We have carried out a comprehensive and self-consistent study of the physic
al and chemical state of the core of the dark cloud L134N (L183), whose mol
ecular abundances provide a standard against which chemical models may be c
ompared. We used observations of the NH3(1, 1) and (2, 2) rotation-inversio
n transitions to estimate the kinetic temperature, which was found to be co
nsistent with 10 K and not varying with position. Densities were determined
from multitransition statistical equilibrium calculations for HC3N, N2H+,
and CS. The average density toward all lines of sight was 2 x 10(4) cm(-3).
As found by previous studies, the emission from various molecular species
peaks in different positions: SO and SO2 peak west of the central position,
which is the location of the strongest emission from (e.g.) N2H+ and CH3OH
, with a second peak occurring for NH3 and HC3N to the north of the center.
The most striking abundance variations occur in a north-south cut through
the core center for HC3N, C2H, CS, SO, and SO2. A north to south decrease i
n the abundance of HC3N and CS and a dramatic change in the CS/SO ratio, wh
ich has been shown to be a sensitive tracer of chemical evolutionary state,
suggests that the north is at a younger evolutionary state than the south.
Despite the "youth" of the N position, the CS/SO ratio suggests that it is
still as "old" as or older than the most evolved region in TMC-1 (the nort
hwest end of the ridge).