Tracing the young massive high-eccentricity binary system Theta 1 Orionis C through periastron passage

TL;DR

This study uses advanced interferometry techniques to precisely measure the orbit of the young, high-eccentricity binary star Theta 1 Orionis C, providing new insights into its fundamental parameters and the Orion Nebula Cluster.

Contribution

It presents the first VLTI/AMBER aperture synthesis image of Theta 1 Orionis C and introduces a new algorithm for extracting astrometric data from interferometric observations.

Findings

The binary has a short orbital period of 11.3 years and high eccentricity of 0.6.

The system's total mass is estimated at 44±7 solar masses.

The dynamical distance to the system is 410±20 parsecs, aligning with radio parallax measurements.

Abstract

The nearby high-mass star binary system Theta 1 Orionis C is the brightest and most massive of the Trapezium OB stars at the core of the Orion Nebula Cluster, and it represents a perfect laboratory to determine the fundamental parameters of young hot stars and to constrain the distance of the Orion Trapezium Cluster. Between January 2007 and March 2008, we observed T1OriC with VLTI/AMBER near-infrared (H- and K-band) long-baseline interferometry, as well as with bispectrum speckle interferometry with the ESO 3.6m and the BTA 6m telescopes (B'- and V'-band). Combining AMBER data taken with three different 3-telescope array configurations, we reconstructed the first VLTI/AMBER closure-phase aperture synthesis image, showing the T1OriC system with a resolution of approx. 2 mas. To extract the astrometric data from our spectrally dispersed AMBER data, we employed a new algorithm, which fits the wavelength-differential visibility and closure phase modulations along the H- and K-band and is insensitive to calibration errors induced, for instance, by changing atmospheric conditions. Our new astrometric measurements show that the companion has nearly completed one orbital revolution since its discovery in 1997. The derived orbital elements imply a short-period (P=11.3 yrs) and high-eccentricity orbit (e=0.6) with periastron passage around 2002.6. The new orbit is consistent with recently published radial velocity measurements, from which we can also derive the first direct constraints on the mass ratio of the binary components. We employ various methods to derive the system mass (M_system=44+/-7 M_sun) and the dynamical distance (d=410+/-20 pc), which is in remarkably good agreement with recently published trigonometric parallax measurements obtained with radio interferometry.