PARSEC V2.0: Stellar tracks and isochrones of low- and intermediate-mass stars with rotation

¹ SISSA, Via Bonomea 265, 34136 Trieste, Italy
e-mail: cnguyen@sissa.it
² Dipartimento di Fisica e Astronomia, Università degli studi di Padova, Vicolo Osservatorio 3, Padova, Italy
e-mail: guglielmo.costa@unipd.it
³ INAF Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio n. 5, Padova, Italy
⁴ INFN – Padova, Via Marzolo 8, 35131 Padova, Italy
⁵ Anhui University, Hefei 230601, PR China
⁶ National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, PR China
⁷ Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, PR China
⁸ The Kavli Institute for Astronomy and Astrophysics at Peking University, 100871 Beijing, PR China
⁹ INAF Osservatorio di Astrofisica e Fisica dello Spazio, Via Gobetti 93/3, 40129 Bologna, Italy
¹⁰ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA

Received: 1 June 2022
Accepted: 19 July 2022

Abstract

We present a new comprehensive collection of stellar evolutionary tracks and isochrones for rotating low- and intermediate-mass stars assembled with the updated version of PARSEC V2.0. This version includes our recent calibration of the extra mixing from overshooting and rotation, as well as several improvements regarding the nuclear reaction network, treatment of convective zones, mass loss, and other physical input parameters. The initial mass of the stellar models covers the range 0.09 M_⊙ to 14 M_⊙ for six sets of initial metallicity, from Z = 0.004 to Z = 0.017. Rotation is considered for stars above ∼1 M_⊙ with a smooth transition between non-rotating and extremely fast-rotating models, based on the initial mass. For stars more massive than ∼1.3 M_⊙, the full rotation range, from low to critical, is considered. We adopt the solar-scaled chemical mixtures with Z_⊙ = 0.01524. All the evolutionary phases from the pre-main-sequence to the first few thermal pulses on the asymptotic giant branch or central C exhaustion are considered. The corresponding theoretical isochrones are further derived with TRILEGAL code and are converted into several photometric systems, taking different inclination angles into account. Besides magnitudes, they also offer many other stellar observables in line with the data being provided by current large surveys. The new collection is fully integrated in a user-friendly web-interface for the benefit of easily performing stellar population studies.