We present observations of 12C32S, 12C34S,
13C32S and 12C33S J=2−1 lines toward a large sample of
massive star forming regions by using the Arizona Radio Observatory 12-m
telescope and the IRAM,30-m. Taking new measurements of the carbon
12C/13C ratio, the 32S/34S isotope ratio was determined
from the integrated 13C32S/12C34S line intensity ratios for
our sample. Our analysis shows a 32S/34S gradient from the inner
Galaxy out to a galactocentric distance of 12,kpc. An unweighted least-squares
fit to our data yields 32S/34S = (1.56 ± 0.17)DGC
- (6.75 ± 1.22) with a correlation coefficient of 0.77. Errors represent
1σ standard deviations. Testing this result by (a) excluding the
Galactic center region, (b) excluding all sources with C34S opacities >
0.25, © combining our data and old data from previous study, and (d) using
different sets of carbon isotope ratios leads to the conclusion that the
observed 32S/34S gradient is not an artefact but persists
irrespective of the choice of the sample and carbon isotope data. A gradient
with rising 32S/34S values as a function of galactocentric radius
implies that the solar system ratio should be larger than that of the local
interstellar medium. With the new carbon isotope ratios we obtain indeed a
local 32S/34S isotope ratio about 10% below the solar system
one, as expected in case of decreasing 32S/34S ratios with time and
increased amounts of stellar processing. However, taking older carbon isotope
ratios based on a lesser amount of data, such a decrease is not seen. No
systematic variation of 34S/33S ratios along galactocentric
distance was found.