Oral Presentation

The ALMA-JWST synergy: Mapping protostars at high resolution

Author(s): Mayank Narang (ASIAA), ‪Nagayoshi Ohashi‬ (ASIAA)

Presenter: Mayank Narang (Institute of Astronomy and Astrophysics, Academia Sinica)

The masses of stars are determined by flows of gas through protostars: gravitationally driven infall onto the central disks, accretion from the disks onto the stars, and the resulting feedback from accretion-driven jets and winds. Protostars, during their primary accretion phase, are too deeply embedded to be studied with optical and near-IR telescopes. However, with JWST, we can study accretion onto these embedded protostars and investigate the clearing of envelopes by accretion-driven jets/winds and the entrainment of the infalling gas in outflows. Through the Investigation Protostellar Accretion (IPA) JWST cycle-1 GO program, we map the surfaces of the protostellar cavities with 0.1-1” angular resolution, and using the spectral line maps, we trace the shocks from the winds impacting the cavity walls and the ionic jets being launched from the central protostar. However, while JWST can map the ionic, atomic, and molecular species - including H2 - in shock-heated gas, ALMA can map the 3D velocity+spatial distribution of the molecular gas. Using isotopologues of CO and dense gas tracers, ALMA can detect the cool gas that dominates the mass of the envelopes and is too cold to be detected by JWST. Since JWST lacks the angular resolution needed to map the velocity structure of the gas, ALMA is required to map the motions of the gas, measuring both the linewidth and the central velocity of the gas with an angular resolution better than JWST. Such high-resolution ALMA observations have been carried out by the Early Planet Formation in Embedded Disks (eDisk) large program. We will present our preliminary results from the joint analysis of the eDisk ALMA survey and IPA JWST program. We will derive the mass outflow and mass accretion rates onto the protostar from ALMA and compare them with the mass outflow and mass accretion rates derived from JWST. Furthermore, we will compare the distribution of ice and warm dust (from JWST) with the cold gas and dust (from ALMA) content of the protostellar disk.