Volume 575, March 2015
|Number of page(s)||17|
|Section||Catalogs and data|
|Published online||19 February 2015|
OH and H2O maser variations in W33B⋆
LESIA, Observatoire de Paris, Section de Meudon, CNRS, UPMC, Université
5 place Jules Janssen,
2 Lomonosov Moscow State University, Sternberg Astronomical Institute, 13 Universitetskij prospekt, Moscow 119234, Russia
Received: 19 November 2013
Accepted: 22 October 2014
Context. The active star-forming region W33B is a source of OH and H2O maser emission located in distinct zones around the central object.
Aims. The aim was to obtain the complete Stokes pattern of polarised OH maser emission and to trace its variability and to investigate flares and long-term variability of the H2O maser and evolution of individual emission features.
Methods. Observations in the OH lines at a wavelength of 18 cm were carried out on the Nançay radio telescope (France) at a number of epochs in 2008−2014; H2O line observations (long-term monitoring) at λ = 1.35 cm were performed on the 22 m radio telescope of the Pushchino Radio Astronomy Observatory (Russia) between 1981 and 2014.
Results. We have observed strong variability of the emission features in the main 1665- and 1667 MHz OH lines as well as in the 1612 MHz satellite line. Zeeman splitting has been detected in the 1665 MHz OH line at 62 km s-1 and in the 1667 MHz line at 62 and 64 km s-1. The magnetic field intensity was estimated to be from 2 to 3 mG. The H2O emission features form filaments, chains with radial-velocity gradients, or more complicated structures including large-scale ones.
Conclusions. Long-term observations of the hydroxyl maser in the W33B region have revealed narrowband polarised emission in the 1612 MHz line with a double-peak profile characteristic of type IIb circumstellar masers. The 30 year monitoring of the water-vapour maser in W33B showed several strong flares of the H2O line. The observed radial-velocity drift of the H2O emission features suggests propagation of an excitation wave in the masering medium with a gradient of radial velocities. In OH and H2O masers some turbulent motions of material are inferred.
Key words: masers / ISM: magnetic fields / ISM: molecules / ISM: lines and bands / ISM: individual objects: W33B
The spectra of Fig. 7 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/575/A49 or at http://comet.sai.msu.ru/~gmr/Maser_monitoring/W33B
© ESO, 2015
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