On the nature of the Herbig B[e] star binary system V921 Scorpii: Discovery of a close companion and relation to the large-scale bipolar nebula

TL;DR

This study uses high-resolution interferometry to discover a close companion to the B[e] star V921 Scorpii, revealing a binary system with a circumstellar disk and bipolar nebula, shedding light on the B[e] phenomenon.

Contribution

First high-resolution imaging of V921 Sco revealing a close companion and its orbital motion, linking binary interaction to the B[e] star characteristics.

Findings

Discovered a close companion at 29 AU from the primary.

Measured an orbital period of approximately 35 years.

Detected episodic outflow activity with a 25-year cycle.

Abstract

Belonging to the group of B[e] stars, V921 Scorpii is associated with a strong infrared excess and permitted and forbidden line emission, indicating the presence of low- and high-density circumstellar gas and dust. Many aspects of V921 Sco and other B[e] stars still remain mysterious, including their evolutionary state and the physical conditions resulting in the class-defining characteristics. In this paper, we employ VLTI/AMBER spectro-interferometry in order to reconstruct high-resolution (lambda/2B=0.0013") model-independent interferometric images for three wavelength bands around 1.65, 2.0, and 2.3 micrometer. In our images, we discover a close (25.0+/-0.8 milliarcsecond, corresponding to 29+/-0.9 AU at 1.15 kpc) companion around V921 Sco. Between two epochs in 2008 and 2009, we measure orbital motion of 7 degrees, implying an orbital period of about 35 years (for a circular orbit). Around the primary star, we detect a disk-like structure with indications for a radial temperature gradient. The polar axis of this AU-scale disk is aligned with the arcminute-scale bipolar nebula in which V921 Sco is embedded. Using Magellan/IMACS imaging, we detect multi-layered arc-shaped sub-structure in the nebula, suggesting episodic outflow activity from the system with a period of about 25 years, roughly matching the estimated orbital period of the companion. Our study supports the hypothesis that the B[e] phenomenon is related to dynamical interaction in a close binary system.