| Issue |
A&A
Volume 681, January 2024
|
|
|---|---|---|
| Article Number | A13 | |
| Number of page(s) | 18 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/202347618 | |
| Published online | 05 January 2024 | |
Age-dating the young open cluster UBC 1 with g-mode asteroseismology, gyrochronology, and isochrone fitting⋆
1
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
e-mail: dario.fritzewski@kuleuven.be
2
Department of Astrophysics, IMAPP, Radboud University Nijmegen, PO Box 9010 6500 GL Nijmegen, The Netherlands
3
Max Planck Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
4
Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, 2145 Sheridan Road, Evanston, IL 60208, USA
Received:
1
August
2023
Accepted:
20
October
2023
Aims. UBC 1 is an open cluster discovered in Gaia data and located near the edge of the Transiting Exoplanet Survey Satellite’s (TESS) continuous viewing zone. We aim to provide age constraints for this poorly studied open cluster from the combination of gravity-mode (g-mode) asteroseismology, gyrochronology, and isochrone fitting.
Methods. We established the members of UBC 1 from a spatial-kinematic filtering and estimate the cluster age and its parameters. Firstly, we fitted rotating isochrones to the single star cluster sequence. Secondly, using TESS time-series photometry, we explored the variability of the upper main sequence members and identified potential g-mode pulsators. For one star, we found a clear period spacing pattern that we used to deduce the buoyancy travel time, the near-core rotation rate, and an asteroseismic age. For a third independent age estimate, we employed the rotation periods of low-mass members of UBC 1.
Results. Based on isochrone fitting, we find log t = 8.1 ± 0.4, where the large uncertainty occurs because UBC 1 does not host evolved stars. From asteroseismology of one g-mode pulsator, we find a constrained age of log t = 8.24−0.14+0.43. From gyrochronology based on 17 cool star cluster members, we estimate log t = 8.35−0.25+0.16. Combined, all three methods lead to a consistent age in the range of 150 − 300 Myr.
Conclusions. Our results show that even a single cluster member with identified g modes can improve age-dating of young open clusters. Combining the gyrochronology of low-mass members with asteroseismology of intermediate-mass members is a powerful tool for young open cluster modelling, including high-precision age-dating.
Key words: asteroseismology / stars: variables: general / stars: rotation / open clusters and associations: individual: UBC 1 / techniques: photometric
Full Table 1 is available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/681/A13
© The Authors 2024
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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