Volume 448, Number 1, March II 2006
|Page(s)||351 - 366|
|Published online||17 February 2006|
Detailed spectroscopic analysis of the Trapezium cluster stars inside the Orion nebula
Rotational velocities, stellar parameters, and oxygen abundances
Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain e-mail: firstname.lastname@example.org
2 Isaac Newton Group of Telescopes, Apartado de Correos 321, 38700 Santa Cruz de la Palma, Tenerife, Spain
3 Departamento de Astrofísica, Universidad de La Laguna, Avda. Astrofísico Francisco Sánchez, s/n, 38071 La Laguna, Spain
4 Instituto de Estructura de la Materia, CSIC, C/ Serrano 121, 28006 Madrid, Spain
Accepted: 1 October 2005
We present the results of a spectroscopic analysis of the Trapezium cluster stars inside the Orion nebula. The rotational velocities were obtained using the Fourier analysis method, and we found agreement with values derived by the usual method based on linewidth measurements. The rotational velocity derived for Ori C by this method is consistent with the variability of some of its spectral features that have a period of 15.42 days. By means of the fit of , , and observed profiles with Fastwind synthetic profiles, stellar parameters and wind characteristics were derived. This methodology let us estimate the errors associated with these parameters, and we found that macroturbulence effects have to be included for a good fit to the lines in the spectrum of Ori C. By means of a very accurate study, oxygen abundances were derived for the three B0.5V stars Ori A, D, and Ori B. Final abundances are consistent with the nebular gas-phase results presented in Esteban et al. (2004) and are lower than those given by Cunha & Lambert (1994). Our results suggest a lower dust depletion factor of oxygen than previous estimations for the Orion nebula.
Key words: stars: abundances / stars: early-type / stars: fundamental parameters / ISM: abundances / ISM: H ii regions / ISM: individual objects: Orion nebula
© ESO, 2006
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