PARSEC V2.0: Rotating tracks and isochrones for seven additional metallicities in the range Z = 0.0001–0.03^⋆

¹ INAF Osservatorio Astronomico di Trieste, Via Giambattista Tiepolo, 11, Trieste, Italy
² University of Trieste, Piazzale Europa, 1, Trieste, Italy
³ SISSA, Via Bonomea 265, I-34136 Trieste, Italy
⁴ Dipartimento di Fisica e Astronomia, Università degli studi di Padova, Vicolo dell’Osservatorio 3, Padova, Italy
⁵ INAF - Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, Padova, Italy
⁶ Department of Physics and Astronomy, Uppsala University, Box 516 SE-75120 Uppsala, Sweden
⁷ Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, 226-Boulevards du Triomphe-B, 1050 Bruxelles, Belgium
⁸ Anhui University, Hefei 230601, China
⁹ Dipartimento di Fisica e Astronomia, Università di Bologna, Via Gobetti 93/2, I-40129 Bologna, Italy
¹⁰ INAF – Astrophysics and Space Science Observatory of Bologna, Via Gobetti 93/3, 40129 Bologna, Italy

^⋆⋆ Corresponding author: chi.nguyen@inaf.it

Received: 18 June 2025
Accepted: 1 August 2025

Abstract

PARSEC v2.0 rotating stellar tracks were previously presented for six metallicity values from subsolar to solar values, with initial rotation rates (ω_i, defined as the ratio of the angular velocity and its critical value) spanning from the non-rotating case to very near the critical velocity (i.e. ω_i = 0.99), and for initial masses covering the ∼0.7 M_⊙ to 14 M_⊙ interval. Furthermore, we provided the corresponding isochrones converted into several photometric systems for different inclination angles between the line-of-sight and the rotation axes, from 0° (pole-on) to 90° (equator-on). In this work, we expand this database with seven other metallicity sets, including five sets of low metallicity (Z = 0.0001 − 0.002) and two sets of super-solar values (up to Z = 0.03). We present the new stellar tracks, which comprise ∼3040 tracks in total (∼5500 including previous sets), along with the new corresponding rotating isochrones. We also introduce the possibility of creating isochrones by interpolation for values of rotating rates that were not available in the initial set of tracks. We compared a selection of our new models with rotating stellar tracks from the Geneva Stellar Evolution Code, and we assessed the quality of our new tracks by fitting the colour-magnitude diagram of the open cluster NGC 6067. We took advantage of the projected rotational velocity of member stars measured by Gaia to validate our results and examined the surface oxygen abundances in comparison with the observed data. All newly computed stellar tracks and isochrones can be retrieved via our dedicated web databases and interfaces.