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We present molecular line observations, made with angular resolutions of~20", toward the filamentary infrared dark cloud G34.43+0.24 using the APEX[CO(3-2), 13CO(3-2), C18O(3-2) and CS(7-6) transitions], Nobeyama 45 m[CS(2-1), SiO(2-1), C34S(2-1), HCO+(1-0), H13CO+(1-0) and CH3OH(2-1)transitions], and SEST [CS(2-1) and C18O(2-1) transitions] telescopes. We findthat the spatial distribution of the molecular emission is similar to that ofthe dust continuum emission observed with 11" resolution showing a filamentarystructure and four cores. The cores have local thermodynamic equilibrium massesranging from 3.3x10^2 - 1.5x10^3 solar masses and virial masses from 1.1x10^3 -1.5x10^3 solar masses, molecular hydrogen densities between 1.8x10^4 and3.9x10^5 cm^{-3}, and column densities >2.0x10^{22} cm^{-2}; valuescharacteristics of massive star forming cores. The 13CO(3-2) profile observedtoward the most massive core reveals a blue profile indicating that the core isundergoing large-scale inward motion with an average infall velocity of 1.3km/s and a mass infall rate of 1.8x10^{-3} solar masses per year. We report thediscovery of a molecular outflow toward the northernmost core thought to be ina very early stage of evolution. We also detect the presence of high velocitygas toward each of the other three cores, giving support to the hypothesis thatthe excess 4.5 $\mu$ emission ("green fuzzies") detected toward these cores isdue to shocked gas. The molecular outflows are massive and energetic, withmasses ranging from 25 -- 80 solar masses, momentum 2.3 - 6.9x10^2 \Msun km/s,and kinetic energies 1.1 - 3.6x10^3 \Msun km^2 s^{-2}; indicating that they aredriven by luminous, high-mass young stellar objects.

Molecular outflows within the filamentary infrared dark cloud G34.43+0.24