SIMBAD references

We investigated the surroundings of MWC 314 in the framework of the study of hot emission line star environments using the SAC method. This star is either a B[e] supergiant or a luminous blue variable and appears to be extremely luminous and massive. We determine the structure and physical conditions of the emitting region and study the possible variations. We measured the absorption and emission line radial velocities and the emission line fluxes on high-resolution spectra obtained with Aurelie at the 1.52m OHP telescope in July 1998, with Elodie at the 1.93m OHP telescope at various epochs, and with echelle spectrographs of the Asiago and Loiano observatories (Italy) in 2006. We used the statistical approach of the self-absorption curve method (SAC) to derive physical parameters of the line-emitting region. We detected drastic variations of the photospheric absorption line radial velocities with time, while the emission line velocities appear to be stable. The CrII, TiII, and FeII emission lines have a complex structure. They are double-peaked, and each of these two 60km/s separated components, is composed of a narrow and a broad component, while the [FeII] line components are narrower. The fit of the various components of the FeII lines to a SAC curve indicates that their intensities are affected by some self absorption. We obtained a Boltzmann-type population law whose mean excitation temperature is 6500_–1000⁺¹⁵⁰⁰K for the narrow component lower and upper levels. We obtained a higher Boltzmann-type population law of 10500_–2000⁺³⁰⁰⁰K for the forbidden transition upper levels. From the absorption lines we confirm the binarity for MWC 314. The periodicity has nevertheless to be improved with a higher sampling frequency. Our results from the emission lines are consistent with line formation in a rotating disk around a star. The typical minimum radius of the line emitting region obtained from the SAC study is 3.5x10¹³cm (2.0x10¹³cm<R<6.3x10¹³cm). We argue, in the framework of a very simplified geometrical model, that the [FeII] lines are emitted farther out than the permitted Cr II, Ti II, and FeII lines, in a disk inclined 25±5 degrees to the plane of sky. If the rotation of the disk is Keplerian, the FeII lines are emitted in a zone defined by 4x10¹²cm<R<7x10¹³cm, while for a rotation with conservation of angular momentum, they are emitted from 4x10¹²cm<R<2x10¹³cm.