The source of maser emission in W33C (G12.8-0.2)

Colom, P.; Lekht, E.E.; Pashchenko, M.I.; Rudnitskii, G.M.

Авторы: Colom P., Lekht E.E., Pashchenko M.I., Rudnitskii G.M.
Журнал: Astronomy Reports
Том: 56
Номер: 10
Год издания: 2012
Издательство: Maik Nauka/Interperiodica Publishing
Местоположение издательства: Russian Federation
Первая страница: 731
Последняя страница: 740
DOI: 10.1134/S1063772912100034
Аннотация: The results of observations of the H2O and OH maser sources toward the region of W33C (G12.8–0.2) are reported. The observations were carried out on the 22-m radio telescope of the Pushchino Radio Astronomy Observatory in the 1.35-cm water-vapor line and on the Large Radio Telescope at Nancay (France), in the main (1665 and 1667 MHz) and satellite (1612 and 1720 MHz) OH lines. Multiple, strongly variable, short-lived H2O emission features were detected in a broad interval of radial velocities, from −7 to 55 km/s. OH maser emission in the 1667-MHz line was detected at velocities of 35–41 km/s. The Stokes parameters of the maser emission in the main OH lines 1665 and 1667 MHz were measured. Zeeman splitting was detected in the 1665-MHz line at 33.4 and 39.4 km/s, and in the 1667 MHz line only at 39.4 km/s. The magnetic-field intensity was estimated. Appreciable variability of the Zeeman splitting components was observed at 39 and 39.8 km/s in both main lines. The extended spectrum and fast variability of the H2O maser emission, together with the variability of the Zeeman splitting components in the main OH lines, may indicate a composite clumpy structure of the molecular cloud and the presence of large-scale rotation, bipolar outflows, and turbulent motions of material in this cloud.
Добавил в систему: Лехт Евгений Евгеньевич

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