Using red clump stars to correct the Gaia DR1 parallaxes
Using red clump stars to correct the Gaia DR1 parallaxes
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DOI：
10.1051/0004-6361/201630066
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发表时间：
2017-01
影响因子：
6.5
通讯作者：
G. Davies;M. Lund;A. Miglio;Y. Elsworth;J. Kuszlewicz;Thomas S. H. North;B. Rendle;W. Chaplin;T. Rodrigues;T. Campante;L. Girardi;S. Hale;O. Hall;Caitlin D. Jones;S. Kawaler;I. Roxburgh;Mathew Schofield
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文献类型：
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作者：
G. Davies;M. Lund;A. Miglio;Y. Elsworth;J. Kuszlewicz;Thomas S. H. North;B. Rendle;W. Chaplin;T. Rodrigues;T. Campante;L. Girardi;S. Hale;O. Hall;Caitlin D. Jones;S. Kawaler;I. Roxburgh;Mathew Schofield
最近的结果表明，Gaia DR1TGAS距离与通过食双星或红巨星上的星震学确定的光度所获得的距离之间存在张力。我们使用由星震学识别和表征的红团星的K-S波段光度来做出独立的距离估计。我们的结果表明，Gaia TGAS距离包含一个系统误差，该误差随着距离的增加而减小。我们提出了一种校正，以减小这种偏移量作为视差的函数，该函数对于开普勒场和小于~1.6 mA的视差值是有效的。对于大于此的视差，我们发现与先前公布的值一致。我们注意到疏散星团M67的TGAS距离显示出很高的不一致程度，这是很难纠正的。
Recent results have suggested that there is tension between the Gaia DR1 TGAS distances and the distances obtained using luminosities determined by eclipsing binaries or asteroseismology on red giant stars. We use the K s -band luminosities of red clump stars, identified and characterized by asteroseismology, to make independent distance estimates. Our results suggest that Gaia TGAS distances contain a systematic error that decreases with increasing distance. We propose a correction to mitigate this offset as a function of parallax that is valid for the Kepler field and values of parallax that are less than ~1.6 mas. For parallaxes greater than this, we find agreement with previously published values. We note that the TGAS distances to the red clump stars of the open cluster M67 show a high level of disagreement that is difficult to correct for.