A detailed analysis of the Czernik 38 cluster and its associated tidal tail, utilizing Gaia DR3 and 2MASS

A detailed analysis of the Czernik 38 cluster and its associated tidal tail, utilizing Gaia DR3 and 2MASS | Research Square window.SnipcartSettings = { analytics: { enabled: false } }; (function() { var accessVector = localStorage.getItem('access_vector') || ''; window.dataLayer = window.dataLayer || []; if (accessVector) { window.dataLayer.push({ user: { profile: { profileInfo: { snid: accessVector } } } }); } })(); (function(w,d,s,l,i){w[l]=w[l]||[];w[l].push({'gtm.start':new Date().getTime(),event:'gtm.js'});var f=d.getElementsByTagName(s)[0],j=d.createElement(s),dl=l!='dataLayer'?'&l='+l:'';j.async=true;j.src='https://www.googletagmanager.com/gtm.js?id='+i+dl;f.parentNode.insertBefore(j,f);})(window,document,'script','dataLayer','GTM-K279D39R'); Browse Preprints In Review Journals COVID-19 Preprints AJE Video Bytes Research Tools Research Promotion AJE Professional Editing AJE Rubriq About Preprint Platform In Review Editorial Policies Our Team Advisory Board Help Center Sign In Submit a Preprint Cite Share Download PDF Article A detailed analysis of the Czernik 38 cluster and its associated tidal tail, utilizing Gaia DR3 and 2MASS Nasser M. Ahmed This is a preprint; it has not been peer reviewed by a journal. https://doi.org/ 10.21203/rs.3.rs-7600993/v1 This work is licensed under a CC BY 4.0 License Status: Published Journal Publication published 12 Feb, 2026 Read the published version in Scientific Reports → Version 1 posted 10 You are reading this latest preprint version Abstract This study provides a thorough investigation of the open cluster Czernik 38, employing photometric and astrometric data from Gaia DR3 and 2MASS. Our analysis refines the fundamental parameters of the cluster, including its structure, kinematics, evolutionary status, age, and morphology. To evaluate membership, we utilized the pyUPMASK Python package in conjunction with the HDBSCAN algorithm. The main focus of this research is our novel method of assigning a membership probability at each radius, instead of using a singular value for the entire cluster. A primary conclusion from our research is the existence of a leading tidal tail within the cluster radius; however, it does not show a S-shaped arrangement (which would consist of a leading and a trailing tail). Furthermore, we have discovered a new star cluster located 32 arcminutes from the center of Czerink. This cluster may serve as a companion to the Czernik 38 cluster in a binary cluster system or a complex colliding system; we will explore this further in subsequent research. According to Gaia, the distance modulus of the cluster and the color excess E(G BP − G RP) are measured at 12.69± 0.08 mag and 2.40 ± 0.04 mas, respectively. Additionally, from 2Mass, the distance modulus is 12.87 ± 0.93 mag, while the color excess E(J − K s) is 0.89 ± 0.2 mag. Moreover, the cluster age is determined to be 115.0± 20.3 Myr. The components of proper motion (µ α cos δ , µ δ) and the parallax (ϖ) were found as-2.41 ± 0.328 mas yr −1 ,-5.263 ± 1.063 mas yr −1 , and 0.21 ± 0.083 mas, respectively. The calculated mean Gaia distances are roughly 3580.4 ± 230.5 pc, which is in agreement with the photometric data from the Gaia and 2Mass data, within the error. There are 37 stars that exhibit radial velocity with average 46.1 ± 8.54 km/s, which allows us to derive orbital parameters, using the galpy python package. As a result, the cluster is moving parallel to the Galactic plane towards the Galactic center. Physical sciences/Astronomy and planetary science Physical sciences/Mathematics and computing Physical sciences/Optics and photonics Physical sciences/Physics Full Text Additional Declarations No competing interests reported. Cite Share Download PDF Status: Published Journal Publication published 12 Feb, 2026 Read the published version in Scientific Reports → Version 1 posted Editorial decision: Revision requested 23 Oct, 2025 Reviews received at journal 19 Oct, 2025 Reviews received at journal 18 Oct, 2025 Reviewers agreed at journal 29 Sep, 2025 Reviewers agreed at journal 28 Sep, 2025 Reviewers invited by journal 27 Sep, 2025 Editor invited by journal 22 Sep, 2025 Editor assigned by journal 17 Sep, 2025 Submission checks completed at journal 14 Sep, 2025 First submitted to journal 12 Sep, 2025 You are reading this latest preprint version Research Square lets you share your work early, gain feedback from the community, and start making changes to your manuscript prior to peer review in a journal. As a division of Research Square Company, we’re committed to making research communication faster, fairer, and more useful. We do this by developing innovative software and high quality services for the global research community. Our growing team is made up of researchers and industry professionals working together to solve the most critical problems facing scientific publishing. Also discoverable on Platform About Our Team In Review Editorial Policies Advisory Board Help Center Resources Author Services Accessibility API Access RSS feed Manage Cookie Preferences © Research Square 2026 | ISSN 2693-5015 (online) Privacy Policy Terms of Service Do Not Sell My Personal Information {"props":{"pageProps":{"initialData":{"identity":"rs-7600993","acceptedTermsAndConditions":true,"allowDirectSubmit":false,"archivedVersions":[],"articleType":"Article","associatedPublications":[],"authors":[{"id":526229898,"identity":"33c556ce-088b-4414-bee7-cf1520406cc3","order_by":0,"name":"Nasser M. 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Our analysis refines the fundamental parameters of the cluster, including its structure, kinematics, evolutionary status, age, and morphology. To evaluate membership, we utilized the pyUPMASK Python package in conjunction with the HDBSCAN algorithm. The main focus of this research is our novel method of assigning a membership probability at each radius, instead of using a singular value for the entire cluster. A primary conclusion from our research is the existence of a leading tidal tail within the cluster radius; however, it does not show a S-shaped arrangement (which would consist of a leading and a trailing tail). Furthermore, we have discovered a new star cluster located 32 arcminutes from the center of Czerink. This cluster may serve as a companion to the Czernik 38 cluster in a binary cluster system or a complex colliding system; we will explore this further in subsequent research. According to Gaia, the distance modulus of the cluster and the color excess E(G BP − G RP) are measured at 12.69± 0.08 mag and 2.40 ± 0.04 mas, respectively. Additionally, from 2Mass, the distance modulus is 12.87 ± 0.93 mag, while the color excess E(J − K s) is 0.89 ± 0.2 mag. Moreover, the cluster age is determined to be 115.0± 20.3 Myr. The components of proper motion (µ α cos δ , µ δ) and the parallax (ϖ) were found as-2.41 ± 0.328 mas yr −1 ,-5.263 ± 1.063 mas yr −1 , and 0.21 ± 0.083 mas, respectively. The calculated mean Gaia distances are roughly 3580.4 ± 230.5 pc, which is in agreement with the photometric data from the Gaia and 2Mass data, within the error. There are 37 stars that exhibit radial velocity with average 46.1 ± 8.54 km/s, which allows us to derive orbital parameters, using the galpy python package. 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