Initial stellar diameter measurements with the Mark III interferometer

Shao, M.; Colavita, M. M.; Hines, Braden E.; Staelin, D. H.; Hutter, D. J.; Johnston, K. J.; Mozurkewich, D.; Simon, R. S.; Hershey, J. L.; Hughes, J. A.; Kaplan, G. H.

doi:10.1086/166248

Cited by 18 publications

(13 citation statements)

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“…More importantly, the data were taken using baselines in the range of 8-12 m. Our experience is that observing with more baselines, or at least a larger range of baselines, is necessary if we are to understand the systematics in the data. These comments are also true for the observations by Shao et al (1988b), where all four of the stars were reported to have systematically larger angular diameters than those we obtain in this work.…”

Section: Comparison With Other Observationssupporting

confidence: 79%

“…The Mark III Stellar Interferometer was a joint project of the Naval Research Laboratory, the US Naval Observatory, the Smithsonian Astrophysical Observatory, and MIT, and was located on Mount Wilson, near Pasadena, California (Shao et al 1988a). The Mark III was designed primarily for wide-angle astrometry and consisted initially of three 5 cm apertures used in pairs, with baseline lengths of 12 m. First stellar fringes with these astrometric elements were detected in 1986.…”

Section: Observationsmentioning

confidence: 99%

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Angular Diameters of Stars from the Mark III Optical Interferometer

Mozurkewich¹,

Armstrong²,

Hindsley³

et al. 2003

Astron J

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180

181

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Observations of 85 stars were obtained at wavelengths between 451 and 800 nm with the Mark III Stellar Interferometer on Mount Wilson, near Pasadena, California. Angular diameters were determined by fitting a uniform-disk model to the visibility amplitude versus projected baseline length. Half the angular diameters determined at 800 nm have formal errors smaller than 1%. Limb-darkened angular diameters, effective temperatures, and surface brightnesses were determined for these stars, and relationships between these parameters are presented. Scatter in these relationships is larger than would be expected from the measurement uncertainties. We argue that this scatter is not due to an underestimate of the angular diameter errors; whether it is due to photometric errors or is intrinsic to the relationship is unresolved. The agreement with other observations of the same stars at the same wavelengths is good; the width of the difference distribution is comparable to that estimated from the error bars, but the wings of the distribution are larger than Gaussian. Comparison with infrared measurements is more problematic; in disagreement with models, cooler stars appear systematically smaller in the near-infrared than expected, warmer stars larger.

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Section: Comparison With Other Observationssupporting

confidence: 79%

Section: Observationsmentioning

confidence: 99%

Angular Diameters of Stars from the Mark III Optical Interferometer

Mozurkewich¹,

Armstrong²,

Hindsley³

et al. 2003

Astron J

Self Cite

180

181

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“…Mass Age (2003) 7.95±0.09 Nordgren et al (2001) 7.97±0.11 Nordgren et al (2001) 8.035±0.08 Mozurkewich et al (1991) 9.26±0.15 Shao et al (1988) 7.90±0.31 di Benedetto & Rabbia (1987) (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 2.624±0.034 Mozurkewich et al (2003) 2.50±0.08 Nordgren et al (2001) 2.64±0.04 Nordgren et al (2001) 2.42±0.07 Nordgren et al (1999) 156283 5.519±0.011 5.275±0.067 Mozurkewich et al (2003) 5.26±0.06 Nordgren et al (2001) 5.27±0.07 Nordgren et al (2001) 5.20±0.03 Nordgren et al (1999) (2016) 2.12±0.02 Ligi et al (2012) 2.041±0.043 Baines et al (2010) 172167 3.280±0.016 2.930±0.007 Monnier et al (2012) 3.08±0.03 * Mourard et al (2009) 3.202±0.005 * Absil et al (2006) 3.329±0.006 Aufdenberg et al (2006) 3.225±0.032 Mozurkewich et al (2003) 3.28±0.01 Ciardi et al (2001) Mozurkewich et al (2003) 3.11±0.04 Nordgren et al (2001) 3.20±0.05 Nordgren et al (2001) 3.08±0.03 Nordgren et al (1999) Note- * No LD diameter was provided, therefore we list the UD diameter here. Figure 4 shows a graphical representation of this table.…”

Section: Targetmentioning

confidence: 99%

Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer

et al. 2017

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We present the fundamental properties of 87 stars based on angular diameter measurements from the Navy Precision Optical Interferometer, 36 of which have not been measured previously using interferometry. Our sample consists of 5 dwarfs, 3 subgiants, 69 giants, 3 bright giants, and 7 supergiants, and span a wide range of spectral classes from B to M. We combined our angular diameters with photometric and distance information from the literature to determine each star's physical radius, effective temperature, bolometric flux, luminosity, mass, and age.

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“…To complement this sample, we have searched the literature, and added to our list the measurements related to the stars of luminosity classes IV and V. Most of the visible and infrared interferometers are represented in our sample, with measurements from the NII (Narrabri Intensity Interferometer, Hanbury Brown et al 1967), the Mk III (Shao et al 1988), the PTI (Palomar Testbed Interferometer, Colavita et al 1999) and the NPOI (Navy Prototype Optical Interferometer, Armstrong et al 1998). Our findings originally included a few lunar occultation measurements, but they were rejected as they were related to variable or multiple stars, or their precision was not sufficient to give them any weight in the fitting process.…”

Section: Angular Diametersmentioning

confidence: 99%

The angular sizes of dwarf stars and subgiants

Kervella

Thévenin

Folco

et al. 2004

A&A

496

546

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Abstract. The availability of a number of new interferometric measurements of Main Sequence and subgiant stars makes it possible to calibrate the surface brightness relations of these stars using exclusively direct angular diameter measurements. These empirical laws make it possible to predict the limb darkened angular diameters θ LD of dwarfs and subgiants using their dereddened Johnson magnitudes, or their effective temperature. The smallest intrinsic dispersions of σ ≤ 1% in θ LD are obtained for the relations based on the K and L magnitudes, for instance logOur calibrations are valid between the spectral types A0 and M2 for dwarf stars (with a possible extension to later types when using the effective temperature), and between A0 and K0 for subgiants. Such relations are particularly useful for estimating the angular sizes of calibrators for long-baseline interferometry from readily available broadband photometry.

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Initial stellar diameter measurements with the Mark III interferometer

Cited by 18 publications

References 0 publications

Angular Diameters of Stars from the Mark III Optical Interferometer

Angular Diameters of Stars from the Mark III Optical Interferometer

Fundamental Parameters of 87 Stars from the Navy Precision Optical Interferometer

The angular sizes of dwarf stars and subgiants

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