The ALMA-PILS survey: 3D modeling of the envelope, disks and dust filament of IRAS 16293-2422

摘要

Context. The Class 0 protostellar binary IRAS 16293-2422 is an interestingtarget for (sub)millimeter observations due to, both, the rich chemistry towardthe two main components of the binary and its complex morphology. Its proximityto Earth allows the study of its physical and chemical structure on solarsystem scales using high angular resolution observations. Such data reveal acomplex morphology that cannot be accounted for in traditional, spherical 1Dmodels of the envelope. Aims. The purpose of this paper is to study theenvironment of the two components of the binary through 3D radiative transfermodeling and to compare with data from the Atacama LargeMillimeter/submillimeter Array. Such comparisons can be used to constrain theprotoplanetary disk structures, the luminosities of the two components of thebinary and the chemistry of simple species. Methods. We present 13CO, C17O andC18O J=3-2 observations from the ALMA Protostellar Interferometric Line Survey(PILS), together with a qualitative study of the dust and gas densitydistribution of IRAS 16293-2422. A 3D dust and gas model including disks and adust filament between the two protostars is constructed which qualitativelyreproduces the dust continuum and gas line emission. Results and conclusions.Radiative transfer modeling of source A and B, with the density solution of aninfalling, rotating collapse or a protoplanetary disk model, can match theconstraints for the disk-like emission around source A and B from the observeddust continuum and CO isotopologue gas emission. If a protoplanetary disk modelis used around source B, it has to have an unusually high scale-height in orderto reach the dust continuum peak emission value, while fulfilling the otherobservational constraints. Our 3D model requires source A to be much moreluminous than source B; LA ~ 18 $L_\odot$ and LB ~ 3 $L_\odot$.