We present ALMA observations of the Class I source Oph IRS63 in the context
of the Early Planet Formation in Embedded Disks (eDisk) large program. Our ALMA
observations of Oph IRS63 show a myriad of protostellar features, such as a
shell-like bipolar outflow (in 12CO), an extended rotating envelope
structure (in 13CO), a streamer connecting the envelope to the disk (in
C18O), and several small-scale spiral structures seen towards the edge of
the dust continuum (in SO). By analyzing the velocity pattern of 13CO and
C18O, we measure a protostellar mass of M⋆=0.5±0.2~M⊙ and confirm the presence of a disk rotating at almost Keplerian
velocity that extends up to ∼260 au. These calculations also show that the
gaseous disk is about four times larger than the dust disk, which could
indicate dust evolution and radial drift. Furthermore, we model the C18O
streamer and SO spiral structures as features originating from an infalling
rotating structure that continuously feeds the young protostellar disk. We
compute an envelope-to-disk mass infall rate of ∼10−6~M⊙yr−1 and compare it to the disk-to-star mass accretion rate of ∼10−8~M⊙yr−1, from which we infer that the protostellar
disk is in a mass build-up phase. At the current mass infall rate, we speculate
that soon the disk will become too massive to be gravitationally stable.Comment: 26 pages and 17 figure