of the map, in units of both mJy beam$^{-1}$ and  beam$^{-1}$. The coordinates of the map centers were taken from either the positions of interesting objects in the *Spitzer* observations (if available), the location of molecular emission peaks from literature (e.g., Lee et al. 2001; Caselli et al. 2002), or positions suggested by collaborators to optimize the mapping coverage. The B59 core consists of a cluster of low mass sources, and in this survey we only observed the one that is most likely associated with B59-MMS1 (Reipurth et al. 1996; Brooke et al. 2006). Integrations on each source were separated into blocks of ten minutes in stable weather or five minutes in unstable (variable) weather. The pointing was checked every 1-2 hours each night, primarily with planets such as Mars, Uranus, and Neptune. If no planets were available we used secondary objects such as CRL618, IRC+10216, and IRAS 16293-2422. After averaging over all the runs, the blind pointing uncertainty is 21 for azimuth and 31 for zenith angle. But since we corrected the pointing after each check, these actually represent upper limits. For any given observation, the pointing uncertainty should be smaller than this. The pointing sources were also used 