A search for 4750- and 4765-MHz OH masers in Southern Star Forming Regions

Details A search for 4750- and 4765-MHz OH masers in Southern Star Forming Regions A search for 4750- and 4765-MHz OH masers in Southern Star Forming Regions

2002-01-17

arxiv.org/abs/astro-ph/0201296v2

Mon.Not.Roy.Astron.Soc. 333 (2002) 307; Erratum-ibid. 366 (2006) 1119

Astronomy and Astrophysics

Astrophysics

Included an Erratum with Max as another author. This erratum was rejected by MNRAS (Feb 04) as it contained too much data. Res

Scientific paper

10.1046/j.1365-8711.2002.05428.x

We have used the Australia Telescope Compact Array (ATCA) to make a sensitive (5-$\sigma$ $\simeq$ 100 mJy) search for maser emission from the 4765-MHz $^2\Pi_{1/2}$ F=1$\to$0 transition of OH. Fifty five star formation regions were searched and maser emission with a peak flux density in excess of 100 mJy was detected toward fourteen sites, with ten of these being new discoveries. In addition we observed the 4750-MHz $^2\Pi_{1/2}$ F=1$\to$1 transition towards a sample of star formation regions known to contain 1720-MHz OH masers, detecting marginal maser emission from G348.550-0.979. If confirmed this would be only the second maser discovered from this transition. The occurrence of 4765-MHz OH maser emission accompanying 1720-MHz OH masers in a small number of well studied star formation regions has lead to a general perception in the literature that the two transitions favour similar physical conditions. Our search has found that the presence of the excited-state 6035-MHz OH transition is a much better predictor of 4765-MHz OH maser emission from the same region than is 1720-MHz OH maser emission. Combining our results with those of previous high resolution observations of other OH transitions we have examined the published theoretical models of OH masers and find that none of them predict any conditions in which the 1665-, 6035- and 4765-MHz transitions are simultaneously inverted. Erratum abstract: Dodson & Ellingsen (2002) included several observations with significant pointing errors, invalidating the upper limits found in these directions. These have now been reobserved or recalculated. A new table of upper limits has been generated, and two more masers that would have been seen have been found.

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