Imaging the spinning gas and dust in the disc around the supergiant A[e] star HD62623

TL;DR

This study used high-resolution interferometry to image and analyze the dust and gas in the circumstellar disc of the supergiant star HD 62623, revealing a Keplerian rotating disc likely influenced by a low-mass companion.

Contribution

First velocity-resolved infrared images of HD 62623's disc were reconstructed, providing detailed measurements of its structure and kinematics, challenging previous ejection mechanism assumptions.

Findings

Disentangled dust and gas emission in the circumstellar disc.

Measured the inner rim of the dusty disc at 6 mas.

Found the gaseous disc extension at 2 mas with Keplerian rotation.

Abstract

Context. To progress in the understanding of evolution of massive stars one needs to constrain the mass-loss and determine the phenomenon responsible for the ejection of matter an its reorganization in the circumstellar environment Aims. In order to test various mass-ejection processes, we probed the geometry and kinematics of the dust and gas surrounding the A[e] supergiant HD 62623. Methods. We used the combined high spectral and spatial resolution covered by the VLTI/AMBER instrument. Thanks to a new multiwavelength optical/IR interferometry imaging technique, we reconstructed the first velocity-resolved images with a milliarcsecond resolution in the infrared domain. Results. We managed to disentangle the dust and gas emission in the HD 62623 circumstellar disc.We measured the dusty disc inner inner rim, i.e. 6 mas, constrained the inclination angle and the position angle of the major-axis of the disc.We also measured the inner gaseous disc extension (2 mas) and probed its velocity field thanks to AMBER high spectral resolution. We find that the expansion velocity is negligible, and that Keplerian rotation is a favoured velocity field. Such a velocity field is unexpected if fast rotation of the central star alone is the main mechanism of matter ejection. Conclusions. As the star itself seems to rotate below its breakup-up velocity, rotation cannot explain the formation of the dense equatorial disc. Moreover, as the expansion velocity is negligible, radiatively driven wind is also not a suitable explanation to explain the disc formation. Consequently, the most probable hypothesis is that the accumulation of matter in the equatorial plane is due to the presence of the spectroscopic low mass companion.