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We have observed the 70 $\mu$m dark infrared dark cloud (IRDC) G14.492-00.139in the N$_2$D$^+$ $J$=3--2, DCO$^+$ $J$=3--2, DCN $J$=3--2, and C$^{18}$O$J$=2--1 lines, using the Atacama Large Millimeter/submillimeter Array (ALMA)as part of the ALMA Survey of 70 $\mu$m Dark High-mass Clumps in Early Stages(ASHES). We find that the spatial distribution is different among the observedemission from the deuterated molecular lines. The N$_2$D$^+$ emission tracesrelatively quiescent regions, while both the DCO$^+$ and DCN emission emanatesmainly from regions with signs of active star-formation. In addition, theDCO$^+$/N$_2$D$^+$ ratio is found to be lower in several dense cores than instarless cores embedded in low-mass star-forming regions. By comparing theobservational results with chemical model calculations, we discuss the originof the low DCO$^+$/N$_2$D$^+$ ratio in this IRDC clump. The lowDCO$^+$/N$_2$D$^+$ ratio can be explained if the temperature of the dense coresis in the range between the sublimation temperature of N$_2$ ($\sim$20 K) andCO ($\sim$25 K). The results suggest that the dense cores in G14.492-00.139 arewarmer and denser than the dense cores in low-mass star-forming regions.

The ALMA Survey of 70 $\mu$m Dark High-mass Clumps in Early Stages (ASHES). V. Deuterated Molecules in the 70 $\mu$m dark IRDC G14.492-00.139