2017/08/16 by Daniel J. Stevens, Keivan G. Stassun, B. Scott Gaudi · 47 citations
Physics and Astronomy · #Angular diameter #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Bolometer #Effective temperature #Flux (metallurgy) #Galaxy #Luminosity #Physics #RADIUS #Stars #Stellar classification #Stellar, planetary, and galactic studies #Subgiant #astro-ph.SR
paper · pdf · doi:10.3847/1538-3881/aa957b
published in The Astronomical Journal 154(6), 259 (Institute of Physics) · Submitted to AAS Journals
arxiv created 2017/08/16 · openalex created_date 2017/08/31 · openalex publication_date 2017/11/29 · arxiv updated 2017/12/13 · openalex updated_date 2026/08/05
We present bolometric fluxes and angular diameters for over 1.6 million stars in the \it Tycho-2 catalog, determined using previously-determined empirical color-temperature and color-flux relations. We vet these relations via full fits to the full broadband spectral energy distributions for a subset of benchmark stars, and perform quality checks against the large set of stars for which spectroscopically-determined parameters are available from LAMOST, RAVE, and/or APOGEE. We then estimate radii for the 355,502 \it Tycho-2 stars in our sample whose Gaia DR1 parallaxes are precise to \lesssim10%. For the 64,960 of these stars with external spectroscopic information, we achieve median uncertainties on the effective temperatures, bolometric fluxes, angular diameters, and radii of 1.0%, 1.4%, 2.4%, and 7.5%, respectively. For the 290,542 remaining stars, we achieve median uncertainties of 0.9%, 1.3%, 2.2%, and 7.5%, respectively. These stellar parameters are shown to be reliable for stars with T\rm eff\lesssim7000~K. The over half a million bolometric fluxes and angular diameters presented here will serve as an immediate trove of empirical stellar radii with the \it Gaia\/ second data release, at which point effective temperature uncertainties will dominate the radius uncertainties. Already, dwarf, subgiant, and giant populations are readily identifiable in our purely empirical luminosity-effective temperature (theoretical) Hertzsprung-Russell diagrams.