The system will be going down for regular maintenance. Please save your work and logout.
Colour Excesses of 74 Supergiants and 30 Classical Cepheids
SOUBIRAN, C.
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
See more >
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
SOUBIRAN, C.
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
< Reduce
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
Language
en
Article de revue
This item was published in
Odessa Astronomical Publications. 2007, vol. 20, p. 91
AstroPrint
English Abstract
We derive accurate, homogeneous atmospheric parameters (Teff , log g, Vt, [Fe/H]) for 74 FGK non-variable supergiants and for 30 classical cepheids in 302 pulsation phases based on the highresolution, high signal-to-noise ...Read more >
We derive accurate, homogeneous atmospheric parameters (Teff , log g, Vt, [Fe/H]) for 74 FGK non-variable supergiants and for 30 classical cepheids in 302 pulsation phases based on the highresolution, high signal-to-noise echelle spectra. The extremely high precision of the effective temperature determination (10-30 K) is achieved by using the line-depth ratio method. These parameters are correlated with unreddened B-V colour index compiled from the literature for investigated stars to obtain an empirical relationship of the form (B-V )0 = 57.984 - 10.3587(logTeff )2 + +1.67572(logTeff )3 - 3.356logg + 0.0321Vt+ +0.2615[Fe/H] + 0.8833(logg)(logTeff) This expression have been used for the estimation of the colour excesses E(B-V) of individual supergiants and classical cepheids with an error 0.05 mag, which matches precision of the most sophisticated photometric techniques. The application range is F0-K0, luminosity classes I and II. Considering the large distances of supergiants, this method opens up a possibility for the large-scale extinction mapping of the Galaxy, with sensitivity down to 0.1-0.2 mag.Read less <
English Keywords
Stars: fundamental parameters
stars: colour excesses
stars: supergiants
stars: classical cepheids
stars: classical cepheids.
Origin
Hal imported