COLOUR EXCESSES OF 74 SUPERGIANTS AND 30 CLASSICAL CEPHEIDS
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 det...
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Odessa I. I. Mechnykov National University
2007-12-01
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doaj-5acddf79561c4c258d139831925402d12020-11-25T03:27:02ZengOdessa I. I. Mechnykov National UniversityOdessa Astronomical Publications1810-42152007-12-01201919410.18524/1810-4215.2007.20.8703887038COLOUR EXCESSES OF 74 SUPERGIANTS AND 30 CLASSICAL CEPHEIDSV. V. Kovtyukh0C. SoubiranS. I. BelikM. P. YasinskayaF. A. ChehonadskihV. MalyutoOdessa Astronomical Observatory, Odessa National University T.G. Shevchenko Park, Odessa 65014 UkraineWe 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.http://oap.onu.edu.ua/article/view/87038 |
collection |
DOAJ |
language |
English |
format |
Article |
sources |
DOAJ |
author |
V. V. Kovtyukh C. Soubiran S. I. Belik M. P. Yasinskaya F. A. Chehonadskih V. Malyuto |
spellingShingle |
V. V. Kovtyukh C. Soubiran S. I. Belik M. P. Yasinskaya F. A. Chehonadskih V. Malyuto COLOUR EXCESSES OF 74 SUPERGIANTS AND 30 CLASSICAL CEPHEIDS Odessa Astronomical Publications |
author_facet |
V. V. Kovtyukh C. Soubiran S. I. Belik M. P. Yasinskaya F. A. Chehonadskih V. Malyuto |
author_sort |
V. V. Kovtyukh |
title |
COLOUR EXCESSES OF 74 SUPERGIANTS AND 30 CLASSICAL CEPHEIDS |
title_short |
COLOUR EXCESSES OF 74 SUPERGIANTS AND 30 CLASSICAL CEPHEIDS |
title_full |
COLOUR EXCESSES OF 74 SUPERGIANTS AND 30 CLASSICAL CEPHEIDS |
title_fullStr |
COLOUR EXCESSES OF 74 SUPERGIANTS AND 30 CLASSICAL CEPHEIDS |
title_full_unstemmed |
COLOUR EXCESSES OF 74 SUPERGIANTS AND 30 CLASSICAL CEPHEIDS |
title_sort |
colour excesses of 74 supergiants and 30 classical cepheids |
publisher |
Odessa I. I. Mechnykov National University |
series |
Odessa Astronomical Publications |
issn |
1810-4215 |
publishDate |
2007-12-01 |
description |
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. |
url |
http://oap.onu.edu.ua/article/view/87038 |
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