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arXiv 1802.01670astro-ph.SRastro-ph.GA
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经验Gaia G带消光系数

The empirical Gaia G-band extinction coefficient

C. Danielski, C. Babusiaux, L. Ruiz-Dern, P. Sartoretti, F. Arenou

备注：
8 pages, 5 figures, accepted for publication in A&A
发表信息：
A&A 614, A19 (2018)
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摘要：

第一个盖亚数据发布解锁了对$G$波段11亿个光源的光度信息的访问。然而，考虑到大通带（如盖亚$G$带）的消光和光谱能量分布之间的高度简并性，为了利用盖亚数据，需要对星际红化进行校正。这份手稿的目的是提供红巨星和主序星的盖亚$G$波段消光系数$k_G$的经验估计，以便能够利用第一次数据发布DR 1。我们选择了两个单星样本：一个是红巨星，一个是主序星。这两个样本都是盖亚DR 1和2 MASS星表之间交叉匹配的结果;它们包括$G$ -、$J$ -和$Ks$ -波段的高质量测光。这些样本分别由APOGEE DR 13和LAMOST DR 2调查中检索到的温度和金属丰度信息进行了补充。我们实现了马尔可夫链蒙特卡罗方法，其中我们使用$(G-Ks)_0$与$T_\mathrm{eff}$和$(J-Ks)_0$与$(G-Ks)_0$校准关系来估计消光系数$k_G$，并通过自举响应方法量化其相应的置信区间。我们在红巨星和主序星的样本上测试了我们的方法，找到了一致的解决方案。我们在这里提出的盖亚消光系数的测定，通过一个完全经验的方法。此外，我们提供了科学界的公式来测量消光系数作为恒星有效温度，固有颜色$(G-Ks)_0$和吸收的函数。

英文摘要：

The first Gaia data release unlocked the access to the photometric information of 1.1 billion sources in the $G$-band. Yet, given the high level of degeneracy between extinction and spectral energy distribution for large passbands such as the Gaia $G$-band, a correction for the interstellar reddening is needed in order to exploit Gaia data. The purpose of this manuscript is to provide the empirical estimation of the Gaia $G$-band extinction coefficient $k_G$ for both the red giants and main sequence stars, in order to be able to exploit the first data release DR1. We selected two samples of single stars: one for the red giants and one for the main sequence. Both samples are the result of a cross-match between Gaia DR1 and 2MASS catalogues; they consist of high quality photometry in the $G$-, $J$- and $Ks$-bands. These samples were complemented by temperature and metallicity information retrieved from, respectively, APOGEE DR13 and LAMOST DR2 surveys. We implemented a Markov Chain Monte Carlo method where we used $(G-Ks)_0$ vs $T_\mathrm{eff}$ and $(J-Ks)_0$ vs $(G-Ks)_0$ calibration relations to estimate the extinction coefficient $k_G$ and we quantify its corresponding confidence interval via bootstrap resampling method. We tested our method on samples of red giants and main sequence stars, finding consistent solutions. We present here the determination of the Gaia extinction coefficient through a completely empirical method. Furthermore we provide the scientific community a formula for measuring the extinction coefficient as a function of stellar effective temperature, the intrinsic colour $(G-Ks)_0$ and absorption.

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