A JWST inventory of protoplanetary disk ices: The edge-on protoplanetary disk HH 48 NE, seen with the Ice Age ERS program

Ices are the main carriers of volatiles in protoplanetary disks and are crucial to our understanding of the protoplanetary disk chemistry that ultimately sets the organic composition of planets. The Director’s Discretionary-Early Release Science (DD-ERS) program Ice Age on the James Webb Space Telescope (JWST) follows the ice evolution through all stages of star and planet formation. JWST’s exquisite sensitivity and angular resolution uniquely enable detailed and spatially resolved inventories of ices in protoplanetary disks. JWST/NIRSpec observations of the edge-on Class II protoplanetary disk HH 48 NE reveal spatially resolved absorption features of the major ice components H2O, CO2, CO, and multiple weaker signatures from less abundant ices NH3 , OCN− , and OCS. We also detect 13 CO2 ice for the first time in a protoplanetary disk. Since multiple complex light paths contribute to the observed flux, the ice absorption features are filled in by ice-free scattered light. This implies that observed optical depths should be interpreted as lower limits to the total ice column in the disk and that abundance ratios cannot be determined directly from the spectrum. The 12CO2/13CO2 integrated absorption ratio of 11 implies that the 12CO2 feature is saturated, without the flux approaching 0, indicative of a very high CO2 column density on the line of sight, and a corresponding abundance with respect to hydrogen that is higher than ISM values by a factor of at least a few. Observations of rare isotopologues are crucial, as we show that the 13CO2 observation allows us to determine the column density of CO2 to be at least 2.3 × 1018 cm−2; more than an order of magnitude higher than the lower limit directly inferred from the observed optical depth. Spatial variations in the depth of the strong ice features are smaller than a factor of two. Radial variations in ice abundance, e.g., snowlines, are largely washed out since all observed photons have passed through the full radial extent of the disk. CO ice is observed at perplexing heights in the disk, extending to the top of the CO-emitting gas layer. Although poorly understood radiative transfer effects could contribute, we argue that the most likely interpretation is that we observe some CO ice at high temperatures, trapped in less volatile ices like H2O and CO2. Future radiative transfer models are necessary to constrain the physical origin of the ice absorption and the implications of these observations on our current understanding of disk physics and chemistry.