Graczyk, D, Pietrzyński, G, Galan, C, Gieren, W, Tkachenko, A, Anderson, RI, Gallenne, A, Górski, M, Hajdu, G, Kałuszyński, M, Karczmarek, P, Kervella, P, Maxted, PFL ORCID: https://orcid.org/0000-0003-3794-1317, Nardetto, N, Narloch, W, Pavlovski, K, Pilecki, B, Pych, W, Southworth, J ORCID: https://orcid.org/0000-0002-3807-3198, Storm, J, Suchomska, K, Taormina, M, Villanova, S, Wielgórski, P, Zgirski, B and Konorski, P (2021) The surface brightness–colour relations based on eclipsing binary stars and calibrated with Gaia EDR3. Astronomy & Astrophysics, 649. A109 - A109.

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Abstract

<jats:p><jats:italic>Aims.</jats:italic> The surface brightness–colour relation (SBCR) is a basic tool for establishing precise and accurate distances within the Local Group. Detached eclipsing binary stars with accurately determined radii and trigonometric parallaxes allow calibration of the SBCRs with unprecedented accuracy.</jats:p> <jats:p><jats:italic>Methods.</jats:italic> We analysed four nearby eclipsing binary stars containing late F-type main sequence components: AL Ari, AL Dor, FM Leo, and BN Scl. We determined very precise spectroscopic orbits and combined them with high-precision ground- and space-based photometry. We derived the astrophysical parameters of their components with mean errors of 0.1% for mass and 0.4% for radius. We combined those four systems with another 24 nearby eclipsing binaries with accurately known radii from the literature for which <jats:italic>Gaia</jats:italic> EDR3 parallaxes are available in order to derive the SBCRs.</jats:p> <jats:p><jats:italic>Results.</jats:italic> The resulting SBCRs cover stellar spectral types from B9 V to G7 V. For calibrations, we used Johnson optical <jats:italic>B</jats:italic> and <jats:italic>V</jats:italic>, <jats:italic>Gaia</jats:italic> <jats:italic>G</jats:italic><jats:sub>BP</jats:sub> and <jats:italic>G</jats:italic>, and 2MASS <jats:italic>J</jats:italic><jats:italic>H</jats:italic><jats:italic>K</jats:italic> bands. The most precise relations are calibrated using the infrared <jats:italic>K</jats:italic> band and allow angular diameters of A-, F-, and G-type dwarf and subgiant stars to be predicted with a precision of 1%.</jats:p>

Item Type: Article
Additional Information: The final version of this article and all relevant information related to it, including copyrights, can be found online at; https://www.aanda.org/articles/aa/abs/2021/05/aa40571-21/aa40571-21.html
Subjects: Q Science > Q Science (General)
Q Science > QB Astronomy
Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB600 Planets. Planetology
Q Science > QB Astronomy > QB799 Stars
Q Science > QC Physics
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 04 Aug 2021 09:51
Last Modified: 04 Aug 2021 09:51
URI: https://eprints.keele.ac.uk/id/eprint/9846

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