Kinematics and Distance of Water Masers in W3 IRS5

Details Kinematics and Distance of Water Masers in W3 IRS5 Kinematics and Distance of Water Masers in W3 IRS5

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..298i&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

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Scientific paper

We have measured the three-dimensional motions of water maser features in the massive star forming region W3 IRS5 with the VLBA. The masers are clustered in two groups which are associated with at least two different origins of the outflows. Positions of the outflow origins are close to the hyper-compact radio continuum sources, which are probably driving sources of the outflows. With kinematical model fitting for the maser feature cluster assuming an expanding flow with a spherically symmetric velocity field, we obtained a distance to the W3 IRS5 region as 1.88+/-0.28 kpc. The two outflows are roughly parallel to each other and to the global outflow seen in CO (J=2--1) emission. This suggests that the massive star cluster in the W3 IRS5 region was created through formation of hierarchical structure of the parent molecular core with keeping the angular momentum vector which may be parallel to the directions of the present outflows. With statistical analysis of spatial and velocity distribution of the maser spots using two-point correlation function and rms and meidan values of the velocity differences, we found that such structure is dominated by turbulent motions on the scale of 0.01--300 AU.

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