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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Аннотация

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.

Авторлар туралы

P. Colom

LESIA, Observatoire de Paris-Meudon, CNRS, UPMC

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

N. Ashimbaeva

Sternberg Astronomical Institute

Email: lekht@sai.msu.ru
Ресей, Moscow, 119234

E. Lekht

Sternberg Astronomical Institute

Хат алмасуға жауапты Автор.
Email: lekht@sai.msu.ru
Ресей, Moscow, 119234

M. Pashchenko

Sternberg Astronomical Institute

Email: lekht@sai.msu.ru
Ресей, Moscow, 119234

G. Rudnitskii

Sternberg Astronomical Institute

Email: lekht@sai.msu.ru
Ресей, Moscow, 119234

A. Tolmachev

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

Email: lekht@sai.msu.ru
Ресей, Pushchino, Moscow region, 142290

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