The OGLE Collection of Variable Stars: Nearly 66,000 Mira Stars in the Milky Way

• Published in: The Astrophysical journal. Supplement series 2022-06, Vol.260 (2), p.46
• Main Authors: Iwanek, Patryk, Soszyński, Igor, Kozłowski, Szymon, Poleski, Radosław, Pietrukowicz, Paweł, Skowron, Jan, Wrona, Marcin, Mróz, Przemysław, Udalski, Andrzej, Szymański, Michał K., Skowron, Dorota M., Ulaczyk, Krzysztof, Gromadzki, Mariusz, Rybicki, Krzysztof, Ratajczak, Milena
• Format: Article
• Language: English
• Subjects: Algorithms; Astrographic catalogs; Asymptotic giant branch stars; Carbon stars; Celestial bodies; Galactic bulge; Galactic center; Galactic disk; Gravitational lenses; Inspection; Light curve; Long period variable stars; Machine learning; Milky Way; Milky Way disk; Milky Way Galaxy; Mira variable stars; Mira variables; Semiregular variable stars; Sky surveys; Time series analysis
• ISSN: 0067-0049; 1538-4365
• DOI: 10.3847/1538-4365/ac6676

We present a collection of 65,981 Mira-type variable stars found in the Optical Gravitational Lensing Experiment (OGLE) project database. Two-thirds of our sample (40,356 objects) are located in the Galactic bulge fields, whereas 25,625 stars are in the Galactic disk. The vast majority of the collection (47,532 objects) comprises new discoveries. We provide basic observational parameters of the Mira variables: equatorial coordinates, pulsation periods, I -band and V -band mean magnitudes, I -band brightness amplitudes, and identifications in other catalogs of variable stars. We also provide the I -band and V -band time-series photometry collected since 1997 during the OGLE-II, OGLE-III, and OGLE-IV phases. The classical selection process, i.e., being mostly based on the visual inspection of light curves by experienced astronomers, has led to the high purity of the catalog. As a result, this collection can be used as a training set for machine-learning classification algorithms. Using overlapping areas of adjacent OGLE fields, we estimate the completeness of the catalog to be about 96%. We compare and discuss the statistical features of Miras located in different regions of the Milky Way. We show examples of stars that change their type over time, from a semiregular variable to Mira and vice versa. This data set is perfectly suited to studying the three-dimensional structure of the Milky Way, and it may help to explain the puzzle of the X-shaped bulge.