N[TINF]2[/TINF]H[TSUP]+[/TSUP] and C[TSUP]18[/TSUP]O Depletion in a Cold Dark Cloud

We present sensitive, high angular resolution molecular line observations of C 18 O and N 2 H + toward the dark globule B68. We directly compare these data with the near-infrared extinction measurements of Alves, Lada, & Lada to derive the first evidence for the depletion of N 2 H + , and by inference N 2 , in a prestellar dark cloud. We also find widespread C 18 O depletion throughout the centrally condensed core of the B68 cloud. Specifically, we find the N 2 H + emission to peak in a shell partially surrounding the peak of dust extinction. Moreover, N 2 H + peaks inside the much larger C 18 O depletion hole and has a smaller depletion zone, confirming theoretical predictions. These data are analyzed through a direct coupling of time-dependent chemical models to a radiation transfer code. This analysis highlights the importance of photodissociation at cloud edges and suggests that the CO abundance declines by 2 orders of magnitude from edge to center. In contrast, N 2 H + declines in abundance, at minimum, by at least a factor of 2. Indeed, it is entirely possible that both N 2 H + and N 2 are completely absent from the central regions of the B68 core. The depletion of N 2 H + , and its parent molecule N 2 , opens up the possibility that the centers of dense cores, prior to the formation of a star, may evade detection by conventional methods of probing cores using molecular emission. Under these conditions, H 2 D + may be the sole viable molecular probe of the innermost regions of star-forming cores.