Erratum: Exploring the M-dwarf Luminosity-Temperature-Radius relationships using Gaia DR2
Erratum: Exploring the M-dwarf Luminosity-Temperature-Radius relationships using Gaia DR2
复制标题
勘误表：使用 Gaia DR2 探索 M 矮星光度-温度-半径关系
DOI：
10.1093/mnras/staa926
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发表时间：
2020
影响因子：
4.8
通讯作者：
Morrell S
中科院分区：
文献类型：
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作者：
Morrell S
这是一篇论文“Exploring the M-dwarf Luminosity-Temperature-Radius relationships using Gaia DR 2”的勘误表，发表在MNRAS 489，2615-2633（2019）。我们已经发现了两个重要的问题，损害了在这项工作中进行的拟合的合成光度学。然而，这些问题在相反的意义上起作用，并有效地相互抵消。因此，经过修正后，这里提供的修订目录中99%的目标的半径与我们最初提供的值相差不到1%。然而，考虑到我们在最初的工作中测量恒星半径的精度，我们认为公布对衍生星表和关系的修订是明智的。完整的修订目录可通过匿名ftp到cdsarc在CDS上获得。u-strasbg.法国法郎（130.79法郎）。128.5）或通过http：//cdsarc. u-strasbg. fr/viz-bin/qcat？VI/156，埃克塞特大学ORE存储库（https：//doi. org/10.24378/exe。1683）和Morrell & Naylor（2019）的补充材料的GitHub存储库。[1]我们还提供了补充材料的修订版本，即表列的温度-半径-光度关系。根据这些修订，我们认为还应该包括并描述我们对计算恒星参数不确定性的过程所做的改进。我们现在将详细介绍问题，以及我们已经应用的补救措施。正如Evans et al.（2018），最初描述于Jordi et al.（2010），使用Vega设置Gaia Data Release 2（DR 2）测光系统的零点通量f λ（参见Evans等人2018的公式2）。这个零点的参考SED是一颗A0 V星星的SED，它来自Kurucz/ATLAS 9 Vega光谱，Teff= 9550 K，log（g）= 3.95 dex，[Fe/H]=− 0.5，νmicro= 2 km s− 1。这个SED被归一化，使得λ= 550 nm处的通量密度为λ550= 3.66× 10− 11 Wm− 2 nm− 1。由于生成用于拟合的网格的代码中的错误配置，在我们的原始工作中，合成测光的零点通量由Bohlin & Gilliland（2004）的Vega光谱提供。这给Gaia DR 2合成测光引入了系统零点误差，ZPBP=− 0.030，ZPRP=− 0.028。在修订后的目录中，拟合是在网格上进行的，零点校正与Evans等人的规定一致。（2018年）。
This is an erratum for the paper ‘Exploring the M-dwarf Luminosity–Temperature–Radius relationships using Gaia DR2’, published in MNRAS 489, 2615–2633 (2019). We have discovered two important issues compromising the synthetic photometry underlying the fitting performed in this work. However, these issues act in the opposite sense, and effectively work to counteract each other. As a result, after being corrected, the radii of 99 percent of the targets in the revised catalogue presented here differ by less than 1 per cent from the values we originally presented. However given the precision to which we measured stellar radii in the original work we thought it prudent to publish revisions to the derived catalogues and relations. The full revised catalogue is available at CDS via anonymous ftp to cdsarc. u-strasbg. fr (130.79. 128.5) or via http://cdsarc. u-strasbg. fr/viz-bin/qcat? VI/156, the University of Exeter ORE repository (https://doi. org/10.24378/exe. 1683) and the GitHub repository of supplementary material for Morrell & Naylor (2019). 1 We also provide a revised version of the supplementary material, which are the tabulated temperature-radius-luminosity relationships. In light of these revisions, we thought it prudent to also include, and describe, improvements we have made to the process through which the uncertainties of our stellar parameters are calculated. We will now detail the issues, and the remediations which we have applied. As presented in Evans et al.(2018), and originally described in Jordi et al.(2010), the zero-point flux f◦ λ for the Gaia Data Release 2 (DR2) photometric system is set using Vega (see equation 2 of Evans et al. 2018). The reference SED for this zero-point is that of an A0V star from the Kurucz/ATLAS9 Vega spectrum with Teff= 9550 K, log (g)= 3.95 dex,[Fe/H]=− 0.5 and νmicro= 2 km s− 1. This SED is normalized such that the flux density at λ= 550 nm is λ550= 3.66× 10− 11 Wm− 2 nm− 1. Due to a misconfiguration in the code that produced the grids used for the fitting, the zeropoint flux for the synthetic photometry in our original work was instead provided by the Vega spectrum of Bohlin & Gilliland (2004). This introduced a systematic zero-point error into the Gaia DR2 synthetic photometry of ZPBP=− 0.030 and ZPRP=− 0.028. In the revised catalogue, the fitting is performed on grids with the zero-point corrected to be consistent with that prescribed in Evans et al.(2018).