  We report interferometric observations of the high-mass star-forming object
IRAS 23033+5951. Our observations reveal two massive molecular cloud cores,
designated IRAS 23033+5951-MMS1 and IRAS 23033+5951-MMS2. MMS1 has already
formed a massive protostar and MMS2 appears to be on the verge of doing so. The
latter core may be an example of a massive analogue to a "Class 0" star-forming
object. The more evolved core shows some evidence of N2H+ destruction near the
protostar, consistent with similar findings in low-mass star-forming objects.
In addition to the already-known prominent HCO+ outflow, our SiO 2--1, and
CH3OH 2--1 maps show evidence for two more candidate outflows, both presumably
less powerful than the main one. Both cores are embedded in an elongated
feature whose major axis is oriented almost exactly perpendicular to the axis
of the most prominent outflow in the region. Although it has many of the
characteristics of a disk, the 87,000 AU (0.42 pc) diameter of this structure
suggests that it is more likely to be the flattened, rotating remnant of the
natal molecular cloud fragment from which the star-forming cores condensed. We
conclude that IRAS 23033+5951 is an excellent example of massive star formation
proceeding in relative isolation, perhaps by the method of monolithic collapse
and disk accretion.
