Resolving the stellar components of the massive multiple system Herschel 36 with AMBER/VLTI

TL;DR

This study used long-baseline optical interferometry to resolve and characterize the components of the massive triple star system Herschel 36, providing new insights into its structure and orbital configuration.

Contribution

First application of long-baseline interferometry to image and measure the components of Herschel 36, enhancing understanding of massive star multiplicity.

Findings

Resolved the Aa+Ab components with approx. 2 mas resolution.

Located Ab at 1.81 mas from Aa with a position angle of 222 degrees.

Flux ratio between Aa and Ab is close to one.

Abstract

Context: Massive stars are extremely important for the evolution of the galaxies; there are large gaps in our understanding of their properties and formation, however, mainly because they evolve rapidly, are rare, and distant. It may well be that almost all massive stars are born as triples or higher multiples, but their large distances require very high angular resolution to directly detect the companions at milliarcsecond scales. Aims: Herschel36 is a young massive system located at 1.3 kpc. It has a combined smallest predicted mass of 45 M_sun. Multi-epoch spectroscopic data suggest the existence of at least three gravitationally bound components. Two of them, system Ab, are tightly bound in a spectroscopic binary, and the third one, component Aa, orbits in a wider orbit. Our aim was to image and obtain astrometric and photometric measurements of components Aa and Ab using, for the first time, long-baseline optical interferometry to further constrain its nature. Methods: We observed Herschel 36 with the near-infrared instrument AMBER attached to the ESO VLT Interferometer, which provides an angular resolution of approx. 2 mas. We used the code BSMEM to perform the interferometric image reconstruction. We fitted the interferometric observables using proprietary IDL routines and the code LitPro. Results: We imaged the Aa+Ab components of Herschel 36 in H and K filters. Component Ab is located at a projected distance of 1.81 mas, at a position angle of approx. 222 deg. east of north, the flux ratio between components Aa and Ab is close to one. The small measured angular separation indicates that system Ab and Ab may be approaching the periastron of their orbits. These results, only achievable with long-baseline near-infrared interferometry, constitute the first step toward a thorough understanding of this massive triple system.