Fundamental effective temperature measurements for eclipsing binary stars -- III. SPIRou near-infrared spectroscopy and CHEOPS photometry of the benchmark G0V star EBLM J0113+31

P. F. L. Maxted, N. J. Miller, S. Hoyer, V. Adibekyan, S. G. Sousa, N. Billot, A. Fortier, A. E. Simon, A. Collier Cameron, M. I. Sawyne, P. Gutermann, A. H. M. J. Triaud, J. Southworth, Y. Alibert, R. Alonso, G. Anglada, T. Bárczy, D. Barrado y Navascues, S. C. C. Barros, W. BaumjohannM. Beck, T. Beck, W. Benz, X. Bonfils, A. Brandeker, C. Broeg, M. Buder, J. Cabrera, S. Charnoz, C. Corral van Damme, Sz Csizmadia, M. B. Davies, M. Deleuil, L. Delrez, O. Demangeon, B. -O. Demory, D. Ehrenreich, A. Erikson, L. Fossati, M. Fridlund, D. Gandolfi, M. Gillon, M. Güdel, K. Heng, J. E. Hernández Leon, K. G. Isaak, L. L. Kiss, J. Laskar, A. Lecavelier des Etangs, M. Lendl, C. Lovis, D. Magrin, M. Munari, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, G. Peter, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, N. C. Santos, G. Scandariato, D. Ségransan, A. M. S. Smith, M. Steinberger, M. Steller, Gy M. Szabó, N. Thomas, S. Udry, V. Van Grootel, N. Walton

Research output: Contribution to journalArticlepeer-review

Abstract

EBLM J0113+31 is a 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 ± 0.025 M⊙, M2 = 0.197 ± 0.003 M⊙, R1 = 1.417 ± 0.014 R⊙, R2 = 0.215 ± 0.002 R⊙. 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 (<0.2 per cent) is F⊕,0=(2.62±0.05)×10−9 erg cm−2 s−1. Hence, this G0V star has an effective temperature Teff,1=6124K±40K(rnd.)±10K(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.
Original languageEnglish
Pages (from-to)6042–6057
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Volume513
Issue number4
Early online date16 May 2022
DOIs
Publication statusE-pub ahead of print - 16 May 2022

Bibliographical note

Accepted for publication in MNRAS. 15 pages, 9 figures

Keywords

  • techniques: spectroscopic
  • binaries; eclipsing
  • stars:solar type
  • stars: fundamental parameters

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