Binary system and jet precession and expansion in G35.20–0.74N⋆
1 INAF–Osservatorio Astrofisico di
Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
2 I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
3 National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan
4 Department of Astronomical Sciences, SOKENDAI (The Graduate University for Advanced Studies), Mitaka, Tokyo 181-8588, Japan
5 Centre for Astrophysics, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK
6 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal
Accepted: 13 June 2016
Context. Atacama Large Millimeter/submillimeter Array (ALMA) observations of the high-mass star-forming region G35.20−0.74N have revealed the presence of a Keplerian disk in core B rotating about a massive object of 18 M⊙, as computed from the velocity field. The luminosity of such a massive star would be comparable to (or higher than) the luminosity of the whole star-forming region. To solve this problem it has been proposed that core B could harbor a binary system. This could also explain the possible precession of the radio jet associated with this core, which has been suggested by its S-shaped morphology.
Aims. We establish the origin of the free-free emission from core B and investigate the existence of a binary system at the center of this massive core and the possible precession of the radio jet.
Methods. We carried out VLA continuum observations of G35.20−0.74N at 2 cm in the B configuration and at 1.3 cm and 7 mm in the A and B configurations. The bandwidth at 7 mm covers the CH3OH maser line at 44.069 GHz. Continuum images at 6 and 3.6 cm in the A configuration were obtained from the VLA archive. We also carried out VERA observations of the H2O maser line at 22.235 GHz.
Results. The observations have revealed the presence of a binary system of UC/HC Hii regions at the geometrical center of the radio jet in G35.20−0.74N. This binary system, which is associated with a Keplerian rotating disk, consists of two B-type stars of 11 and 6 M⊙. The S-shaped morphology of the radio jet has been successfully explained as being due to precession produced by the binary system. The analysis of the precession of the radio jet has allowed us to better interpret the IR emission in the region, which would be not tracing a wide-angle cavity open by a single outflow with a position angle of ~55°, but two different flows: a precessing one in the NE–SW direction associated with the radio jet, and a second one in an almost E–W direction. Comparison of the radio jet images obtained at different epochs suggests that the jet is expanding at a maximum speed on the plane of the sky of 300 km s-1. The proper motions of the H2O maser spots measured in the region also indicate expansion in a direction similar to that of the radio jet.
Conclusions. We have revealed a binary system of high-mass young stellar objects embedded in the rotating disk in G35.20−0.74N. The presence of a massive binary system is in agreement with the theoretical predictions of high-mass star formation, according to which the gravitational instabilities during the collapse would produce the fragmentation of the disk and the formation of such a system. For the first time, we have detected a high-mass young star associated with an UC/HC Hii region and at the same time powering a radio jet.
Key words: ISM: individual objects: G35.20-0.74N / Hii regions / ISM: jets and outflows / stars: formation
The reduced images (FITS files) is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/593/A49
© ESO, 2016