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Protostellar disks are a ubiquitous part of the star formation process andthe future sites of planet formation. As part of the Early Planet Formation inEmbedded Disks (eDisk) large program, we present high-angular resolution dustcontinuum ($\sim40\,$mas) and molecular line ($\sim150\,$mas) observations ofthe Class 0 protostar, IRAS 15398-3359. The dust continuum is small, compact,and centrally peaked, while more extended dust structures are found in theoutflow directions. We perform a 2D Gaussian fitting to find the deconvolvedsize and $2\sigma$ radius of the dust disk to be $4.5\times2.8\,\mathrm{au}$and $3.8\,\mathrm{au}$, respectively. We estimate the gas+dust disk massassuming optically thin continuum emission to be $0.6-1.8\,M_\mathrm{jup}$,indicating a very low-mass disk. The CO isotopologues trace components of theoutflows and inner envelope, while SO traces a compact, rotating disk-likecomponent. Using several rotation curve fittings on the PV diagram of the SOemission, the lower limits of the protostellar mass and gas disk radius are$0.022\,M_\odot$ and $31.2\,\mathrm{au}$ from our Modified 2 single power-lawfitting. A conservative upper limit of the protostellar mass is inferred to be$0.1\,M_\odot$. The protostellar mass-accretion rate and the specific angularmomentum at the protostellar disk edge are found to be between$1.3-6.1\times10^{-6}\,M_\odot\,\mathrm{yr^{-1}}$ and$1.2-3.8\times10^{-4}\,\mathrm{km\,s^{-1}\,pc}$, respectively, with an ageestimated between $0.4-7.5\times10^{4}\,$yr. At this young age with no clearsubstructures in the disk, planet formation would likely not yet have started.This study highlights the importance of high-resolution observations andsystematic fitting procedures when deriving dynamical properties of deeplyembedded Class 0 protostars.

Early Planet Formation in Embedded Disks (eDisk). VIII. A Small  Protostellar Disk around the Extremely Low-Mass and Young Class 0 Protostar,  IRAS 15398-3359