Volume 521, October 2010
Herschel/HIFI: first science highlights
Article Number L36
Number of page(s) 6
Section Letters
Published online 01 October 2010

Online Material

Appendix A: Observational details

Table A.1 lists the coordinates, observing dates, and the observation identity numbers of our sources along with the assumed distance, the bolometric luminosity, the envelope mass and the source type. For comparison, Ser SMM1 and NGC 1333 IRAS 4 observed with ISO are included as well. For Ser SMM1, we use the average values of the fluxes presented by Larsson et al. (2002). The data for NGC 1333 IRAS 4 are taken from Giannini et al. (2001). Note that for NGC 1333 IRAS 4, we use the luminosity and mass of NGC 1333 IRAS 4A.

Table A.1:   Source properties and observational details.

Appendix B: OH line ratios

\end{figure} Figure B.1:

Ratios of the observed OH fluxes. The numbers denote the corresponding wavelengths. The symbols are: circle for HH 46, upward triangle for TMR 1, downward triangle for IRAS 15398-3359, squares for NGC 7129 FIRS 2, plus signs for DK Cha, crosses for Ser SMM1 and diamonds for NGC 1333 IRAS 4. The color coding is the same as in Fig. 3.

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Appendix C: OH term diagram

\end{figure} Figure C.1:

Level diagram of the lowest excited states of OH up to $E_{{\rm up}} \approx 300~{\rm K}$. Splitting of the levels because of $\Lambda $-doubling and hyperfine structure is not to scale. Transitions observed with PACS are shown in green, the high-resolution observations of the hyperfine transitions carried out with HIFI in red.

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