Evidence for Co-Propagation of 4765- and 1720-MHz OH Masers in Star-Forming Regions

Details Evidence for Co-Propagation of 4765- and 1720-MHz OH Masers in Star-Forming Regions Evidence for Co-Propagation of 4765- and 1720-MHz OH Masers in Star-Forming Regions

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005ap%26ss.295...37n&link_type=abstract

Astrophysics and Space Science, Volume 295, Issue 1-2, pp. 37-42

Astronomy and Astrophysics

Astrophysics

1

Masers, Stars: Formation, Ism: Molecules, Radio Lines: Ism, H Ii Regions

Scientific paper

Two star-forming regions Cepheus A and W75N, were searched for the 4765-MHz OH maser emission using the multi-element radio linked interferometer network (MERLIN). The excited OH emission has an arc-like structure of 40 mas in Cep A and a linear structure of size 45 mas in W75N. We also found the 1720-MHz line in Cep A and Hutawarakorn [MNRAS 330 (2002) 349] reported the 1720-MHz emission in W75N. The 1720- and 4765-MHz OH spots coincided in space within 60 mas and in velocity within 0.3 km s-1 in both targets implying that both maser transitions arise from the same region. According to the modelling by Gray [MNRAS 252 (1991) 30] the 1720/4765-MHz co-propagation requires a low density, warm environment. The masers lie at the edges of H II regions where such conditions are expected.

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