Angular Diameters of Stars from the Mark III Optical Interferometer

By D. Mozurkewich, J. Armstrong, R. Hindsley, A. Quirrenbach, C. Hummel, Donald Hutter, K. Johnston, A. Hajian, N. Elias, D. Buscher and 1 more. 2003

159 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/cc10b0624c5d98f5c000ab3381156e1468e77879

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Citations in the corpus

FUNDAMENTAL PARAMETERS AND CHEMICAL COMPOSITION OF ARCTURUS (2011, background): “According to Mozurkewich et al. (2003), systematic uncertainties alone limit the precision of these measurements to no better than 1%, which is about 0.2mas for Arcturus.”
M dwarfs: effective temperatures, radii and metallicities (2008, methodology): “Davis & Tango (1986) obtained θ = 5.93 ± 0.08 (when updated limb-darkening coefficients are used, see Kervella et al. 2003), while Mozurkewich et al. (2003) found θ = 5.993 ± 0.108.”
Abundances In Very Metal-Poor Dwarf Stars (2004, methodology): “Mozurkewich et al. (2003) used the Mark III interferometer to determine limb-darkenening corrected radii for a sample of very bright nearby stars.”
SearchCal: a Virtual Observatory tool for searching calibrators in optical long-baseline interferometry II. The faint-object case (2006, methodology): “The (O-C) (difference between the measured and the computed angular diameters) are calculated for the stars of Ségransan et al. (2003) and Mozurkewich et al. (2003).”
Circumstellar material in the Vega inner system revealed by CHARA/FLUOR (2006, methodology): “Previous interferometric measurements obtained in the visible by Hanbury Brown et al. (1974) and Mozurkewich et al. (2003) were used to derive uniform disk (UD) diameters θUD = 3.08 ± 0.07 (λ = 440 nm) and θUD = 3.15 ± 0.03 (λ = 800 nm) respectively.”
VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance (2009, unknown): “For Vega (HD 172167) we found θUD−700 nm = 2.90 ± 0.03 mas and θUD−555 nm = 3.08 ± 0.03 mas, which matches well with the results determined by Mark III (Mozurkewich et al. 2003): θUD−800 nm = 3.149±0.31 and θUD−500 nm = 2.996±0.047.”
Accurate fundamental parameters for lower main‐sequence stars (2006, methodology): “This value implies and angular diameter of 3.272 mas for Vega, which compares very well with the interferometric angular diameter measurements of 3.24 ± 0.07 mas (Code et al. 1976), 3.28 ± 0.06 mas (Ciardi et al. 2001) and 3.225 ± 0.032 (Mozurkewich et al. 2003).”
A Planetary Companion to the Hyades Giant ϵ Tauri (2007, background): “Mozurkewich et al. (2003) measured an angular diameter of 2:671 0:032 mas for the star by interferometry, which yielded the stellar radiusR ¼ 13:7 0:6R combinedwith theHipparcos distance.”
SURVEYING THE BRIGHT STARS BY OPTICAL INTERFEROMETRY. I. A SEARCH FOR MULTIPLICITY AMONG STARS OF SPECTRAL TYPES F-K (2016, methodology): “The most discordant point in Figure 15 is a Mark III measurement for η Draconis (Mozurkewich et al. 2003).”
Effective temperature scale and bolometric corrections from 2MASS photometry (2006, background): “…approaches we find the remarkable work by Code et al. (1976), which is based on interferometric measurements of stellar angular semi-diameters (θ) and total fluxes (Fbol) at Earth, and the more recent works of Mozurkewich et al. (2003) and Kervella et al. (2004), also based on interferometry.”
Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “However, there are five other stars with angular diameter determinations at optical wavelengths by the same author (Mozurkewich et al. 2003) with good agreement with determinations in the infrared.”
First Results from the CHARA Array. VII. Long-Baseline Interferometric Measurements of Vega Consistent with a Pole-On, Rapidly Rotating Star (2006, methodology): “Specifically, uniform disk fits to data obtained in the first lobe of Vega’s visibility curve, from the Mark III interferometer (Mozurkewich et al. 2003) at 500 nm and 800 nm and from the Palomar Testbed Interferometer (PTI) (Ciardi et al. 2001) in the K-band, show the expected progression due to…”
Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer (2017, background): “…3.355±0.077 Hutter et al. (2016) 3.722±0.071 Mozurkewich et al. (2003) 3.34±0.07 Nordgren et al. (2001) 3.68±0.05 Nordgren et al. (2001) 148856 3.472±0.008 3.462±0.035 Mozurkewich et al. (2003) 3.53±0.08 Nordgren et al. (2001) 3.51±0.05 Nordgren et al. (2001) 150997 2.493±0.018…”