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


如何引用文章

全文:

开放存取 开放存取
受限制的访问 ##reader.subscriptionAccessGranted##
受限制的访问 订阅存取

详细

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.

作者简介

P. Colom

LESIA, Observatoire de Paris-Meudon, CNRS, UPMC

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

N. Ashimbaeva

Sternberg Astronomical Institute

Email: lekht@sai.msu.ru
俄罗斯联邦, Moscow, 119234

E. Lekht

Sternberg Astronomical Institute

编辑信件的主要联系方式.
Email: lekht@sai.msu.ru
俄罗斯联邦, Moscow, 119234

M. Pashchenko

Sternberg Astronomical Institute

Email: lekht@sai.msu.ru
俄罗斯联邦, Moscow, 119234

G. Rudnitskii

Sternberg Astronomical Institute

Email: lekht@sai.msu.ru
俄罗斯联邦, Moscow, 119234

A. Tolmachev

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

Email: lekht@sai.msu.ru
俄罗斯联邦, Pushchino, Moscow region, 142290

补充文件

附件文件
动作
1. JATS XML

版权所有 © Pleiades Publishing, Ltd., 2019