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XI16 - An H₂O Maser survey towards BGPS sources in the Outer Galaxy

Short title: Xi et al. (2016)
Authors: Xi, Hong-WeiZhou, Jian-JunEsimbek, JarkenWu, GangHe, Yu-XinJi, Wei-GuangTang, Xiao-KeYuan, Ye
Journal: Research in Astronomy and Astrophysics, Volume 16, Issue 6, article id. 89 (2016).
Bibcode:

Target type: Bolocam

Abstract
We performed an H₂O maser survey towards 274 Bolocam Galactic Plane Survey (BGPS) sources with 852O masers, and five of them are new detections. The detection rate of H₂O masers in our sample is 9% which is very low. The detection rate of H₂O masers increases as the 1.1 mm flux density of BGPS sources increases, and both the peak flux density and luminosity of H₂O masers increase as the sources evolve. The detection rate of H₂O masers toward BGPS sources without HCO⁺ emission is low. The BGPS sources associated with both H₂O and CH₃OH masers seem to be more compact than those only associated with H₂O masers. This indicates that the sources with both masers may be in a relatively later evolutionary stage. The strongest H₂O maser source G133.715+01.217, also well known as W3 IRS 5 which has a flux density of 2.9x10³ Jy, was detected at eight different nearby positions. By measuring the correlation between the flux densities of these H₂O masers and their angular distance from the true source location, we get the influence radius... 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.

Abstract

We performed an H₂O maser survey towards 274 Bolocam Galactic Plane Survey (BGPS) sources with 852O masers, and five of them are new detections. The detection rate of H₂O masers in our sample is 9% which is very low. The detection rate of H₂O masers increases as the 1.1 mm flux density of BGPS sources increases, and both the peak flux density and luminosity of H₂O masers increase as the sources evolve. The detection rate of H₂O masers toward BGPS sources without HCO⁺ emission is low. The BGPS sources associated with both H₂O and CH₃OH masers seem to be more compact than those only associated with H₂O masers. This indicates that the sources with both masers may be in a relatively later evolutionary stage. The strongest H₂O maser source G133.715+01.217, also well known as W3 IRS 5 which has a flux density of 2.9x10³ Jy, was detected at eight different nearby positions. By measuring the correlation between the flux densities of these H₂O masers and their angular distance from the true source location, we get the influence radius... 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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Detection table from Xi et al. (2016)

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Non-detection table from Xi et al. (2016)