CCD UBV and Gaia DR3 based analysis of NGC 189, NGC 1758 and NGC 7762 open clusters

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dc.authoridCakmak, Hikmet/0000-0002-1959-6049
dc.authoridBanks, Timothy/0000-0001-9445-4588
dc.authoridBilir, Selcuk/0000-0003-3510-1509
dc.contributor.authorYontan, Talar
dc.contributor.authorBilir, Selcuk
dc.contributor.authorCakmak, Hikmet
dc.contributor.authorRaul, Michel
dc.contributor.authorBanks, Timothy
dc.contributor.authorSoydugan, Esin
dc.contributor.authorCanbay, Remziye
dc.date.accessioned2025-01-27T21:00:00Z
dc.date.available2025-01-27T21:00:00Z
dc.date.issued2023
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThis paper presents photometric, astrometric, and kinematic analyses of the open clusters NGC 189, NGC 1758 and NGC 7762 based on CCD UBV photometric and Gaia Data Release 3 (DR3) data. According to membership analyses, we identified 32, 57 and 106 most probable member stars with membership probabilities P >= 0:5 in NGC 189, NGC 1758 and NGC 7762, respectively. The color excesses and photometric metallicities of each cluster were determined separately using UBV two-color diagrams. The color excess E(B - V) is 0: 590 +/- 0:023 mag for NGC 189, 0:310 +/- 0:022 mag for NGC 1758 and 0:640 +/- 0:017 mag for NGC 7762. The photometric metallicity [Fe/H] is -0:08 +/- 0:03 dex for both NGC 189 and NGC 1758, and -0:12 +/- 0:02 dex for NGC 7762. Distance moduli and ages of the clusters were obtained by comparing PARSEC isochrones with the color-magnitude diagrams constructed from UBV and Gaia photometric data. During this process, we kept as constant color excess and metallicity for each cluster. The estimated isochrone distance is 1201 +/- 53 pc for NGC 189, 902 +/- 33 pc for NGC 1758 and 911 +/- 31 pc for NGC 7762. These are compatible with the values obtained from trigonometric parallax. Ages of the clusters are 500 +/- 50 Myr, 650 +/- 50 Myr and 2000 +/- 200 Myr for NGC 189, NGC 1758 and NGC 7762, respectively. Galactic orbit integration of the clusters showed that NGC 1758 completely orbits outside the solar circle, while NGC 189 and NGC 7762 enter the solar circle during their orbits. (c) 2023 COSPAR. Published by Elsevier B.V. All rights reserved.
dc.description.sponsorshipScientific and Technological Research Council (TUBITAK) [122F109]
dc.description.sponsorshipThis study has been supported in part by the Scientific and Technological Research Council (TUB_ITAK) 122F109. The observations of this publication were made at the National Astronomical Observatory, San Pedro Martir, Baja California, Mexico, and the authors wish to thank the staff of the Observatory for their assistance during these observations. This research has made use of the WEBDA database, operated at the Department of Theoretical Physics and Astrophysics of the Masaryk University. We also made use of NASA's Astrophysics Data System as well as the VizieR and Simbad databases at CDS, Strasbourg, France and data from the European Space Agency (ESA) mission Gaia7, processed by the Gaia Data Processing and Analysis Consortium (DPAC)8. Funding for DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. IRAF was distributed by the National Optical Astronomy Observatory, which was operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. PyRAF is a product of the Space Telescope Science Institute, which is operated by AURA for NASA. We thank the University of Queensland for the collaboration software. We are grateful to the anonymous referees for their feedback, which improved the paper.
dc.identifier.doi10.1016/j.asr.2023.04.015
dc.identifier.endpage1473
dc.identifier.issn0273-1177
dc.identifier.issn1879-1948
dc.identifier.issue4
dc.identifier.scopus2-s2.0-85153583215
dc.identifier.scopusqualityQ1
dc.identifier.startpage1454
dc.identifier.urihttps://doi.org/10.1016/j.asr.2023.04.015
dc.identifier.urihttps://hdl.handle.net/20.500.12428/26910
dc.identifier.volume72
dc.identifier.wosWOS:001072679700001
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherElsevier Sci Ltd
dc.relation.ispartofAdvances in Space Research
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectGalaxy: open clusters and associations
dc.subjectIndividual: NGC 189
dc.subjectNGC 1758
dc.subjectNGC 7762
dc.subjectDatabase: Gaia Photometry: color-magnitude diagram
dc.subjectGalaxy kinematics
dc.subjectStellar kinematics
dc.titleCCD UBV and Gaia DR3 based analysis of NGC 189, NGC 1758 and NGC 7762 open clusters
dc.typeArticle

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