Trigonometric parallaxes of massive star forming regions: G012.88+0.48 and W33

We report trigonometric parallaxes for water masers in the G012.88+0.48 region and in the massive star forming complex W33 (containing G012.68−0.18, G012.81−0.19, G012.90−0.24, G012.90−0.26), from the Bar and Spiral Structure Legacy (BeSSeL) survey using the Very Long Baseline Array. The parallax di...

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Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2013-05, Vol.553, p.1-8
Main Authors: Immer, K., Reid, M. J., Menten, K. M., Brunthaler, A., Dame, T. M.
Format: Article
Language:English
Subjects:
astrometry
Astronomy
Kinematics
masers
Massive stars
Parallax
parallaxes
proper motions
Spectra
Spirals
Star formation
stars: distances
stars: formation
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Summary:We report trigonometric parallaxes for water masers in the G012.88+0.48 region and in the massive star forming complex W33 (containing G012.68−0.18, G012.81−0.19, G012.90−0.24, G012.90−0.26), from the Bar and Spiral Structure Legacy (BeSSeL) survey using the Very Long Baseline Array. The parallax distances to all these masers are consistent with \hbox{$2.40^{+0.17}_{-0.15}$}2.40-0.15+0.17 kpc, which locates the W33 complex and G012.88+0.48 in the Scutum spiral arm. Our results show that W33 is a single star forming complex at about two-thirds the kinematic distance of 3.7 kpc. The luminosity and mass of this region, based on the kinematic distance, have therefore been overestimated by more than a factor of two. The spectral types in the star cluster in W33 Main have to be changed by 1.5 points to later types.
ISSN:0004-6361
1432-0746
DOI:10.1051/0004-6361/201220793