AI 中文总结
该研究利用多天文目录数据，区分银核与银晕蒭藁型变星类型，发现两者金属丰度分布、周期等特征存在显著差异，红外与光学波段的周期-星等相关性因尘埃反转。
AI 中文摘要
本研究旨在观测银河系核球、银晕中的蒭藁型变星（包括球状星团中的这类恒星）。研究采用AAVSO国际变星索引VSX目录检索蒭藁型变星，球状星团信息取自Harris 1976年发表的McMaster目录及Holger Baumgardt的表格；恒星的金属丰度、有效温度$T_{\rm eff}$、视差、颜色等特征数据，来自Gaia EDR3目录、Gaia DR3 VariSumarry、Gaia DR3目录、2MASS点源目录、AllWISE及ZTF目录。研究使用UPSILoN程序、色-色图或色-星等图，验证所获恒星确实为蒭藁型变星，并区分其为O型还是C型蒭藁变星。针对主要影响银核恒星的消光问题，研究采用IRSA DUST档案、OGLE-III数据，重新计算无消光的Wesenheit星等。最终获得银核中1608颗蒭藁型变星的数据，其中308颗位于15个球状星团内；银晕中获得1954颗蒭藁型变星的数据，其中4颗位于3个球状星团内。银核蒭藁型变星的金属丰度分布呈双峰形态，峰值分别为-0.4 dex和+0.5 dex；银晕蒭藁型变星仅呈现单峰分布，峰值为+0.5 dex。银核蒭藁型变星的平均周期比银晕的长30天，且银核中O型蒭藁变星的数量多于C型；在红外波段，蒭藁型变星周期的以10为底的对数与星等呈线性相关，若采用光学波段的滤光片，因蒭藁型变星周围存在尘埃，该相关性会发生反转。
英文摘要
This work aimed to study Miras in the bulge and halo of our galaxy, including those in globular clusters. The AAVSO International Variable Star Index VSX catalogue was used to retrieve Mira variable stars, while the information about globular clusters were taken from the Harris \citep{Harris1976}, McMaster catalogue \citep{33} and Holger Baumgardt \citep{34} table. Stellar characteristics such as metallicity, $T_{\rm eff}$, parallax and colors were obtained by Gaia EDR3 catalogue, Gaia DR3 VariSumarry, Gaia DR3 catalogue, 2MASS Point Source Catalogue, AllWISE, and ZTF catalogue. The UPSILoN program, color-color or color-magnitude diagrams were used to verify that our stars are indeed Miras-type variable stars and whether they are O or C type Miras. To deal with extinction, which affects stars mainly in the galactic bulge, we used IRSA DUST archive, OGLE-III and recalculation to the extiction-free Wesenheit magnitude. We obtained data for 1608 Miras in the bulge, of which 308 are located in 15 globular clusters. For the stars in the halo, we obtained data for 1954 Miras, of which 4 are located in 3 globular clusters. Miras in the bulge show a bimodal metallicity distribution with peaks at \text{--}0.4 dex and $+$0.5 dex, while Miras in the halo show only one peak at $+$0.5 dex. The period of Miras in the bulge is, on average, 30 days longer than for Miras in the halo, and O-type Miras are more abundant in the bulge than C-type Miras. The dependence of the logarithm of the base 10 period on magnitude in the infrared part of the spectrum gives us a linear dependence, with the dependence inverting when a filter is used in the optical part of the spectrum, because of the dust around the Miras.
