论文标题
Ariadne：通过SED配件测量准确而精确的恒星参数
ARIADNE: Measuring accurate and precise stellar parameters through SED fitting
论文作者
论文摘要
准确测量恒星参数是提高我们对可观察到宇宙的理解的关键目标。但是，当前方法受到许多因素的限制，特别是这些方法是基础进化或大气模型的基础，这些偏见和物理假设是这些方法所依赖的模型。在这里，我们介绍了代码频谱能量分配贝叶斯模型平均钳工（Ariadne），该模型通过使用贝叶斯模型平均来解决所有恒星模型的信息来解决此问题，以获得准确而精确的值。该代码使用光谱能量分布拟合方法，结合精确的Gaia距离，以测量温度，log G，[fe/h]，$ _ {\ text V} $和恒星的半径。当与经过跨度测量的半径Ariadne相比，在广泛的恒星参数上产生了极好的一致性值，平均分数差仅为0.001 $ \ pm $ 0.070。目前，我们合并了六个不同的型号，在某些情况下，我们发现它们之间的显着偏移，在温度和半径上分别达到550 K和0.6 r $ _ \ odot $的差异。例如，恒星半径中的这种偏移会导致行星半径的差异为60％，在结合不同模型的结果时否定了同质性。我们还发现了小于0.4-0.5 r $ _ \ odot $的恒星的趋势，即使总体范围在干涉测量的不确定性之内，这表明需要做更多的工作来更好地对这些恒星进行建模。我们倡导使用Ariadne提供附近A至M DWARFS的改进的批量参数，以进行未来的研究。
Accurately measuring stellar parameters is a key goal to increase our understanding of the observable universe. However, current methods are limited by many factors, in particular, the biases and physical assumptions that are the basis for the underlying evolutionary or atmospheric models, those that these methods rely upon. Here we introduce our code spectrAl eneRgy dIstribution bAyesian moDel averagiNg fittEr (ARIADNE), which tackles this problem by using Bayesian Model Averaging to incorporate the information from all stellar models to arrive at accurate and precise values. This code uses spectral energy distribution fitting methods, combined with precise Gaia distances, to measure the temperature, log g, [Fe/H], A$_{\text V}$, and radius of a star. When compared with interferometrically measured radii ARIADNE produces values in excellent agreement across a wide range of stellar parameters, with a mean fractional difference of only 0.001 $\pm$ 0.070. We currently incorporate six different models, and in some cases we find significant offsets between them, reaching differences of up to 550 K and 0.6 R$_\odot$ in temperature and radius, respectively. For example, such offsets in stellar radius would give rise to a difference in planetary radius of 60%, negating homogeneity when combining results from different models. We also find a trend for stars smaller than 0.4-0.5 R$_\odot$, which shows more work needs to be done to better model these stars, even though the overall extent is within the uncertainties of the interferometric measurements. We advocate for the use of ARIADNE to provide improved bulk parameters of nearby A to M dwarfs for future studies.
