Performance of the Stellar Abundances and atmospheric Parameters Pipeline adapted for M dwarfs I. Atmospheric parameters from the spectroscopic module - 2025
stars: fundamental parameters; stars: late-type; stars: low-mass; techniques: miscellaneous; Atmospheric parameters; Effective temperature; Metallicities; Spectra's; Stars: low mass; Stars:fundamental parameters; Stars:late type; Stellars; Surface gravity; Technique: miscellaneous; Astronomy and Astrophysics; Space and Planetary Science; astro-ph.SR; astro-ph.EP; astro-ph.IM
Abstract :
[en] 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 near-infrared 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.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Olander, Terese ; Observational Astrophysics, Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden
Gent, Matthew R.; Max Planck Institute for Astronomy, Heidelberg, Germany ; Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, IRAP/UMR 5277, Toulouse, France
Heiter, Ulrike ; Observational Astrophysics, Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden
Kochukhov, Oleg ; Observational Astrophysics, Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden
Bergemann, Maria ; Max Planck Institute for Astronomy, Heidelberg, Germany
Magg, Ekaterina; Max Planck Institute for Astronomy, Heidelberg, Germany
Kovalev, Mikhail ; Yunnan Observatories, China Academy of Sciences, Kunming, China ; Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, China
Morel, Thierry ; Université de Liège - ULiège > Département d'astrophysique, géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE)
Miller, Nicola J.; Observational Astrophysics, Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden
Souto, Diogo ; Departamento de Física, Universidade Federal de Sergipe, São Cristóvão, Brazil
Shan, Yutong ; Centre for Planetary Habitability, Department of Geosciences, University of Oslo, Oslo, Norway ; Institut für Astrophysik, Georg-August-Universität, Göttingen, Germany
Rojas-Ayala, Bárbara ; Instituto de Alta Investigación, Universidad de Tarapacá, Arica, Chile
Delgado-Mena, Elisa ; Instituto de Astrofísica e Ciências do Espaço (IA), CAUP, Universidade do Porto, Porto, Portugal ; Centro de Astrobiología (CAB), CSIC-INTA, Spain
Wang, Haiyang S. ; Center for Star and Planet Formation, Globe Institute, the University of Copenhagen, København K, Denmark
Swedish National Space Agency Vetenskapsrådet Lise Meitner grant European Research Council Royal Swedish Academy of Sciences Deutsche Forschungsgemeinschaft European Union - NextGenerationEU INAF theory grant Belgian Federal Science Policy Office Carlsberg Foundation Conselho Nacional de Desenvolvimento Científico e Tecnológico ANID
Funding text :
We thank Andrew Mann, Vera Passegger, and Denis Mourard for useful discussions. T.O., U.H., O.K., and N.J.M. acknowledge support from the Swedish National Space Agency (SNSA/Rymdstyrelsen). O.K. also acknowledges support by the Swedish Research Council (grant agreement no. 2019-03548) and the Royal Swedish Academy of Sciences. M.B. is supported through the Lise Meitner grant from the Max Planck Society. This project has received funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation programme (Grant agreement No. 949173). E.M. acknowledges support by the Collaborative Research centre SFB 881, Heidelberg University, of the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation). S.C. has been funded by the European Union \u2013 \u201CNextGenerationEU\u201D RRF M4C2 1.1 n: 2022HY2NSX. \u201CCHRONOS: adjusting the clock(s) to unveil the CHRONO-chemo-dynamical Structure of the Galaxy\u201D (PI: S. Cassisi), and by INAF Theory grant \u201CLasting\u201D (PI: S. Cassisi). T.M. acknowledges financial support from Belspo for contract PRODEX PLATO mission development. H.S.W. acknowledges support from the Carlsberg Foundation\u2019s Semper Ardens grant (\u2018FIRSTATMO\u2019; PI: A. Johansen). D.S. thanks the National Council for Scientific and Technological Development \u2013 CNPq. B.R.-A. acknowledges funding support from the ANID Basal project FB210003. E.D.M. acknowledges the support by the Ram\u00F3n y Cajal contract RyC2022-035854-I funded by the Spanish MICIU/AEI/10.13039/501100011033 and by ESF+. This research was partially supported by the project AI4Research at Uppsala University. Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High Performance Computing at the University of Utah. The SDSS website is www.sdss4.org. SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, Center for Astrophysics / Harvard & Smithsonian, the Chilean Participation Group, the French Participation Group, Instituto de Astrof\u00EDsica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut f\u00FCr Astrophysik Potsdam (AIP), Max-Planck-Institut f\u00FCr Astronomie (MPIA Heidelberg), Max-Planck-Institut f\u00FCr Astrophysik (MPA Garching), Max-Planck-Institut f\u00FCr Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observat\u00E1rio Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Aut\u00F3noma de M\u00E9xico, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
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