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• W2050362735 endingPage "464" @default.
• W2050362735 startingPage "446" @default.
• W2050362735 abstract "The infrared flux method (IRFM) has been applied to a sample of 135 dwarf and 36 giant stars covering the following regions of the atmospheric parameter space: (1) the metal-rich ([Fe/H] ≳ 0) end (consisting mostly of planet-hosting stars), (2) the cool (Teff ≲ 5000 K) metal-poor (-1 ≲ [Fe/H] ≲ -3) dwarf region, and (3) the very metal-poor ([Fe/H] ≲ -2.5) end. These stars were especially selected to cover gaps in previous works on Teff versus color relations, particularly the IRFM Teff scale of A. Alonso and collaborators. Our IRFM implementation was largely based on the Alonso et al. study (absolute infrared flux calibration, bolometric flux calibration, etc.) with the aim of extending the ranges of applicability of their Teff versus color calibrations. In addition, in order to improve the internal accuracy of the IRFM Teff scale, we recomputed the temperatures of almost all stars from the Alonso et al. work using updated input data. The updated temperatures do not significantly differ from the original ones, with few exceptions, leaving the Teff scale of Alonso et al. mostly unchanged. Including the stars with updated temperatures, a large sample of 580 dwarf and 470 giant stars (in the field and in clusters), which cover the ranges 3600 K ≲ Teff ≲ 8000 K and -4.0 ≲ [Fe/H] ≲ +0.5, have Teff homogeneously determined with the IRFM. The mean uncertainty of the temperatures derived is 75 K for dwarfs and 60 K for giants, which is about 1.3% at solar temperature and 4500 K, respectively. It is shown that the IRFM temperatures are reliable in an absolute scale given the consistency of the angular diameters resulting from the IRFM with those measured by long baseline interferometry, lunar occultation, and transit observations. Using the measured angular diameters and bolometric fluxes, a comparison is made between IRFM and direct temperatures, which shows excellent agreement, with the mean difference being less than 10 K for giants and about 20 K for dwarf stars (the IRFM temperatures being larger in both cases). This result was obtained for giants in the ranges 3800 K < Teff < 5000 K and -0.7 < [Fe/H] < 0.2 and dwarfs in the ranges 4000 K < Teff < 6500 K and -0.55 < [Fe/H] < 0.25; thus, the zero point of the IRFM Teff scale is essentially the absolute one (that derived from angular diameters and bolometric fluxes) within these limits. The influence of the bolometric flux calibration adopted is explored and it is shown that its effect on the Teff scale, although systematic, is conservatively no larger than 50 K. Finally, a comparison with temperatures derived with other techniques is made. Agreement is found with the temperatures from Balmer line profile fitting and the surface brightness technique. The temperatures derived from the spectroscopic equilibrium of Fe I lines are differentially consistent with the IRFM, but a systematic difference of about 100 and 65 K (the IRFM temperatures being lower) is observed in the metal-rich dwarf and metal-poor giant Teff scales, respectively." @default.
• W2050362735 created "2016-06-24" @default.
• W2050362735 creator A5031353884 @default.
• W2050362735 creator A5054681294 @default.
• W2050362735 date "2005-06-10" @default.
• W2050362735 modified "2023-10-18" @default.
• W2050362735 title "The Effective Temperature Scale of FGK Stars. I. Determination of Temperatures and Angular Diameters with the Infrared Flux Method" @default.
• W2050362735 cites W1488678412 @default.
• W2050362735 cites W1524699564 @default.
• W2050362735 cites W1843615779 @default.
• W2050362735 cites W1964031925 @default.
• W2050362735 cites W1964118876 @default.
• W2050362735 cites W1968817327 @default.
• W2050362735 cites W1972419586 @default.
• W2050362735 cites W1978636874 @default.
• W2050362735 cites W1979257798 @default.
• W2050362735 cites W1980118658 @default.
• W2050362735 cites W1986270837 @default.
• W2050362735 cites W2001417160 @default.
• W2050362735 cites W2002876153 @default.
• W2050362735 cites W2012853668 @default.
• W2050362735 cites W2015590058 @default.
• W2050362735 cites W2016734711 @default.
• W2050362735 cites W2018654274 @default.
• W2050362735 cites W2019850909 @default.
• W2050362735 cites W2024353730 @default.
• W2050362735 cites W2025123617 @default.
• W2050362735 cites W2027965892 @default.
• W2050362735 cites W2035819620 @default.
• W2050362735 cites W2036211428 @default.
• W2050362735 cites W2036245243 @default.
• W2050362735 cites W2047228913 @default.
• W2050362735 cites W2053487809 @default.
• W2050362735 cites W2056932217 @default.
• W2050362735 cites W2057869491 @default.
• W2050362735 cites W2063906968 @default.
• W2050362735 cites W2064045241 @default.
• W2050362735 cites W2064076500 @default.
• W2050362735 cites W2064913823 @default.
• W2050362735 cites W2069105369 @default.
• W2050362735 cites W2069697128 @default.
• W2050362735 cites W2071615312 @default.
• W2050362735 cites W2073332494 @default.
• W2050362735 cites W2073891539 @default.
• W2050362735 cites W2077329592 @default.
• W2050362735 cites W2078930188 @default.
• W2050362735 cites W2082325318 @default.
• W2050362735 cites W2083164825 @default.
• W2050362735 cites W2096499801 @default.
• W2050362735 cites W2097597961 @default.
• W2050362735 cites W2098846125 @default.
• W2050362735 cites W2110253451 @default.
• W2050362735 cites W2111817932 @default.
• W2050362735 cites W2119855645 @default.
• W2050362735 cites W2122068167 @default.
• W2050362735 cites W2122502856 @default.
• W2050362735 cites W2128490266 @default.
• W2050362735 cites W2131757010 @default.
• W2050362735 cites W2133076698 @default.
• W2050362735 cites W2186043533 @default.
• W2050362735 cites W3098641407 @default.
• W2050362735 cites W3099154566 @default.
• W2050362735 cites W3099819036 @default.
• W2050362735 cites W3099865027 @default.
• W2050362735 cites W3100331031 @default.
• W2050362735 cites W3101266941 @default.
• W2050362735 cites W3101413529 @default.
• W2050362735 cites W3104948151 @default.
• W2050362735 cites W3105777284 @default.
• W2050362735 cites W3122924837 @default.
• W2050362735 cites W3125406988 @default.
• W2050362735 cites W4244945807 @default.
• W2050362735 cites W4289788995 @default.
• W2050362735 cites W4292310310 @default.
• W2050362735 cites W4292508310 @default.
• W2050362735 doi "https://doi.org/10.1086/430101" @default.
• W2050362735 hasPublicationYear "2005" @default.
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