Resolving the B[e] star Hen 3-1191 at 10 μm with VLTI/MIDI

We report spatially resolved, spectrally dispersed N-band observations of the B[e] star Hen 3-1191 with the MIDI instrument of the Very Large Telescope Interferometer. The object is resolved with a 40 m baseline and has an equivalent uniform disc diameter ranging from 24 mas at 8 ${\mu{\rm m}}$ to 36 mas at 13 ${\mu{\rm m}}$. The MIDI spectrum and visibilities show a curvature which can arise from a weak silicate feature in which the object appears ≈ 15% larger than in the continuum, but this could result from a change in the object's geometry within the band.
We then model Hen's 3-1191 spectral energy distribution (.4-60 $\mu{\rm m}$) and N-band visibilities. Because of the unknown nature of the object, we use a wide variety of models for objects with IR excesses. We find the observations to be consistent with a disc featuring an unusually high mass accretion and a large central gap almost void of matter, an excretion disc, and a binary made of two IR sources. We are unable to find a circumstellar shell model consistent with the data.
We review the different hypotheses concerning the physical nature of the star and conclude that it is neither a Be supergiant nor a symbiotic star. However, we could not discriminate between the scenario of a young stellar object featuring an unusually strong FU Orionis-like outburst of mass accretion ($4{-}250\times10^{-4}~\ensuremath{M_\odot}/\ensuremath{{\rm yr}}$) and that of a protoplanetary nebula with an equatorial mass excretion rate $\ga$$4 \times 10^{-5}\,\ensuremath{M_\odot}/\ensuremath{{\rm yr}}$. In both cases, taking the additional presence of an envelope or wind into account would result in lower mass flows.