Abstract
Based on our H α interferometry and 21-cm and CO observations, we analyze the structure and kinematics of the interstellar medium around the stars WR 134 and WR 135. We conclude that the HI bubble found here previously is associated with WR 135, not with WR 134. High-velocity motions of ionized gas that can be interpreted as expansion of the gas swept up by the stellar wind with a velocity up to 50–80 km s−1 are observed around both stars. The line-of-sight velocity field of the ionized hydrogen in the Cygnus arm is shown to agree with the large-scale line-of-sight velocity distribution of the CO emission.
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Original Russian Text © T.G. Sitnik, T.A. Lozinskaya, 2009, published in Pis’ma v Astronomicheskiĭ Zhurnal, 2009, Vol. 35, No. 2, pp. 137–148.
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Sitnik, T.G., Lozinskaya, T.A. Structure and kinematics of the interstellar medium around WR 134 and WR 135. Astron. Lett. 35, 121–131 (2009). https://doi.org/10.1134/S1063773709020066
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DOI: https://doi.org/10.1134/S1063773709020066