Oral Presentation
Dissecting the massive YSO G335-MM1: a potential multiple system?
Presenter: Fernando Olguin (National Tsing Hua University)
Binary/multiple stellar systems are ubiquitous and relatively common. Recent ALMA observations have started to shed light into the formation of high- and low-mass binary systems, but observational evidence of in-situ formation of a multiple massive stellar system is more elusive. In this presentation, we will show the latest results of our study of the high-mass star forming region G335.579-0.272 MM1 (hereafter G335-MM1). This young and luminous (L>10E4 Lsun) region, located at 3.25 kpc, is within one of the most massive IR dark clouds in the Galaxy and being fed by large-scale filaments (Peretto et al. 2013). Our ALMA observations reveal that this region has several molecular cores (size <0.1 pc), with one the most massive showing clear evince of rotation. Most strikingly, we see from 0.05" (160 au) resolution observations that in the most massive core a multiple system is potentially forming.
At the potential location of the proto-stars the dust continuum becomes optically thick. The system also shows extended line emission which seems to be tracing a common disk/envelope, and is powering a single molecular outflow. Radio and maser emission (Avison et al. 2015) indicates that at least one of the proto-stars is massive with a potential spectral type B, but since the system is fed by large scale filaments the proto-stars can grow further. Higher-resolution radio or recombination lines observations will be needed to assign an specific origin to the ionizing radiation and to investigate its effect on the inflow of matter.
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