2020A&A...636A..26H

Context. Water is a key volatile that provides insight into the initial stages of planet formation. The low water abundances inferred from water observations toward low-mass protostellar objects may point to a rapid locking of water as ice by large dust grains during star and planet formation. However, little is known about the water vapor abundance in newly formed planet-forming disks.
Aims. We aim to determine the water abundance in embedded Keplerian disks through spatially-resolved observations of H₂¹⁸O lines to understand the evolution of water during star and planet formation.
Methods. We present H₂¹⁸O line observations with ALMA and NOEMA millimeter interferometers toward five young stellar objects. NOEMA observed the 3_1,3-2_2,0 line (E_up/k_B=203.7K) while ALMA targeted the 4_1,4-3_2,1 line (E_up/k_B=322.0K). Water column densities were derived considering optically thin and thermalized emission. Our observations were sensitive to the emission from the known Keplerian disks around three out of the five Class I objects in the sample.
Results. No H₂¹⁸O emission is detected toward any of our five Class I disks. We report upper limits to the integrated line intensities. The inferred water column densities in Class I disks are N_H218^O<10¹⁵cm^–2 on 100 au scales, which include both the disk and envelope. The upper limits imply a disk-averaged water abundance of ≤10^–6 with respect to H₂ for Class I objects. After taking the physical structure of the disk into account, the upper limit to the water abundance averaged over the inner warm disk with T>100K is between ∼10^–7 and 10^–5.
Conclusions. Water vapor is not abundant in warm protostellar envelopes around Class I protostars. Upper limits to the water vapor column densities in Class I disks are at least two orders of magnitude lower than values found in Class 0 disk-like structures.