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Results of observations of the maser sources toward the W33C region(G12.8-0.2) carried out on the 22-m radio telescope of the Pushchino RadioAstronomy Observatory in the 1.35-cm H2O line and on the Large radio telescopein Nancay (France) in the main (1665 and 1667 MHz) and satellite (1612 and 1720MHz) OH lines are reported. Multiple, strongly variable short-lived H2Oemission 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 discovered in avelocity range of 35-41 km/s. Stokes parameters of maser emission in the mainOH lines 1665 and 1667 MHz were measured. Zeeman splitting was detected in the1665-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. A appreciable variability of Zeemansplitting components was observed at 39 and 39.8 km/s in both main lines. Theextended spectrum and fast variability of the H2O maser emission together withthe variability of the Zeeman splitting components in the main OH lines can bedue to the composite clumpy structure of the molecular cloud and to thepresence in it of large-scale rotation and bipolar outflow as well as ofturbulent motions of material.

The Source of Maser Emission W33C (G12.8-0.2)