Recent southern maser surveys

Caswell, J. L.

doi:10.1017/s1743921307012963

Cited by 1 publication

(1 citation statement)

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“…H 2 O, CH 3 OH and OH masers are common interstellar masers associated with a star formation region (SFR). H 2 O masers are the most common maser species in our MW (Caswell 2007). They are associated with both lowand high-mass SFRs.…”

Section: Introductionmentioning

confidence: 92%

An H₂O Maser survey towards BGPS sources in the Outer Galaxy

Zhou

Esimbek

et al. 2016

Res. Astron. Astrophys.

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We performed an H 2 O maser survey towards 274 Bolocam Galactic Plane Survey (BGPS) sources with 85 • < l < 193 • using the Nanshan 25 m radio telescope. We detected 25 H 2 O masers, and five of them are new detections. The detection rate of H 2 O masers in our sample is 9% which is very low. The detection rate of H 2 O masers increases as the 1.1 mm flux density of BGPS sources increases, and both the peak flux density and luminosity of H 2 O masers increase as the sources evolve. The detection rate of H 2 O masers toward BGPS sources without HCO + emission is low. The BGPS sources associated with both H 2 O and CH 3 OH masers seem to be more compact than those only associated with H 2 O masers. This indicates that the sources with both masers may be in a relatively later evolutionary stage. The strongest H 2 O maser source G133.715+01.217, also well known as W3 IRS 5 which has a flux density of 2.9×10 3 Jy, was detected at eight different nearby positions. By measuring the correlation between the flux densities of these H 2 O masers and their angular distance from the true source location, we get the influence radius r = 1 0.8 log( F0 3rms ). For our observations, strong sources can be detected anywhere within this radius. It is helpful to determine whether or not a weak maser nearby the strong maser is a true detection.

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Section: Introductionmentioning

confidence: 92%