Physical and Chemical Structure of the Disk and Envelope of the Class 0/I Protostar L1527

Abstract Submillimeter spectral line and continuum emission from the protoplanetary disks envelopes of protostars is a powerful probe their structure, chemistry, dynamics. Here we present benchmark study our modeling code, RadChemT, that for first time uses chemical model to reproduce ALMA C 18 O (2–1), CARMA 12 CO (1–0) N 2 H + observations L1527; this allows us distinguish disk, infalling envelope, outflow Class 0/I protostar. RadChemT combines dynamics, radiative transfer, gas gas–grain reactions generate models can be directly compared with individual protostars. Rather than individually fit abundances large number free parameters, aim best match maps by (i) adopting physical based on density structure luminosity derived primarily previous work energy distribution 2D imaging data, updating it include narrow jet detected in data near (?75 au) protostar, then (ii) computing resulting astrochemical 292 species. Our reproduces strengths within factor 3.0; encouraging considering pronounced abundance variation (factor >10 3 ) between shell snowline region midplane. Further, confirms suggestions regarding anticorrelation 400 au 2000 central star. tools represent new capability which exploit richness provided modern submillimeter interferometers.