  We present Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 3
observations of 73 starless and protostellar cores in the Orion B North
molecular cloud. We detect a total of 34 continuum sources at 106 GHz, and
after comparisons with other data, 4 of these sources appear to be starless.
Three of the four sources are located near groupings of protostellar sources,
while one source is an isolated detection. We use synthetic observations of a
simulation modeling a collapsing turbulent, magnetized core to compute the
expected number of starless cores that should be detectable with our ALMA
observations and find at least two (1.52) starless core should be detectable,
consistent with our data. We run a simple virial analysis of the cores to put
the Orion B North observations into context with similar previous ALMA surveys
of cores in Chamaeleon I and Ophiuchus. We conclude that the Chamaeleon I
starless core population is characteristically less bounded than the other two
populations, along with external pressure contributions dominating the binding
energy of the cores. These differences may explain why the Chamaeleon I cores
do not follow turbulent model predictions, while the Ophiuchus and Orion B
North cores are consistent with the model.
