Performance of the Stellar Abundances and atmospheric Parameters Pipeline adapted for M dwarfs

I. Atmospheric parameters from the spectroscopic module

¹ Observational Astrophysics, Department of Physics and Astronomy, Uppsala University, Box 516, 751 20 Uppsala, Sweden
² Max Planck Institute for Astronomy, 69117 Heidelberg, Germany
³ Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, IRAP/UMR 5277, 14 Avenue Edouard Belin, 31400, Toulouse, France
⁴ INAF – Osservatorio Astronomico d’Abruzzo, Via M. Maggini, s/n, 64100 Teramo, Italy; INFN, Sezione di Pisa, Largo Pontecorvo 3, 56127 Pisa, Italy
⁵ Yunnan Observatories, China Academy of Sciences, Kunming 650216, China; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China
⁶ Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Quartier Agora, Allée du 6 Août 19c, Bât. B5c, B4000 Liège, Belgium
⁷ Departamento de Física, Universidade Federal de Sergipe, Av. Marcelo Deda Chagas, S/N Cep 49.107-230, São Cristóvão, SE, Brazil
⁸ Centre for Planetary Habitability, Department of Geosciences, University of Oslo, Sem Sælands vei 2b, 0315 Oslo, Norway
⁹ Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
¹⁰ Instituto de Alta Investigación, Universidad de Tarapacá, Casilla 7D, Arica, Chile
¹¹ Instituto de Astrofísica e Ciências do Espaço (IA), CAUP, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
¹² Centro de Astrobiología (CAB), CSIC-INTA, Camino Bajo del Castillo s/n, 28692 Villanueva de la Cañada (Madrid), Spain
¹³ Center for Star and Planet Formation, Globe Institute, the University of Copenhagen, Øster Voldgade 5–7, 1350 København K, Denmark

^★ Corresponding authors; terese.olander@physics.uu.se; mgent@irap.omp.eu; ulrike.heiter@physics.uu.se

Received: 29 August 2024
Accepted: 10 February 2025

Abstract

Context. M dwarfs are important targets in the search for Earth-like exoplanets due to their small masses and low luminosities. Several ongoing and upcoming space missions are targeting M dwarfs for this reason, and the ESA PLATO mission is one of these.

Aims. In order to fully characterise a planetary system the properties of the host star must be known. For M dwarfs we can derive effective temperature, surface gravity, metallicity, and abundances of various elements from spectroscopic observations in combination with photometric data.

Methods. The Stellar Abundances and atmospheric Parameters Pipeline (SAPP) has been developed to serve as a prototype for one of the stellar science software within the PLATO consortium. The pipeline combines results from a spectroscopy, a photometry, an interferometry, and an asteroseismology module to derive stellar parameters for FGK-type stars. We have modified the pipeline to be able to analyse the M dwarf part of the PLATO target sample. The current version of the pipeline for M dwarfs mostly relies on spectroscopic observations. The module processing these data is based on the machine learning algorithm The Payne and fits a grid of model spectra to an observed spectrum to derive effective temperature and metallicity. We use spectra in the H-band, as the nearinfrared region is beneficial for M dwarfs because there are fewer molecular lines and they are brighter in this wavelength region than in the optical. A method based on synthetic spectra was developed for the continuum normalisation of the spectra, taking into account the pseudo-continuum formed by numerous lines of the water molecule. Photometry is used to constrain the surface gravity.

Results. We tested the modified SAPP on spectra of M dwarfs from the APOGEE survey. Our validation sample of 26 stars includes stars with interferometric observations and binaries. We found a good agreement between our derived values and reference values from a range of previous studies. We estimate the overall uncertainties in the derived effective temperature, surface gravity, and metallicity to be 100 K, 0.1 dex, and 0.15 dex, respectively.

Conclusions. We find that the modified SAPP performs well on M dwarfs and identify possible areas of future development that should lead to an improved precision of the derived stellar parameters.