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We investigate molecular evolution from a molecular cloud core to a firsthydrostatic core in three spatial dimensions. We perform a radiationhydrodynamic simulation in order to trace fluid parcels, in which molecularevolution is investigated, using a gas-phase and grain-surface chemicalreaction network. We derive spatial distributions of molecular abundances andcolumn densities in the core harboring the first core. We find that the totalof gas and ice abundances of many species in a cold era (10 K) remain unaltereduntil the temperature reaches ~500 K. The gas abundances in the warm envelopeand the outer layer of the first core (T < 500 K) are mainly determined via thesublimation of ice-mantle species. Above 500 K, the abundant molecules, such asH2CO, start to be destroyed, and simple molecules, such as CO, H2O and N2 arereformed. On the other hand, some molecules are effectively formed at hightemperature; carbon-chains, such as C2H2 and cyanopolyynes, are formed at thetemperature of >700 K. We also find that large organic molecules, such as CH3OHand HCOOCH3, are associated with the first core (r < 10 AU). Although theabundances of these molecules in the first core stage are comparable or lessthan in the protostellar stage (hot corino), reflecting the lower luminosity ofthe central object, their column densities in our model are comparable to theobserved values toward the prototypical hot corino, IRAS 16293-2422. We proposethat these large organic molecules can be good tracers of the first cores.

Chemistry in the First Hydrostatic Core Stage By Adopting Three-Dimensional Radiation Hydrodynamic Simulations