The empirical Gaia G-band extinction coefficient

被引:57
作者
Danielski, C. [1 ,2 ]
Babusiaux, C. [1 ,3 ]
Ruiz-Dern, L. [1 ]
Sartoretti, P. [1 ]
Arenou, F. [1 ]
机构
[1] PSL Res Univ, CNRS, Observ Paris, GEPI, 5 Pl Jules Janssen, F-92190 Meudon, France
[2] Sorbonne Univ, UMR 7095, CNRS, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France
[3] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France
基金
美国安德鲁·梅隆基金会; 美国国家科学基金会; 美国国家航空航天局;
关键词
methods: data analysis; methods: statistical; techniques: photometric; dust; extinction; stars: fundamental parameters; SKY SURVEY; CALIBRATION; EVOLUTION; SHAPES;
D O I
10.1051/0004-6361/201732327
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. The first Gaia data release unlocked the access to photometric information for 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. Aims. 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. Methods. 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 APOGEE DR13 and LAMOST DR2 surveys, respectively. We implemented a Markov chain Monte Carlo method where we used (G - K-S)(0) versus T-eff and (J - K-S)(0) versus (G - K-S)(0) calibration relations to estimate the extinction coefficient kG and we quantify its corresponding confidence interval via bootstrap resampling. We tested our method on samples of red giants and main sequence stars, finding consistent solutions. Results. We present here the determination of the Gaia extinction coefficient through a completely empirical method. Furthermore we provide the scientific community with a formula for measuring the extinction coefficient as a function of stellar effective temperature, the intrinsic colour (G - K-S)(0), and absorption.
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页数:8
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