Water Vapor in the Inner 25 AU of a Young Disk around a Low-Mass Protostar

TL;DR

This study presents the first spatially resolved observation of water vapor emission in the inner 25 AU of a young protostellar disk, revealing a warm, thin water layer with a tentative velocity gradient, indicative of disk-related processes.

Contribution

It provides the first spatially resolved detection of water vapor in a young protostellar disk, offering insights into disk composition and kinematics at early stages.

Findings

Water vapor detected within 25 AU of the protostar.

Emission suggests a thin, warm water layer in the disk.

Evidence of a velocity gradient perpendicular to outflow direction.

Abstract

Water is one of the key molecules in the physical and chemical evolution of star- and planet-forming regions. We here report the first spatially resolved observation of thermal emission of (an isotopologue of) water with the Plateau de Bure Interferometer toward the deeply embedded Class 0 protostar NGC 1333-IRAS4B. The observations of the H2-18-O 3_13-2_20 transition at 203.4 GHz resolve the emission of water toward this source with an extent of about 0.2" corresponding to the inner 25 AU (radius). The H2-18-O emission reveals a tentative velocity gradient perpendicular to the extent of the protostellar outflow/jet probed by observations of CO rotational transitions and water masers. The line is narrow, about 1 km/s (FWHM), significantly less than what would be expected for emission from an infalling envelope or accretion shock, but consistent with emission from a disk seen at a low inclination angle. The water column density inferred from these data suggests that the water emitting gas is a thin warm layer containing about 25 M_Earth of material, 0.03% of the total disk mass traced by continuum observations.