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We have observed the clump G34.43+00.24 MM3 associated with an infrared darkcloud in DNC $J$=3--2, HN$^{13}$C $J$=3--2, and N$_2$H$^+$ $J$=3--2 with theAtacama Large Millimeter/submillimeter Array (ALMA). The N$_2$H$^+$ emission isfound to be relatively weak near the hot core and the outflows, and itsdistribution is clearly anti-correlated with the CS emission. This resultindicates that a young outflow is interacting with cold ambient gas. TheHN$^{13}$C emission is compact and mostly emanates from the hot core, whereasthe DNC emission is extended around the hot core. Thus, the DNC and HN$^{13}$Cemission traces warm regions near the protostar differently. The DNC emissionis stronger than the HN$^{13}$C emission toward most parts of this clump. TheDNC/HNC abundance ratio averaged within a $15^{\prime\prime} \times15^{\prime\prime}$ area around the phase center is higher than 0.06. This ratiois much higher than the value obtained by the previous single-dish observationsof DNC and HN$^{13}$C $J$=1--0 ($\sim$0.003). It seems likely that the DNC andHNC emission observed with the single-dish telescope traces lower densityenvelopes, while that observed with ALMA traces higher density and highlydeuterated regions. We have compared the observational results withchemical-model results in order to investigate the behavior of DNC and HNC inthe dense cores. Taking these results into account, we suggest that the lowDNC/HNC ratio in the high-mass sources obtained by the single-dish observationsare at least partly due to the low filling factor of the high density regions.

ALMA Observations of the IRDC Clump G34.43+00.24 MM3: DNC/HNC Ratio