On the internal structure of starless cores. II. A molecular survey of L1498 and L1517B

Details On the internal structure of starless cores. II. A molecular survey of L1498 and L1517B On the internal structure of starless cores. II. A molecular survey of L1498 and L1517B

2006-05-19

arxiv.org/abs/astro-ph/0605513v1

Astronomy and Astrophysics

Astrophysics

22 pages, 12 figures, A&A accepted

Scientific paper

10.1051/0004-6361:20065311

[Abridged] We present a molecular survey of the starless cores L1498 and L1517B. These cores have been selected for their relative isolation and close-to-round shape, and they have been observed in a number of lines of 13 molecular species (4 already presented in the first part of this series): CO, CS, N2H+, NH3, CH3OH, SO, C3H2, HC3N, C2S, HCN, H2CO, HCO+, and DCO+. Using a physical model of core structure and a Monte Carlo radiative transfer code, we determine for each core a self-consistent set abundances that fits simultaneously the observed radial profile of integrated intensity and the emergent spectrum towards the core center (for abundant species, optically thin isopologues are used). From this work, we find that L1498 and L1517B have similar abundance patterns, with most species suffering a significant drop toward the core center. This occurs for CO, CS, CH3OH, SO, C3H2, HC3N, C2S, HCN, H2CO, HCO+, and DCO+, which we fit with profiles having a sharp central hole. The size of this hole varies with molecule: DCO+, HCN, and HC3N have the smallest holes while SO, C2S and CO have the largest holes. Only N2H+ and NH3 are present in the gas phase at the core centers. From the different behavior of molecules, we select SO, C2S, and CH3OH as the most sensitive tracers of molecular depletion. Comparing our abundance determinations with the predictions from current chemical models we find order of magnitude discrepancies. Finally, we show how the ``contribution function'' can be used to study the formation of line profiles from the different regions of a core.

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