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A possible formation mechanism of the asymmetry in the H2O maser emission line

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Abstract

We present a possible formation mechanism of the asymmetry in the maser emission line of H2O sources associated with star-forming regions. Observations with the RT-22 radio telescope at the Pushchino Radio Astronomy Observatory are used. We analyze the line profiles of emission features in the sources G43.8-0.1, NGC 2071, and ON1. If the line is asymmetric, the left (low-velocity) wing is higher than the right wing. The proposed mechanism accounts for the observed asymmetry and makes it possible to estimate some physical parameters of the medium in the vicinity of a maser spot.

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Authors and Affiliations

  1. Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro No. 1, Apdo Postal 51 y 216, 72840, Tonantzintla, Puebla, México

    N. A. Silant’ev, E. E. Lekht & J. E. Mendosa-Torres

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

    N. A. Silant’ev

  3. Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119899, Russia

    E. E. Lekht

  4. Pushchino Radio Astronomy Observatory, Astrospace Center, Lebedev Physical Institute, Russian Academy of Sciences, Pushchino, Moscow oblast, 142292, Russia

    A. M. Tolmachev

Authors
  1. N. A. Silant’ev
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  2. E. E. Lekht
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  3. J. E. Mendosa-Torres
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  4. A. M. Tolmachev
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Translated from Pis’ma v Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l}\) Zhurnal, Vol. 28, No. 4, 2002, pp. 253–259.

Original Russian Text Copyright © 2002 by Silant’ev, Lekht, Mendosa-Torres, Tolmachev.

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Silant’ev, N.A., Lekht, E.E., Mendosa-Torres, J.E. et al. A possible formation mechanism of the asymmetry in the H2O maser emission line. Astron. Lett. 28, 217–222 (2002). https://doi.org/10.1134/1.1467256

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  • DOI: https://doi.org/10.1134/1.1467256

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