Back to Search Start Over

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

Authors :
P. Colom
M. I. Pashchenko
E. E. Lekht
N. T. Ashimbaeva
A. M. Tolmachev
G. M. Rudnitskii
Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109))
Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Source :
Astronomicheskii Zhurnal / Astronomy Reports, Astronomicheskii Zhurnal / Astronomy Reports, MAIK Nauka/Interperiodica, 2019, 63 (7), pp.565-570. ⟨10.1134/S1063772919070047⟩
Publication Year :
2019
Publisher :
HAL CCSD, 2019.

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.

Details

Language :
English
ISSN :
10637729 and 15626881
Database :
OpenAIRE
Journal :
Astronomicheskii Zhurnal / Astronomy Reports, Astronomicheskii Zhurnal / Astronomy Reports, MAIK Nauka/Interperiodica, 2019, 63 (7), pp.565-570. ⟨10.1134/S1063772919070047⟩
Accession number :
edsair.doi.dedup.....693cf0ee1d1bdeddda24c0bf12b39393
Full Text :
https://doi.org/10.1134/S1063772919070047⟩