论文标题
通过星团的CMD估计恒星参数的基础：开放（NGC2360）和球形（NGC 5272）
Fundamentals of Stellar Parameters Estimation through CMD of Star Clusters: Open (NGC2360) and Globular (NGC 5272)
论文作者
论文摘要
在这项工作中广泛介绍了开放群集NGC 2360和Globular clusters-NGC 5272的基本原理。在这里，全面讨论了通过在颜色幅度图（CMDS）上手动拟合适当的同丝来评估恒星参数的评估。使用孔径数学工具（APT），在G，R和I标准带滤波器图像上进行了孔径光度法和PSF拟合光度法，以获得相应的CMD。此外，为了实现恒星参数，详细描述了等线构拟合。关于恒星参数评估的这项工作已达到以下结果：NGC 2360的年龄为708 MYR，具有金属性，[Fe/H]为-0.15，而NGC 5272的年龄为11.56 Gyrs的年龄为11.56 Gyrs，具有金属性，[Fe/H]，[Fe/H]，of -1.57。此外，对于NGC 2360，星际红色，E（B-V）和距离模量DM分别为0.12和11.65。而对于NGC 5272，星际红色以E（B-V）= 0.015的形式获得，并且距离模量为DM = 15.1。发现这些恒星参数的值与基于IRAF分析技术的文献中提供的结果紧密近似。对于两个开始簇，包括半径，质量和温度的分布以及初始质量函数（IMF）。因此，本文将有助于通过天文学光度法分析来洞悉评估恒星参数，该分析将连续提高对我们宇宙的理解。应当指出的是，从前景/背景恒星中清除CMD上的簇群，清除虚假对象，错误估计和成员确定的确定，并被视为单独的分析项目。
The fundamentals of estimating essential stellar parameters of an open cluster-NGC 2360 and globular clusters-NGC 5272 are presented extensively in this work. Here, the evaluation of stellar parameters, by manually fitting the appropriate isochrones on the color magnitude diagrams (CMDs), of the selected star clusters is discussed comprehensively. Aperture photometry and PSF fitting photometry are conducted on g, r, and i standard band filter images of Sloan Digital Sky Survey (SDSS) using the aperture photometry tool (APT) to obtain the respective CMDs. Further, to achieve the stellar parameters, isochrone fitting is described in detail. This work on stellar parameters evaluation has attained the following results: age of NGC 2360 is found to be 708 Myrs with metallicity, [Fe/H], of -0.15, whereas NGC 5272 is having age of 11.56 Gyrs with metallicity, [Fe/H], of -1.57. Additionally, the interstellar reddening, E(B-V), and distance modulus, DM, for NGC 2360 are obtained as 0.12 and 11.65, respectively. While, for NGC 5272, the interstellar reddening is attained as E(B-V)=0.015, and the distance modulus is DM=15.1. The values of these stellar parameters are found to be in close approximation with the results provided in the literature based on the IRAF analysis technique. The distribution of radii, masses, and temperatures are included along with the initial mass function (IMF) for both the start clusters. Thus, this article would aid in providing insight into the evaluation of stellar parameters by the astronomical photometry analysis which would successively upsurge the understanding of our universe. It should be noted that the cleaning of cluster population on the CMDs from the foreground/background stars, clearing of spurious objects, error estimations and the membership determination are not carried out in this work and are considered as separate project for analysis.
