A Centimeter-wave Study of Methanol and Ammonia Isotopologues in Sgr B2(N): Physical and Chemical Differentiation between Two Hot Cores

We present new radio-frequency interferometric maps of emission from the 14NH3, 15NH3, and 14NH2D isotopologues of ammonia, and the 12CH3OH and 13CH3OH isotopologues of methanol toward Sgr B2(N). With a resolution of ~3'' (0.1 pc), we are able to spatially resolve emission from two hot cores in this source and separate it from absorption against the compact HII regions in this area. The first (N1) is the well-known v = 64 km/s core, and the second (N2) is a core 6'' to the north at v = 73 km/s. Using emission from 15NH3, and hyperfine satellites of 14NH3 metastable transitions we estimate the 14NH3 column densities of these sources and compare them to those of 14NH2D. We find that the ammonia deuteration fraction of N2 is roughly 10-20 times higher than in N1. We also measure an [15NH3/14NH3] abundance ratio that is apparently 2-3 times higher in N2 than N1, which could indicate a correspondingly higher degree of nitrogen fractionation in N2. In addition, we find that N2 has a factor of 7 higher methanol abundance than N1. Together, these abundance signatures suggest that N2 is a younger source, for which species characteristic of grain chemistry at low temperatures are currently being actively liberated from ice mantles, and have not yet reached chemical equilibrium in the warm gas phase. The high D abundance and possible high 15N abundance in NH3 found in N2 are interesting for studying the potential interstellar origin of abundances in primitive solar system material.