The EBLM project X. Benchmark masses, radii and temperatures for two fully convective M-dwarfs using K2

• Published in: arXiv.org
• Main Authors: Duck, Alison, Martin, David V, Gill, Sam, Armitage, Tayt, Romy Rodríguez Martínez, Maxted, Pierre F L, Sebastian, Daniel, Sethi, Ritika, Swayne, Matthew I, Andrew Collier Cameron, Dransfield, Georgina, Gaudi, B Scott, Gillon, Michael, Hellier, Coel, Kunovac, Vedad, Lovis, Christophe, McCormac, James, Pepe, Francesco A, Pollacco, Don, Sairam, Lalitha, Santerne, Alexandre, Ségransan, Damien, Standing, Matthew R, Southworth, John, Amaury H M J Triaud, Udry, Stephane
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 11.01.2024
• Subjects: Benchmarks; Binary stars; Extrasolar planets; Mathematical models; Parameters; Physics - Earth and Planetary Astrophysics; Physics - Solar and Stellar Astrophysics; Planet detection; Red dwarf stars; Spectrum analysis; Uncertainty
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2208.10534

M-dwarfs are the most abundant stars in the galaxy and popular targets for exoplanet searches. However, their intrinsic faintness and complex spectra inhibit precise characterisation. We only know of dozens of M-dwarfs with fundamental parameters of mass, radius and effective temperature characterised to better than a few per cent. Eclipsing binaries remain the most robust means of stellar characterisation. Here we present two targets from the Eclipsing Binary Low Mass (EBLM) survey that were observed with K2: EBLM J0055-00 and EBLM J2217-04. Combined with HARPS and CORALIE spectroscopy, we measure M-dwarf masses with precisions better than 5%, radii better than 3% and effective temperatures on order 1%. However, our fits require invoking a model to derive parameters for the primary star. By investigating three popular models, we determine that the model uncertainty is of similar magnitude to the statistical uncertainty in the model fits. Therefore, whilst these can be considered benchmark M-dwarfs, we caution the community to consider model uncertainty when pushing the limits of precise stellar characterisation.