{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,8,25]],"date-time":"2026-08-25T12:26:02Z","timestamp":1787660762915,"version":"build-2736575974"},"reference-count":62,"publisher":"Springer Science and Business Media LLC","issue":"1","license":[{"start":{"date-parts":[[2026,8,25]],"date-time":"2026-08-25T00:00:00Z","timestamp":1787616000000},"content-version":"tdm","delay-in-days":0,"URL":"https:\/\/creativecommons.org\/licenses\/by\/4.0"},{"start":{"date-parts":[[2026,8,25]],"date-time":"2026-08-25T00:00:00Z","timestamp":1787616000000},"content-version":"vor","delay-in-days":0,"URL":"https:\/\/creativecommons.org\/licenses\/by\/4.0"}],"funder":[{"name":"The\u00a0National Research Institute of Astronomy and Geophysics"}],"content-domain":{"domain":["link.springer.com"],"crossmark-restriction":false},"short-container-title":["Sci Rep"],"abstract":"<jats:title>Abstract<\/jats:title>\n                  <jats:p>\n                    As populations of stars born concurrently, open clusters serve as fundamental laboratories for validating models of star formation, stellar evolution, and the dynamical processes of the Galactic disk. This paper provides a comprehensive astrometric and photometric analysis of the open cluster AH03_J0748-26.9, leveraging data from the Gaia DR3 catalog. We employ the Hierarchical Density-Based Spatial Clustering of Applications with Noise (HDBSCAN) algorithm to analyze astrometric data from Gaia Data Release 3 (DR3). Our analysis characterizes the identified clusters through several fundamental parameters, specifically the census of probable members, spatial radii, age, distance, the initial mass function (IMF), and total cluster mass.We determined a concentration parameter of\n                    <jats:inline-formula>\n                      <jats:tex-math>$$c=0.396 \\pm 0.077$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    for AH03_J0748-26.9. The estimated number of members for AH03_J0748-26.9 is 128 stars. A distance modulus of\n                    <jats:inline-formula>\n                      <jats:tex-math>$$13.427 \\pm 0.093$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    mag and an age of 114.815 Myr (\n                    <jats:inline-formula>\n                      <jats:tex-math>$$\\log t=8.06 \\pm 0.020$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    ) were derived using PARSEC isochrone fitting. Given a relaxation time of 32.125\u00a0Myr and an age of 114.815\u00a0Myr (\n                    <jats:inline-formula>\n                      <jats:tex-math>$$\\tau = 3.57 &gt; 1$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    ), the cluster AH03_J0748-26.9 is found to be dynamically relaxed. We analyzed the mass function (MF) for AH03_J0748-26.9 using a Monte Carlo method coupled with synthetic cluster modeling. We characterized the MF over the range 0.102\u2013\n                    <jats:inline-formula>\n                      <jats:tex-math>$$5.088\\,M_\\odot $$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    by fitting a two-segment broken power law, deriving slopes of\n                    <jats:inline-formula>\n                      <jats:tex-math>$$\\alpha _A = -3.000 \\pm 0.605$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    (for\n                    <jats:inline-formula>\n                      <jats:tex-math>$$M &gt; 0.15\\,M_\\odot $$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    ) and\n                    <jats:inline-formula>\n                      <jats:tex-math>$$\\alpha _B = 1.596 \\pm 0.183$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    (for\n                    <jats:inline-formula>\n                      <jats:tex-math>$$M &lt; 0.15\\,M_\\odot $$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    ) with a characteristic break mass of\n                    <jats:inline-formula>\n                      <jats:tex-math>$$M_C = 0.150 \\pm 0.025\\,M_\\odot $$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    . The steep slope in the higher mass regime suggests a deviation from the canonical Salpeter IMF, which is consistent with the effects of dynamical evolution and mass segregation. By integrating this best-fit MF and adopting a binary fraction of\n                    <jats:inline-formula>\n                      <jats:tex-math>$$\\sim 0.70$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    \u2014typical for concentrated open clusters\u2014we estimate a total cluster mass of\n                    <jats:inline-formula>\n                      <jats:tex-math>$$290.603 \\pm 3.605\\,M_{\\odot }$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    . A sensitivity analysis indicates that varying the binary fraction between 0.5 and 0.9 alters the total mass estimate by approximately\n                    <jats:inline-formula>\n                      <jats:tex-math>$$\\pm 10\\%$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    , supporting the robustness of the mass scale. A sample of 128 member stars yielded a mean radial velocity of\n                    <jats:inline-formula>\n                      <jats:tex-math>$$69.745\\pm 9.615\\ \\text {km}\\ \\text {s}^{-1}$$<\/jats:tex-math>\n                    <\/jats:inline-formula>\n                    . These kinematic data, combined with proper motions, served as input for the galpy package to determine the cluster\u2019s Galactic orbit.\n                  <\/jats:p>","DOI":"10.1038\/s41598-026-67279-2","type":"journal-article","created":{"date-parts":[[2026,8,25]],"date-time":"2026-08-25T10:54:05Z","timestamp":1787655245000},"update-policy":"https:\/\/doi.org\/10.1007\/springer_crossmark_policy","source":"Crossref","is-referenced-by-count":0,"title":["Machine learning-enabled membership determination of open cluster AH03_J0748-26.9 using Gaia DR3 astrometry"],"prefix":"10.1038","volume":"16","author":[{"given":"W. A.","family":"Badawy","sequence":"first","affiliation":[],"role":[{"vocabulary":"crossref","role":"author"}]},{"given":"H. 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