Volume 554, June 2013
|Number of page(s)||19|
|Section||Interstellar and circumstellar matter|
|Published online||18 June 2013|
Table A.1 lists integrated line strengths of all detected ortho- and para-H2O vapor emission lines and the 1612 MHz OH maser formation rotational cascade lines in the PACS spectrum shown in Figs. 10 and 11. Because the OH emission lines occur in doublets, the integrated line strengths for both components have been summed. We refer to Sylvester et al. (1997) for details on OH spectroscopy. Where confusion due to line blending occurs, we indicate this clearly, as well as list all H2O transitions that may contribute to the emission line. As such we cannot distinguish the relative contribution of each transition in the blend. Blends that might be caused by the emission of other molecules not modeled in this study are not indicated.
© ESO, 2013
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