Photoelectric photometry of stars in the Kapteyn Areas in the Vilnius system

Zdanavicius, K.; Clariá, J. J.; Piatti, A. E.; Straižys, V.

doi:10.1515/astro-1994-0303

Cited by 2 publications

(2 citation statements)

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“…Both narrow-and wide-band photometry in the 0.3 to 30 μm were used as available, including Johnson UBV (see e.g. Eggen (1963); Moreno (1971); Eggen (1972)), Stromgren ubvyβ (Piirola 1976), Two-Micron All-Sky Survey JHK s (Cutri et al 2003), Geneva (Rufener 1976), Vilnius UPXYZS (Zdanavicius et al 1972), WBVR (Kornilov et al 1991) and IRAS 12-μm flux (Neugebauer et al 1984); flux calibrations were based upon the values given in Cox (2000). Magnitudes at 12 μm were established from the IRAS flux values using the relationship found in Hickman, Sloan & Canterna (1995).…”

Section: Spectral Energy Distribution Fittingmentioning

confidence: 99%

Supergiant temperatures and linear radii from near-infrared interferometry

Belle

Creech‐Eakman

Hart

2009

Monthly Notices of the Royal Astronomical Society

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We present angular diameters for 42 Luminosity Class (LC) I stars and 32 LC II stars that have been interferometrically determined with the Palomar Testbed Interferometer. Derived values of radius and effective temperature are established for these objects, and an empirical calibration of these parameters for supergiants will be presented as a function of spectral type and colours. For the effective temperature versus (V−K)0 colour, we find an empirical calibration with a median deviation of ΔT= 70 K in the range of 0.7 < (V−K)0 < 5.1 for LC I stars; for LC II, the median deviation is ΔT= 120 K from 0.4 < (V−K)0 < 4.3. Effective temperature as a function of spectral type is also calibrated from these data, but shows significantly more scatter than the TEFF versus (V−K)0 relationship. No deviation of TEFF versus spectral type is seen for these high‐luminosity objects relative to LC II giants. Directly determined diameters range up to 400 R⊙, though are limited by poor distance determinations, which dominate the error estimates. These temperature and radii measures reflect a direct calibration of these parameters for supergiants from empirical means.

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Section: Spectral Energy Distribution Fittingmentioning

confidence: 99%

Supergiant temperatures and linear radii from near-infrared interferometry

Belle

Creech‐Eakman

Hart

2009

Monthly Notices of the Royal Astronomical Society

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“…Reddening corrections were based upon the empirical reddening determination described by Cardelli et al (1989), which differs little from van de Hulst's theoretical reddening curve number 15 (Johnson 1968;Dyck et al 1996). Both narrowband and wideband photometry in the 0.3 µm to 30 µm were used as available, including Johnson UBV (see, for example, Eggen (1963Eggen ( , 1972; Moreno (1971)), Strömgren ubvyβ (Piirola 1976), Geneva (Rufener 1976), 2Mass JHK s (Cutri et al 2003), and Vilnius UP XY ZS (Zdanavicius et al 1972); zero-magnitude flux density calibrations were based upon the values given in Cox (2000).…”

Section: Bolometric Flux Estimatesmentioning

confidence: 99%

Measurement of the Surface Gravity of η Bootis

Belle

Ciardi

Boden

2007

ApJ

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Direct angular size measurements of the G0IV subgiant η Boo from the Palomar Testbed Interferometer are presented, with limb-darkened angular size of θ LD = 2.1894 +0.0055 −0.0140 mas, which indicate a linear radius of R = 2.672 ± 0.028R ⊙ . A bolometric flux estimate of F BOL = 22.1 ± 0.28 × 10 −7 erg cm −2 s −1 is computed, which indicates an effective temperature of T EF F = 6100 ± 28 K and luminosity of L = 8.89 ± 0.16L ⊙ for this object. Similar data are established for a check star, HD 121860. The η Boo results are compared to, and confirm, similar parameters established by the MOST asteroseismology satellite. In conjunction with the mass estimate from the MOST investigation, a surface gravity of log g = 3.817 ± 0.016 [cm s −2 ] is established for η Boo.

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Photoelectric photometry of stars in the Kapteyn Areas in the Vilnius system

Cited by 2 publications

References 0 publications

Supergiant temperatures and linear radii from near-infrared interferometry

Supergiant temperatures and linear radii from near-infrared interferometry

Measurement of the Surface Gravity of η Bootis

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