Maxted, PFL ORCID:, Miller, NJ, Hoyer, S, Adibekyan, V, Sousa, SG, Billot, N, Fortier, A, Simon, AE, Cameron, AC, Swayne, MI, Gutermann, P, Triaud, AHMJ, Southworth, J ORCID:, Alibert, Y, Alonso, R, Anglada, G, Bárczy, T, Navascues, DBY, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Benz, W, Bonfils, X, Brandeker, A, Broeg, C, Buder, M, Cabrera, J, Charnoz, S, van Damme, CC, Csizmadia, S, Davies, MB, Deleuil, M, Delrez, L, Demangeon, O, Demory, B-O, Ehrenreich, D, Erikson, A, Fossati, L, Fridlund, M, Gandolfi, D, Gillon, M, Güdel, M, Heng, K, Leon, JEHN, Isaak, KG, Kiss, LL, Laskar, J, Etangs, ALD, Lendl, M, Lovis, C, Magrin, D, Munari, M, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Santos, NC, Scandariato, G, Ségransan, D, Smith, AMS, Steinberger, M, Steller, M, Szabó, GM, Thomas, N, Udry, S, Van Grootel, V and Walton, N (2022) Fundamental effective temperature measurements for eclipsing binary stars – III. SPIRou near-infrared spectroscopy and CHEOPS photometry of the benchmark G0V star EBLM J0113+31. Monthly Notices of the Royal Astronomical Society.

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<jats:title>Abstract</jats:title> <jats:p>EBLM J0113+31 is moderately bright (V=10.1), metal-poor ([Fe/H] ≈−0.3) G0V star with a much fainter M dwarf companion on a wide, eccentric orbit (=14.3 d). We have used near-infrared spectroscopy obtained with the SPIRou spectrograph to measure the semi-amplitude of the M dwarf’s spectroscopic orbit, and high-precision photometry of the eclipse and transit from the CHEOPS and TESS space missions to measure the geometry of this binary system. From the combined analysis of these data together with previously published observations we obtain the following model-independent masses and radii: M1 = 1.029 ± 0.025M⊙, M2 = 0.197 ± 0.003M⊙, R1 = 1.417 ± 0.014R⊙, R2 = 0.215 ± 0.002R⊙. Using R1 and the parallax from Gaia EDR3 we find that this star’s angular diameter is θ = 0.0745 ± 0.0007 mas. The apparent bolometric flux of the G0V star corrected for both extinction and the contribution from the M dwarf (&amp;lt;0.2 per cent) is ${\mathcal {F}}_{\oplus ,0} = (2.62\pm 0.05)\times 10^{-9}$ erg cm−2 s−1. Hence, this G0V star has an effective temperature Teff, 1 = 6124 K ± 40 K (rnd.) ± 10 K (sys.). EBLM J0113+31 is an ideal benchmark star that can be used for “end-to-end” tests of the stellar parameters measured by large-scale spectroscopic surveys, or stellar parameters derived from asteroseismology with PLATO. The techniques developed here can be applied to many other eclipsing binaries in order to create a network of such benchmark stars.</jats:p>

Item Type: Article
Additional Information: © The Author(s) 2022. Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (, which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited. Accepted manuscripts are PDF versions of the author’s final manuscript, as accepted for publication by the journal but prior to copyediting or typesetting. They can be cited using the author(s), article title, journal title, year of online publication, and DOI. They will be replaced by the final typeset articles, which may therefore contain changes. The DOI will remain the same throughout.
Subjects: Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB600 Planets. Planetology
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 30 May 2022 14:51
Last Modified: 30 May 2022 14:51

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