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Constraining the thermally pulsing asymptotic giant branch phase with resolved stellar populations in the Small Magellanic Cloud

Giada PastorelliDipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, ItalyPaola MarigoDipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, ItalyL. GirardiOsservatorio Astronomico di Padova – INAF, Vicolo dell’Osservatorio 5, I-35122 Padova, ItalyYang ChenDipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, ItalyStefano RubeleDipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, ItalyMichele TrabucchiDipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, ItalyB. AringerDipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, ItalySara BladhDipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, ItalyA. BressanSISSA, via Bonomea 365, I-34136 Trieste, ItalyJ. MontalbánDipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, ItalyMartha L. BoyerJulianne J. DalcantonDepartment of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USAKjell ErikssonTheoretical Astrophysics, Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20 Uppsala, SwedenM. A. T. GroenewegenKoninklijke Sterrenwacht van België, Ringlaan 3, 1180 Brussel, BelgiumS. HöfnerTheoretical Astrophysics, Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20 Uppsala, SwedenT. LebzelterDepartment of Astrophysics, University of Vienna, Tuerkenschanzstrasse 17, A1180 Vienna, AustriaA. NanniDipartimento di Fisica e Astronomia Galileo Galilei, Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, ItalyPhilip RosenfieldEureka Scientific, Inc., 2452 Delmer Street, Oakland CA 94602, USAP. R. WoodResearch School of Astronomy and Astrophysics, Australian National University, Canberra, ACT2611, AustraliaMaria-Rosa L. CioniLeibniz-Institüt für Astrophysik Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany

2019en

ABI

Annotatsiya

The thermally pulsing asymptotic giant branch (TP-AGB) experienced by low- and intermediate-mass stars is one of the most uncertain phases of stellar evolution and the models need to be calibrated with the aid of observations. To this purpose, we couple high-quality observations of resolved stars in the Small Magellanic Cloud (SMC) with detailed stellar population synthesis simulations computed with the TRILEGAL code. The strength of our approach relies on the detailed spatially resolved star formation history of the SMC, derived from the deep near-infrared photometry of the VISTA survey of the Magellanic Clouds, as well as on the capability to quickly and accurately explore a wide variety of parameters and effects with the COLIBRI code for the TP-AGB evolution. Adopting a well-characterized set of observations - star counts and luminosity functions - we set up a calibration cycle along which we iteratively change a few key parameters of the TP-AGB models until we eventually reach a good fit to the observations. Our work leads to identify two best-fitting models that mainly differ in the efficiencies of the third dredge-up and mass-loss in TP-AGB stars with initial masses larger than about 3 M⊙. On the basis of these calibrated models, we provide a full characterization of the TP-AGB stellar population in the SMC in terms of stellar parameters (initial masses, C/O ratios, carbon excess, mass-loss rates). Extensive tables of isochrones including these improved models are publicly available.

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Identifikatorlar

DOI: 10.1093/mnras/stz725

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