| Issue |
A&A
Volume 428, Number 2, December III 2004
|
|
|---|---|---|
| Page(s) | 587 - 593 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361:20041416 | |
| Published online | 26 November 2004 | |
Cepheid distances from infrared long-baseline interferometry *
III. Calibration of the surface brightness-color relations
1
LESIA, UMR 8109, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92195 Meudon Cedex, France e-mail: Pierre.Kervella@obspm.fr
2
European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago 19, Chile
3
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
4
GEMINI, UMR 6203, Observatoire de la Côte d'Azur, Avenue Copernic, 06130 Grasse, France
5
Observatoire Midi-Pyrénées, UMR 5572, 14, avenue Edouard Belin, 31400 Toulouse, France
Received:
4
June
2004
Accepted:
15
July
2004
The recent VINCI/VLTI observations presented in Paper I have nearly doubled
the total number of available angular diameter measurements of Cepheids.
Taking advantage of the significantly larger color range covered by these observations,
we derive in the present paper high precision calibrations of the surface brightness-color relations
using exclusively Cepheid observations. These empirical laws make it possible to determine
the distance to Cepheids through a Baade-Wesselink type technique. The least dispersed
relations are based on visible-infrared colors, for instance
.
The convergence of the Cepheid (this work) and dwarf star (Kervella et al. [CITE])
visible-infrared surface brightness-color relations is strikingly good.
The astrophysical dispersion of these relations appears to be very small, and below
the present detection sensitivity.
Key words: stars: variables: Cepheids / cosmology: distance scale / stars: oscillations / techniques: interferometric
© ESO, 2004
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