标题： JWST空间任务的4项定律和幂次2定律的 Limb-Darkening 系数，采用高分辨率的PHOENIX球面模型 显示英文标题

标题： Limb-Darkening Coefficients for the 4-Term and Power-2 Laws for the JWST Space Mission, Adopting PHOENIX Spherical Models at High Resolution

摘要： 通过对观测的凌星系外行星或密近双星系统与理论光曲线进行比较来建模观测，需要精确了解恒星盘上特定强度的分布。 我们旨在通过提供广泛的大气边缘消光系数表来促进此类研究，这些表针对安装在詹姆斯韦伯太空望远镜上的NIRCam、NIRISS和NIRSpec仪器中的11个常用近红外和中红外波段。 边缘消光系数的计算基于球对称大气模型系列PHOENIX，具有高光谱分辨率（约$10^{6}$个波长），覆盖波长范围$0.1-6.0~\mu$米。模型计算基于太阳丰度，微湍流速度为1.0公里每秒$^{-1}$。 我们采用了两种更准确的参数化方法来确定系数：四项式定律和幂次两项式定律。 我们应用了Levenberg-Marquardt最小二乘法，并采用了一种策略，以确定接近边缘的观测角度余弦的临界值$\mu_{\rm crit}$，目的是提高数值精度。 边缘消光系数是基于总共306个大气模型得出的，这些模型覆盖了有效温度范围$2400-7800$开尔文，以及$\log g$之间3.0到5.5的日面重力加速度间隔。 我们讨论了幂次两项式定律和四次项定律提供的特定强度拟合质量，以及常用的二次方定律。 根据比较，我们推荐按偏好顺序使用四次项定律或幂次两项式定律。 显示英文摘要

摘要： Modeling observations of transiting exoplanets or close binary systems by comparing the observations with theoretical light curves requires precise knowledge of the distribution of specific intensities across the stellar disk. We aim to facilitate this type of research by providing extensive tabulations of limb-darkening coefficients for 11 frequently used near- and mid-infrared passbands on the NIRCam, NIRISS, and NIRSpec instruments installed on board the James Webb Space Telescope. The calculation of the limb-darkening coefficients was based on spherically symmetric atmosphere models from the PHOENIX series, with high spectral resolution (approximately $10^{6}$ wavelengths), and covering the wavelength range $0.1-6.0~\mu$m. The models were computed for solar composition, and a microturbulent velocity of 1.0 km s$^{-1}$. We adopted two of the more accurate parametrizations for the coefficients: the 4-term law, and the power-2 law. We applied the Levenberg-Marquardt least-squares minimization method, with a strategy to determine the critical value $\mu_{\rm crit}$ of the cosine of the viewing angle near the limb that is designed to improve numerical accuracy. The limb-darkening coefficients were derived based on a total of 306 atmosphere models covering an effective temperature range of $2400-7800$ K, and a $\log g$ interval between 3.0 and 5.5. We discuss the quality of the fits to the specific intensities provided by the power-2 and 4-term laws, as well as by the often used quadratic law. Based on a comparison, we recommend the use of the 4-term or power-2 laws, in that order of preference.