EDP Sciences
Free Access
Issue
A&A
Volume 562, February 2014
Article Number A45
Number of page(s) 22
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201321954
Published online 04 February 2014

Online material

Appendix A: Details of PACS observations

Table A.1 shows the observing log of PACS observations used in this paper. The observations identifications (OBSID), observation day (OD), date of observation, total integration time, primary wavelength ranges, and pointed coordinates (RA, Dec) are listed. All spectra were obtained in pointed/chop-nod observing mode. Additional remarks are given for several sources. G327-0.6 and W33A observations were mispointed. NGC 6334-I, W3IRS5, and NGC 7538-IRS1 spectra were partly saturated and re-observed (re-obs). Two observations each of W51N-e1, G34.26, G5.89, and AFGL2591 were done using different pointing.

Table A.1

Log of PACS observations.

Appendix B: Continuum measurements

Table B.1 shows the continuum fluxes for all our sources measured using the full PACS array. The fluxes were used in the spectral energy distributions presented by van der Tak et al. (2013).

Table B.1

Full-array continuum measurements in 103 Jy.

Appendix C: Tables with fluxes and additional figures

Table C.1 shows line fluxes and 3σ upper limits of CO lines toward all our objects in units of 10-20 W cm-2. For details, see the table caption.

Figure C.1 shows blow-ups of selected spectral regions of W3 IRS5 with high-J CO, H2O, and OH lines. Figures C.2 and C.3 show blow-ups of selected CO and OH transitions towards all sources.

Table C.1

CO line fluxes in 10-20 W cm-2.

thumbnail Fig. C.1

Close-ups of several of the H2O, CO and OH lines in W3IRS5 as shown in Fig. 1. The rest wavelength of each line is indicated by dashed lines: blue for H2O, red for CO, and light blue for OH. Identifications of the undetected lines in the presented spectral regions are shown in parenthesis.

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thumbnail Fig. C.2

Close-ups of several transitions of CO lines in the PACS wavelength range toward all sources. The spectra are continuum-subtracted and shifted vertically for better visualization.

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thumbnail Fig. C.3

Normalized spectra of OH doublets for all our sources at central position. Doublets at 71 and 98 μm are excluded because of poor calibration of those spectral regions observed with PACS. OH doublet at 84.4 μm is a blend with the CO 31–30 line, whereas OH at 65.13 μm can be affected by H2O 625–514 at 65.17 μm.

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Appendix D: OH in low and intermediate mass sources

Figures D.1 and D.2 show rotational diagrams of OH for low- and intermediate-mass young stellar objects based on the fluxes presented in Wampfler et al. (2013). Only the sources with at least three detected doublets in emission (out of 4 targeted in total) are shown in diagrams. Rotational temperatures and total numbers of emitting molecules are summarized in Table D.1. For low-mass YSOs, a single component fit is usually not a good approximation (with the exception of L1527 and IRAS15398). In the intermediate-mass YSOs, on the other hand, such an approximation holds and results in very similar rotational temperatures of OH Trot ~ 35 K for all sources except NGC 7129 FIRS2.

thumbnail Fig. D.1

OH rotational diagrams (from emission lines) for low-mass young stellar objects (fluxes from Wampfler et al. 2013).

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thumbnail Fig. D.2

OH rotational diagrams (from emission lines) for intermediate-mass young stellar objects (fluxes from Wampfler et al. 2013).

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Table D.1

OH rotational excitation and number of emitting molecules based on emission lines for low- and intermediate-mass sources.


© ESO, 2014

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