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V921 Scorpii is a close binary system (separation 0.025") showing theB[e]-phenomenon. The system is surrounded by an enigmatic bipolar nebula, whichmight have been shaped by episodic mass-loss events, possibly triggered bydynamical interactions between the companion and the circumprimary disk (Krauset al. 2012a). In this paper, we investigate the spatial structure andkinematics of the circumprimary disk, with the aim to obtain new insights intothe still strongly debated evolutionary stage. For this purpose, we combine,for the first time, infrared spectro-interferometry (VLTI/AMBER, R=12,000) andspectro-astrometry (VLT/CRIRES, R=100,000), which allows us to study theAU-scale distribution of circumstellar gas and dust with an unprecedentedvelocity resolution of 3 km*s^-1. Using a model-independent photocenteranalysis technique, we find that the Br-gamma-line emission rotates in the sameplane as the dust disk. We can reproduce the wavelength-differentialvisibilities and phases and the double-peaked line profile using aKeplerian-rotating disk model. The derived mass of the central star is5.4+/-0.4 M_sun*(d/1150 pc), which is considerably lower than expected from thespectral classification, suggesting that V921 Sco might be more distant (dapprox 2kpc) than commonly assumed. Using the geometric information provided byour Br-gamma spectro-interferometric data and Paschen, Brackett, and Pfund linedecrement measurements in 61 hydrogen recombination line transitions, we derivethe density of the line-emitting gas (N_e=2...6*10^19 m^-3). Given that ourmeasurements can be reproduced with a Keplerian velocity field withoutoutflowing velocity component and the non-detection of age-indicatingspectroscopic diagnostics, our study provides new evidence for thepre-main-sequence nature of V921 Sco.

On the nature of the Herbig B[e] star binary system V921 Scorpii: Geometry and kinematics of the circumprimary disk on sub-AU scales