Speaker
Description
Most stars, including our Sun, form in clusters embedded within molecular clouds. It is then important to characterize their formation in dense environments and to asses whether the environments play a role in the subsequent evolution, specially whether planet formation is altered with respect to the more isolated stars formed in dark clouds.
We present ALMA observations at 1.1. mm with an angular resolution of 40 mas (or 70 au) to study the disk population around IRAS 18162-2048, a massive B0-type young stellar object located at 1.7 kpc of distance in the GGD 27 reflection nebula. We obtained two dozens of 1.1 mm continuum sources, most of which are likely tracing the disks around young stellar members of GGD 27 cluster. The derived disk radii (R$_{disk}\simeq20-60$ au) are significantly lower than the typical value found in Taurus, indicating possible tidal or dynamical effects due the presence of the central and massive (50 M$_{\odot}$) protostars.
We will discuss the physical parameters of the disk population (mass, size, surface density, and spatial distribution), the seeds of planet formation, in the context of cluster versus isolated mode of star-formation.
