correspondence to V. V. Bobylev.

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Original Russian Text © V.V. Bobylev, A.T. Bajkova, 2007, published in Pis’ma v Astronomicheskiĭ Zhurnal, 2007, Vol. 33, No. 9, pp. 643–656.

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Bobylev, V.V., Bajkova, A.T. Kinematics of the Scorpius-Centaurus OB association. Astron. Lett. 33, 571–583 (2007). https://doi.org/10.1134/S1063773707090010

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  • DOI: https://doi.org/10.1134/S1063773707090010

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