The variable stars in the field of the bulge cluster NGC 6558

被引：2
作者：
Ferro, A. Arellano [1 ]
Guillen, L. J. Zerpa [2 ,3 ]
Yepez, M. A. [4 ,5 ]
Fierro, I. H. Bustos [6 ]
Prudil, Z. [7 ]
Parra, C. E. Perez [2 ,3 ]
机构：
[1] Univ Nacl Autonoma Mexico, Inst Astron, Ciudad De Mexico 04510, Mexico
[2] Univ Los Andes, Fac Ciencias, Dept Fis, Grp Astrofis Teor, Merida 5101, Venezuela
[3] Fdn Ctr Invest Astron Francisco, Dept Cient, J Duarte CIDA, Merida 5101, Venezuela
[4] Inst Nacl Astrofis Opt & Elect INAOE, Luis Enrique Erro 1, Tonantzintla 72840, Pue, Mexico
[5] Consejo Nacl Humanidades Ciencias & Tecnol, Av Insurgentes Sur 1582, Ciudad De Mexico 03940, Mexico
[6] Univ Nacl Cordoba, Observ Astron, RA-5000 Cordoba, Argentina
[7] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2024年 / 532卷 / 02期
关键词：
star: horizontal branch; stars: variables: RR Lyrae; stars: fundamental parameters; globular clusters: individual (NGC 6558); DIFFERENCE IMAGE-ANALYSIS; PHOTOMETRIC SCALE FACTOR; COLOR-MAGNITUDE DIAGRAM; RR-LYRAE VARIABLES; GLOBULAR-CLUSTERS; STELLAR EVOLUTION; OOSTERHOFF DICHOTOMY; HORIZONTAL-BRANCH; GAIA EDR3; METALLICITY;
D O I：
10.1093/mnras/stae1609
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We made a survey of the variable stars in a 13.2 x 13.2 arcmin(2) centred on the field of the Galactic bulge cluster NGC 6558. A total of 78 variables were found in the field of the cluster. Many of these variables are included in the catalogue of variable stars in Galactic globular clusters (Clement et al. 2001), OGLE or Gaia DR3 data releases. A membership analysis based on the proper motions of Gaia DR3 revealed that many of these variables do not belong to the cluster. We employed the data from the aforementioned surveys and our own data in the VI photometric system to estimate the periods, which along with the light-curves morphology and position in a deferentially dereddened colour-magnitude diagram (CMD), help classifying the variable types. Two new member variables were found; an eclipsing binary (V18) and a semiregular SR/L (V19). In the end, we conclude that only nine variables are likely cluster members. Member variables were used to discuss the mean metallicity and distance of the parental cluster and find the average values.
引用
收藏
页码：2159 / 2173
页数：15
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