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Evolution of Maser Emission in the Region of Active Star Formation G43.8–0.1. I. OH Maser Emission at 18 cm

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Abstract

The results of observations of OH maser emission in the star-forming region G43.8–0.1 are presented. In spite of strong flux-density variations in the main lines at 1665 and 1667 MHz, the radial velocities of the spectral features varied only slightly. The main spectral features are identified with maser spots in previously published maps for epochs 1993 and 2001. It is suggested that the regions of OH maser emission may be elongated, nonuniform structures with weak radial velocity gradients (larger-scale analogs of water-maser filaments). The line-of-sight magnetic fields are determined for two Zeeman pairs, which remained essentially constant over at least 17 years.

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Authors and Affiliations

  1. LESIA, Observatoire de Paris-Meudon, CNRS, UPMC, Université Paris-Diderot, 92195, Meudon Cedex, France

    P. Colom

  2. Sternberg Astronomical Institute, Moscow State University, Moscow, 119234, Russia

    N. T. Ashimbaeva, E. E. Lekht, M. I. Pashchenko & G. M. Rudnitskii

  3. Pushchino Radio Astronomy Observatory, Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Pushchino, Moscow region, 142290, Russia

    A. M. Tolmachev

Authors
  1. P. Colom
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  2. N. T. Ashimbaeva
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  3. E. E. Lekht
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  4. M. I. Pashchenko
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  5. G. M. Rudnitskii
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  6. A. M. Tolmachev
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Correspondence to E. E. Lekht.

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Russian Text © The Author(s), 2019, published in Astronomicheskii Zhurnal, 2019, Vol. 96, No. 7, pp. 563–569.

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Colom, P., Ashimbaeva, N.T., Lekht, E.E. et al. Evolution of Maser Emission in the Region of Active Star Formation G43.8–0.1. I. OH Maser Emission at 18 cm. Astron. Rep. 63, 565–570 (2019). https://doi.org/10.1134/S1063772919070047

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  • DOI: https://doi.org/10.1134/S1063772919070047

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