We present observations of the intermediate to massive star-forming region
I05345+3157 using the molecular line tracer CS(2-1) with CARMA to reveal the
properties of the dense gas cores. Seven gas cores are identified in the
integrated intensity map of CS(2-1). Among these, core 1 and core 3 have
counterparts in the 2.7 millimeter continuum data. We suggest that core 1 and
core 3 are star-forming cores that may already or will very soon harbor young
massive protostars. The total masses of core 1 estimated from the LTE method
and dust emission by assuming a gas-to-dust ratio are 5 +- 1 solar masses and
18 +- 6 solar masses, and that of core 3 are 15 +- 7 solar masses and 11 +- 3
solar masses. The spectrum of core 3 shows blue-skewed self-absorption, which
suggests gas infall -- a collapsing core. The observed broad linewidths of the
seven gas cores indicate non-thermal motions. These non-thermal motions can be
interactions with nearby outflows or due to the initial turbulence; the former
is observed, while the role of initial turbulence is less certain. Finally, the
virial masses of the gas cores are larger than the LTE masses, which for a
bound core implies a requirement on the external pressure of ~ 10^8 K/cm^3. The
cores have the potential to further form massive stars.Comment: Accepted for publication in MNRA
