Fernando Olguin (NTHU), Patricio Sanhueza (NAOJ), Vivien Chen (NTHU)
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 poster, we will summarise our analysis of the dust continuum emission and kinematics 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). We will show evidence of rotation and expansion motions towards its most massive core as revealed by our ALMA observations. Furthermore, we will show that this core fragments into a potential multiple system with at least one high-mass (proto-)star.