恒星参数干涉测量巡天：使用“恒星干涉测量管线”进行临边昏暗研究
Interferometric Survey of Stellar Parameters: Limb darkening study with the "Pipeline for Interferometric Measurements of Stars"
- Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学，蔚蓝海岸天文台，法国国家科学研究中心，拉格朗日实验室）
- Max Plank Institute for Astronomy（马克斯·普朗克天文学研究所）
- Space Sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège（列日大学，空间科学与技术及天体物理研究（STAR）研究所）
- LUPM, Univ Montpellier, CNRS（蒙彼利埃大学，法国国家科学研究中心，宇宙物质与粒子物理联合研究实验室）
- The CHARA Array of Georgia State University, Mount Wilson Observatory（佐治亚州立大学CHARA阵列，威尔逊山天文台）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
提出一种基于干涉测量、恒星大气模型及光谱测光数据的恒星参数估计方法，利用人工神经网络拟合强度轮廓，可精确测定Teff、log g和角直径，精度分别达1%、5%和0.5%，并改善质量与年龄测定。
AI中文摘要：
在许多天体物理领域，准确且无偏地确定恒星参数具有重要意义。因此，我们提出了一种改进的恒星参数估计方法，该方法基于干涉观测、恒星大气模型以及光谱和测光数据。通过在较大的光谱窗口内将强度轮廓模型拟合到干涉数据，并结合光谱和测光观测作为拟合的额外约束，来估计基本恒星参数。基于恒星大气模型，我们开发了一种算法，该算法训练人工神经网络（ANNs）来估计恒星在R、H和K三个波段的光谱和强度轮廓。这些人工神经网络覆盖的有效温度（Teff）范围为：矮星4500-7000 K，巨星2500-8000 K；表面重力（log g）范围分别为3.0-5.0 dex和-0.5-3.5 dex，并涵盖12个观测角度。因此，可以估计出一致且精确的恒星参数，如Teff、log g和角直径（$\ heta$）。我们利用CHARA阵列上的SPICA、MIRC-X和MYSTIC仪器对双鱼座ι（F7V）和白羊座δ（G9.5IIIb）进行了拟合，并利用VLTI/PIONIER的档案数据对半人马座α A和B（G2V和K1V）进行了拟合。在角直径估计方面，当使用一维恒星大气模型进行拟合时，我们达到了0.5%的精度。对于Teff和半径，我们获得了约1%的精度，而log g的精度为5%。通过演化模型，我们进一步展示了这些约束如何改善质量和年龄的测定，因为它们在质量方面达到了约2%的精度，在年龄方面达到了5-10%的精度。
英文摘要：
Accurate and unbiased determination of stellar parameters is of importance in many astrophysical domains. We therefore present an improved method to estimate stellar parameters, based on interferometric observations and stellar atmosphere models, as well as spectroscopic and photometric data. The fundamental stellar parameters were estimated by fitting a model of intensity profiles to interferometric data over a large spectral window and combining them with spectroscopic and photometric observations as an additional constraint on the fitting. Based on stellar atmosphere models, we have developed an algorithm that trains artificial neural networks (ANNs) to estimate the spectrum and intensity profile of a star over three bands: R, H, and K. The ANNs cover effective temperatures (Teff) ranging from 4500-7000 K for dwarf stars and 2500-8000 K for giant stars, with surface gravities (log g) ranging from 3.0-5.0 dex and -0.5-3.5 dex, respectively, and 12 viewing angles. As a result, consistent and precise stellar parameters, such as Teff, log g, and angular diameter ($θ$), can be estimated. We fitted $ι$ Psc (F7V) and $δ$ Ari (G9.5IIIb) observed with SPICA, MIRC-X, and MYSTIC at the CHARA Array, and archival data of $α$ Cen A and B (G2V and K1V) from VLTI/PIONIER with PIMS. For angular diameter estimations, when fitting with a one-dimensional stellar atmosphere model, we reached a precision of 0.5%. For Teff and radius, we obtained a precision of approximately 1%, while we obtained a precision of 5% for log g. Through evolutionary models, we further show how these constraints can improve the mass and age determination, as they attain a precision of approximately 2% for mass and 5-10% for age.
