Observations of OH and H2O Maser Emission in the Star-Forming Region S128


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Abstract

Results of monitoring hydroxyl and water masers in the star-forming region S128 are presented. A large number of emission features in the 1665 MHz OH line have been detected in both circular polarizations. In spite of the strong variability of the flux density in the main 1665 MHz line, the radial velocities of the features remained constant. Zeeman splitting of the 1720MHz line equal to 0.86 km/s was detected, corresponding to a longitudinal magnetic field of 3.6 mG. The variability of the H2O emission has a cyclic character with a quasi-period of 4–14 yrs. The evolution of individual features confirms that the H2O sources A and B are associated with an ionization front between two colliding CO clouds, and shows that the activity was transferred from maser B to maser A in 1999–2001.

About the authors

N. T. Ashimbaeva

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lekht@sai.msu.ru
Russian Federation, Moscow, 119992

P. Colom

LESIA, Observatoire de Paris-Meudon, CNRS, UPMC

Email: lekht@sai.msu.ru
France, Meudon Cedex, 92195

E. E. Lekht

Lomonosov Moscow State University, Sternberg Astronomical Institute

Author for correspondence.
Email: lekht@sai.msu.ru
Russian Federation, Moscow, 119992

M. I. Pashchenko

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lekht@sai.msu.ru
Russian Federation, Moscow, 119992

G. M. Rudnitskii

Lomonosov Moscow State University, Sternberg Astronomical Institute

Email: lekht@sai.msu.ru
Russian Federation, Moscow, 119992

A. M. Tolmachev

Pushchino Radio Astronomy Observatory, Astro Space Center, Lebedev Physical Institute

Email: lekht@sai.msu.ru
Russian Federation, Pushchino, Moscow oblast, 142290

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