paper

FAUST XVII: Super deuteration in the planet forming system IRS 63 where the streamer strikes the disk

arXiv:2407.04813 · doi:10.1051/0004-6361/202450742

Abstract

Recent observations suggest that planets formation starts early, in protostellar disks of $\leq 1 0^{5}$ yrs, which are characterized by strong interactions with the environment, e.g., through accretion streamers and molecular outflows. To investigate the impact of such phenomena on disk physical and chemical properties it is key to understand what chemistry planets inherit from their natal environment. In the context of the ALMA Large Program Fifty AU STudy of the chemistry in the disk/envelope system of Solar-like protostars (FAUST), we present observations on scales from ~1500 au to ~60 au of H $_{2}$ CO, HDCO, and D $_{2}$ CO towards the young planet-forming disk IRS~63. H $_{2}$ CO probes the gas in the disk as well as in a large scale streamer (~1500 au) impacting onto the South-East (SE) disk side. We detect for the first time deuterated formaldehyde, HDCO and D $_{2}$ CO, in a planet-forming disk, and HDCO in the streamer that is feeding it. This allows us to estimate the deuterium fractionation of H $_{2}$ CO in the disk: [HDCO]/[H $_{2}$ CO] $\sim 0.1 - 0.3$ and [D $_{2}$ CO]/[H $_{2}$ CO] $\sim 0.1$ . Interestingly, while HDCO follows the H $_{2}$ CO distribution in the disk and in the streamer, the distribution of D $_{2}$ CO is highly asymmetric, with a peak of the emission (and [D]/[H] ratio) in the SE disk side, where the streamer crashes onto the disk. In addition, D $_{2}$ CO is detected in two spots along the blue- and red-shifted outflow. This suggests that: (i) in the disk, HDCO formation is dominated by gas-phase reactions similarly to H $_{2}$ CO, while (ii) D $_{2}$ CO was mainly formed on the grain mantles during the prestellar phase and/or in the disk itself, and is at present released in the gas-phase in the shocks driven by the streamer and the outflow. These findings testify on the key role of streamers in the build-up of the disk both concerning the final mass available for planet formation and its chemical composition.

12 pages, 10 figures, accepted for publication on A&A