An analysis of the line shape for H2O maser emission peaks in star-forming regions |
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| Authors: | E E Lekht N A Silant’ev J E Mendoza-Torres A M Tolmachev |
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| Institution: | (1) Instituto Nacional de Astrofísica, óptica y Electrónica, Luis Enrique Erro No. 1, Apdo Postal 51 y 216, 72840 Tonantzintla, Puebla, México;(2) Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119899, Russia;(3) Pulkovo Astronomical Observatory, Russian Academy of Sciences, Pulkovskoe sh. 65, St. Petersburg, 196140, Russia;(4) Pushchino Radio Astronomy Observatory, Astrospace Center, Lebedev Physical Institute, Russian Academy of Sciences, Pushchino, Moscow oblast, 142292, Russia |
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| Abstract: | We analyze the line shape for emission peaks of H2O maser sources associated with star-forming regions by using the spectra obtained with the RT-22 radio telescope at the Pushchino Radio Astronomy Observatory. For five sources, we found the line profile of emission peaks to be asymmetric. In all cases, the left (high-frequency) line wing is higher than the right wing. Our analysis of the line shape yielded additional information on the structure and evolution of the maser sources under study. In G43.8-0.1, the emission feature was found to split up into two components. To explain the evolution of the 16.8 km s?1 line in NGC 2071, we propose a model in which the line-of-sight velocity gradient changes under the effect of a (non-shock) wave. The observed short-duration flares of individual emission features in W75N can emerge due to a chance projection of the numerous clumps of matter involved in Keplerian motion onto each other. |
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| Keywords: | radio sources star formation |
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