  We present Atacama Large Millimeter Array (ALMA) observations of two
high-redshift systems (SMMJ02399-0136 and the Cloverleaf QSO) in their
rest-frame 122 micron continuum (~650 GHz or ~450 micron on-sky) and [NII] 122
micron line emission. The continuum observations with a synthesized beam of
~0.25" resolve both sources and recover the expected flux. The Cloverleaf is
resolved into a partial Einstein ring, while the SMMJ02399-0136 is
unambiguously separated into two components; an AGN associated point source and
an extend region at the location of a previously identified dusty starburst. We
detect the [NII] line in both systems, though significantly weaker than our
previous detections made with the 1st generation z(Redshift) and Early Universe
Spectrometer. We show that this discrepancy is mostly explained if the line
flux is resolved out due to significantly more extended emission and longer
ALMA baselines than expected. Based on the ALMA observations we determine that
greater than 75% of the total [NII] line flux in each source is produced via
star formation. We use the [NII] line flux that is recovered by ALMA to
constrain the N/H abundance, ionized gas mass, hydrogen ionizing photon rate,
and star formation rate. In SMMJ02399-0136 we discover it contains a
significant amount (~1000 solar masses per year) of unobscured star formation
in addition to its dusty starburst and argue that SMMJ02399-0136 may be similar
to the Antennae Galaxies (Arp 244) locally. In total these observations provide
a new look at two well-studied systems while demonstrating the power and
challenges of Band-9 ALMA observations of high-z systems.
