2022
DOI: 10.3847/1538-3881/ac58a0
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A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939

Abstract: This study calculated astrophysical parameters, as well as kinematic and galactic orbital parameters, of the open clusters NGC 1664 and NGC 6939. The work is based on CCD ultraviolet, blue, and visual (UBV) and Gaia photometric and astrometric data from ground- and space-based observations. Considering Gaia Early Data Release 3 (EDR3) astrometric data, we determined membership probabilities of stars located in both of the clusters. We used two-color diagrams to determine the E(B − V) color excesses for NGC 166… Show more

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Cited by 9 publications
(5 citation statements)
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“…PYUPMASK is written in Python and has a general structure that follows the algorithm of UPMASK (Pera et al 2021). Both algorithms were previously used to calculate the membership probabilities of OCs by various researchers (see Koç et al 2022;Taşdemir & Yontan 2023;Yontan & Canbay 2023).…”
Section: Member Selection and Cmdsmentioning
confidence: 99%
“…PYUPMASK is written in Python and has a general structure that follows the algorithm of UPMASK (Pera et al 2021). Both algorithms were previously used to calculate the membership probabilities of OCs by various researchers (see Koç et al 2022;Taşdemir & Yontan 2023;Yontan & Canbay 2023).…”
Section: Member Selection and Cmdsmentioning
confidence: 99%
“…We utilized UPMASK (Unsupervised Photometric Membership Assignment in Stellar Clusters; [29]) method by using astrometric data of Gaia DR3 for membership analyses. This methodology previously used in many studies ( [6,17,[25][26][27]). UPMASK is the method of clustering algorithm and detects spatially populated groups and identifies membership probabilities of stars.…”
Section: Membership Analysesmentioning
confidence: 99%
“… Although there is a difference of about 450 pc between the calculated parallax distance (dϖ = 3077±322 pc) and isochrone distance (diso=2625±337 pc) results, the two distance values are compatible within the errors. For objects far from the 2 kpc, the zero-point problem and observational biasness cause the measured Gaia trigonometric parallaxes to be smaller ( [20]; [21]; [23]).…”
Section: Conclusion and Suggestionsmentioning
confidence: 99%