RESOLVED DEPLETION ZONES AND SPATIAL DIFFERENTIATION OF N{sub 2}H{sup +} AND N{sub 2}D{sup +}

We present a study on the spatial distribution of N{sub 2}D{sup +} and N{sub 2}H{sup +} in 13 protostellar systems. Eight of thirteen objects observed with the IRAM 30 m telescope show relative offsets between the peak N{sub 2}D{sup +} (J = 2 {yields} 1) and N{sub 2}H{sup +} (J = 1 {yields} 0) emission. We highlight the case of L1157 using interferometric observations from the Submillimeter Array and Plateau de Bure Interferometer of the N{sub 2}D{sup +} (J = 3 {yields} 2) and N{sub 2}H{sup +} (J = 1 {yields} 0) transitions, respectively. Depletion of N{sub 2}D{sup +} in L1157 is clearly observed inside a radius of {approx}2000 AU (7'') and the N{sub 2}H{sup +} emission is resolved into two peaks at radii of {approx}1000 AU (3.''5), inside the depletion region of N{sub 2}D{sup +}. Chemical models predict a depletion zone in N{sub 2}D{sup +} and N{sub 2}H{sup +} due to destruction of H{sub 2}D{sup +} at T {approx} 20 K and the evaporation of CO off dust grains at the same temperature. However, the abundance offsets of 1000 AU between the two species are not reproduced by chemical models, including a model that follows the infall of the protostellar envelope. The average abundance ratios of N{sub 2}D{sup +} to N{sub 2}H{sup +} have been shown to decrease as protostars evolve by Emprechtinger et al., but this is the first time depletion zones of N{sub 2}D{sup +} have been spatially resolved. We suggest that the difference in depletion zone radii for N{sub 2}H{sup +} and N{sub 2}D{sup +} is caused by either the CO evaporation temperature being above 20 K or an H{sub 2} ortho-to-para ratio gradient in the inner envelope.