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Issue A&A Volume 385, Number 3, April III 2002 Page(s) 986 - 994 Section Stellar atmospheres DOI 10.1051/0004-6361:20020186

A&A 385, 986-994 (2002)
DOI: 10.1051/0004-6361:20020186

FUSE observations towards the pole-on Be star HR 5223

Y. Frémat¹, J. Zorec², A.-M. Hubert¹, L. S. Cidale³, R. D. Rohrmann⁴, J.-M. Désert², R. Ferlet², ⁴ and A. Vidal-Madjar<sup>2

1</sup>  Observatoire de Paris, Section d'Astrophysique de Meudon, GEPI, FRE K 2459, 5 place Jules Janssen, 92195 Meudon Cedex, France
²  Institut d'Astrophysique de Paris, CNRS, 98bis boulevard Arago, 75014 Paris, France
³  Facultad de Ciencias Astronómicas y Geofisicas, Universidad Nacional de La Plata, Paseo del Bosque S/N, 1900 La Plata, Argentina
⁴  Observatorio Astronómico, Universidad Nacional de Córdoba, Laprida 854, 5000 Córdoba, Argentina

(Received 26 October, 2001 / Accepted 29 January 2002)

Abstract
New spectra have been obtained for the pole-on Be star HR 5223 (HD 120991) using the Far Ultraviolet Satellite Explorer (FUSE). We give a complete description of the far-UV spectral range (920 to 1180 Å). The spectra are affected by strong blends with interstellar lines and molecular bands that also significantly lower the energy distribution of the star. We produce a synthetic spectrum of the interstellar medium (ISM) to determine the column densities of several elements (H ₂, H I, N I, O I ...) seen towards HR 5223 and to disentangle the components due to the ISM, the photosphere and/or to the circumstellar envelope. The line identification list is available at the CDS. Using the obtained column densities, we determine the reddening of the star due to the ISM only and locate the star relative to the nearby IS clouds. The fit of the dereddened UV flux distribution with models that account for the gravitational darkening due to the stellar fast rotation allowed us to estimate the stellar fundamental parameters ( = 22 000 K; = 3.7) and its distance ( pc). The distance obtained, which has to be considered as the most accurate available at the moment, is in agreement with the characteristics of the ISM matter distribution that affects the observed spectrum of the star and with the detecting limits of the HIPPARCOS satellite.

Key words: stars: emission-line, Be -- stars: fundamental parameters -- stars: individual: HR 5223 -- stars: rotation -- ISM: abundances -- stars: distances

Offprint request: Y. Frémat, yves.fremat@obspm.fr

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