STELLAR DIAMETERS AND TEMPERATURES. III. MAIN-SEQUENCE A, F, G, AND K STARS: ADDITIONAL HIGH-PRECISION MEASUREMENTS AND EMPIRICAL RELATIONS

By T. Boyajian, K. von Braun, G. V. van Belle, C. Farrington, G. Schaefer, Jeremy Jones, Russel J. White, H. Mcalister, T. T. ten Brummelaar, S. Ridgway and 6 more. 2013

162 citations recorded by the source corpus.

Based on CHARA Array measurements, we present the angular diameters of 23 nearby, main-sequence stars, ranging from spectral types A7 to K0, 5 of which are exoplanet host stars. We derive linear radii, effective temperatures, and absolute luminosities of the stars using Hipparcos parallaxes and measured bolometric fluxes. The new data are combined with previously published values to create an Angular Diameter Anthology of measured angular diameters to main-sequence stars (luminosity classes V and IV). This compilation consists of 125 stars with diameter uncertainties of less than 5%, ranging in spectral types from A to M. The large quantity of empirical data is used to derive color–temperature relations to an assortment of color indices in the Johnson (BVRJIJJHK), Cousins (RCIC), Kron (RKIK), Sloan (griz), and WISE (W3W4) photometric systems. These relations have an average standard deviation of ∼3% and are valid for stars with spectral types A0–M4. To derive even more accurate relations for Sun-like stars, we also determined these temperature relations omitting early-type stars (Teff > 6750 K) that may have biased luminosity estimates because of rapid rotation; for this subset the dispersion is only ∼2.5%. We find effective temperatures in agreement within a couple of percent for the interferometrically characterized sample of main-sequence stars compared to those derived via the infrared flux method and spectroscopic analysis.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5d6da77a71855f305674ebbaaf6c5cbbb76018bc

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In Astronomy and Astrophysics

1. D. Huber
2. E. Gaidos
3. J. Johnson
4. E. Petigura
5. D. Charbonneau
6. A. Mann
7. Timothy Morton
8. W. Chaplin

In Instrumentation

1. D. Huber
2. E. Gaidos
3. E. Petigura
4. J. Johnson
5. A. Mann
6. Debra A. Fischer
7. D. Stello
8. W. Chaplin

Citations in the corpus

• THE K2 ECLIPTIC PLANE INPUT CATALOG (EPIC) AND STELLAR CLASSIFICATIONS OF 138,600 TARGETS IN CAMPAIGNS 1–8 (2015, background): “Specifically, radii for M dwarfs at fixed Teff are systematically smaller in Padova models, which disagrees with empirical measurements from long-baseline interferometry (Boyajian et al. 2012b, 2013) or low-mass eclipsing binary systems (Kraus et al. 2011; Carter et al. 2011).”
• The Sirius System and Its Astrophysical Puzzles: Hubble Space Telescope and Ground-based Astrometry (2017, background): “The radius of Sirius A is tightly constrained, as it is derived from precise interferometric measurements (e.g., Kervella et al. 2003; D11; Boyajian et al. 2013 and references therein).”
• The Habitability of Planets Orbiting M-dwarf Stars (2016, background): “As a spectral class, M dwarfs span a larger range in mass than the next three spectral classes (FGK) combined (Boyajian et al., 2012, 2013).”
• REVISED STELLAR PROPERTIES OF KEPLER TARGETS FOR THE QUARTER 1–16 TRANSIT DETECTION RUN (2013, background): “…of low-mass dwarfs with empirically measured radii, masses and effective temperatures from longbaseline interferometry (Boyajian et al. 2012, 2013) or low-mass eclipsing binary systems (Kraus et al. 2011; Carter et al. 2011) (although significant offsets still exist, see Boyajian et al. 2013).”
• Precision Stellar Characterization of FGKM Stars using an Empirical Spectral Library (2017, background): “…Teff , 0.05 4 The von Braun et al. (2014) compilation included results from Kervella et al. (2003), Baines et al. (2008), Baines et al. (2009), van Belle & von Braun (2009), von Braun et al. (2011a), von Braun et al. (2011b), von Braun et al. (2012), Boyajian et al. (2013), and Henry et al. (2013).”
• Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer (2017, background): “Interferometers have produced excellent survey results in the past, such as in van Belle et al. (1999), Nordgren et al. (1999), Mozurkewich et al. (2003), and Boyajian et al. (2013).”
• Habitable Moist Atmospheres on Terrestrial Planets near the Inner Edge of the Habitable Zone around M Dwarfs (2017, methodology): “For stars with >T 3200eff K, we use the empirically derived relationships between the mass, luminosity, and effective temperature of the host stars from Boyajian et al. (2013).”
• The Gaia–Kepler Stellar Properties Catalog. I. Homogeneous Fundamental Properties for 186,301 Kepler Stars (2020, methodology): “…Derived Effective Temperatures To ensure our grid-computed stellar effective temperatures are accurate, we compared them to interferometric Teff measurements for a sample of 108 stars from Boyajian et al. (2013) and Huang et al. (2015) with Tycho B and V photometry as well as 2MASS Ks photometry.”
• PLANETARY CANDIDATES FROM THE FIRST YEAR OF THE K2 MISSION (2015, methodology): “By default, we used the Boyajian et al. (2013) V −K relation.”
• Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “Boyajian et al. (2012b, 2013) also determined bolometric fluxes and effective temperatures for all of these stars.”
• SPECTRAL PROPERTIES OF COOL STARS: EXTENDED ABUNDANCE ANALYSIS OF 1,617 PLANET-SEARCH STARS (2016, methodology): “Teff from Angular Diameters Interferometrically derived effective temperatures rely on very few model dependencies and can be obtained using only the limb darkened angular diameter ΘLD and the bolometric flux FBOL (Boyajian et al. 2013).”
• Planet Hunters IX. KIC 8462852-where's the flux? (2015, unknown): “…(Teff = 6750 ± 140 K) is consistent with the photometric estimate of Teff = 6584+178−279 K from the revised Kepler Input Catalogue properties (Huber et al. 2014), as well as with Teff = 6780 K derived from the empirical (V − K) colour–temperature relation from Boyajian et al. (2013).”
• REVEALING A UNIVERSAL PLANET–METALLICITY CORRELATION FOR PLANETS OF DIFFERENT SIZES AROUND SOLAR-TYPE STARS (2013, methodology): “Finally, we checked all stars whose radii are measured with asteroseismic and interferometric methods (bottom panels in Figure 3, Boyajian et al. 2012, 2013; von Braun et al. 2014; Chaplin et al. 2014).”
• Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes (2016, methodology): “Numerous calibrations of Teff for stars in various color/mass/age ranges have been performed (see, e.g., Casagrande et al. 2008, 2010; Boyajian et al. 2012, 2013; Mann et al. 2015), and thus while there remain systematic uncertainties, in general these uncertainties are well characterized and they…”