Journal
ASTROPHYSICAL JOURNAL
Volume 693, Issue 1, Pages 413-418Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/693/1/413
Keywords
astrometry; Galaxy: structure; stars: individual (G59.7+0.1, W 51 IRS2); techniques: interferometric
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Funding
- Chinese NSF [NSF 10673024, NSF 10733030, NSF 10703010, NSF 10621303]
- NBRPC [2007CB815403]
- DFG Priority Programme [1177]
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We report trigonometric parallaxes for G59.7+0.1 and W 51 IRS2, corresponding to distances of 2.16+(0.10)(-0.09) kpc and 5.1+(2.9)(-1.4) kpc, respectively. The distance to G59.7+0.1 is smaller than its near kinematic distance and places it between the Carina-Sagittarius and Perseus spiral arms, probably in the Local (Orion) spur. The distance to W 51 IRS2, while subject to significant uncertainty, is close to its kinematic distance and places it near the tangent point of the Carina-Sagittarius arm. It also agrees well with a recent estimate based on O-type star spectro/photometry. Combining the distances and proper motions with observed radial velocities gives the full space motions of the star-forming regions. We find modest deviations of 5-10 km s(-1) from circular Galactic orbits for these sources, both counter to Galactic rotation and toward the Galactic center.
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