Detailed spectroscopic analysis of the Trapezium cluster stars inside the Orion nebula

S. Simon-Diaz$^{1,2}, A. Herrero$^{1,3}$, C. Esteban$^{1,3}$, F. Najarro$^4$

1 -Instituto de Astrofisica de Canarias; 2 - Isaac Newton Group; 3 - Departamento de Astrofisica Universidad de La Laguna; 4 - Instituto de Estructura de la Materia, CSIC

We present the results of a spectroscopic analysis of the Trapezium cluster stars inside the Orion Nebula. The rotational velocities have been obtained using Fourier analysis method, finding agreement with values derived from the usual method, based on linewidth measurements. The rotational velocity derived for theta 1 Ori C through 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 H, HeI and HeII observed profiles with FASTWIND synthetic profiles, stellar parameters and wind characteristics have been derived. This methodology let us estimate the errors associated with these parameters. It is found that macroturbulence effects have to be included for a good fit to the HeI-II lines in the spectrum of theta 1 Ori C. By means of a very accurate study, oxygen abundances have been derived for the three B0.5V stars theta 1 Ori A, D and theta 2 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 and Lambert (1994). Our results suggest a lower dust depletion factor of oxygen than previous estimations for the Orion nebula.

Reference: Accepted for A&A
Status: Manuscript has been accepted

Weblink: astro-ph/0510288