  Studying the physical and chemical conditions of young embedded disks is
crucial to constrain the initial conditions for planet formation. Here, we
present Atacama Large Millimeter/submillimeter Array (ALMA) observations of
dust continuum at $\sim$0.06" (8 au) resolution and molecular line emission at
$\sim$0.17" (24 au) resolution toward the Class 0 protostar L1527 IRS from the
Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum
emission is smooth without substructures, but asymmetric along both the major
and minor axes of the disk as previously observed. The detected lines of
$^{12}$CO, $^{13}$CO, C$^{18}$O, H$_2$CO, c-C$_3$H$_2$, SO, SiO, and DCN trace
different components of the protostellar system, with a disk wind potentially
visible in $^{12}$CO. The $^{13}$CO brightness temperature and the H$_2$CO line
ratio confirm that the disk is too warm for CO freeze out, with the snowline
located at $\sim$350 au in the envelope. Both molecules show potential evidence
of a temperature increase around the disk-envelope interface. SO seems to
originate predominantly in UV-irradiated regions such as the disk surface and
the outflow cavity walls rather than at the disk-envelope interface as
previously suggested. Finally, the continuum asymmetry along the minor axis is
consistent with the inclination derived from the large-scale (100" or 14,000
au) outflow, but opposite to that based on the molecular jet and envelope
emission, suggesting a misalignment in the system. Overall, these results
highlight the importance of observing multiple molecular species in multiple
transitions to characterize the physical and chemical environment of young
disks.
