Free Access
Issue
A&A
Volume 559, November 2013
Article Number A84
Number of page(s) 20
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201321122
Published online 20 November 2013

Online material

Appendix A: Detection of CO transitions

In Table A.1, we list the transitions that were detected in our PACS spectra, while we show windows around the position of the CO lines for those objects where CO line emission was detected in Figs. A.1 to A.8.

Table A.1

CO Transitions detected in the PACS SED scans.

thumbnail Fig. A.1

Spectra of AB Aur, centered on the CO lines, indicated in red. The OH line at 84.42 μm blends with the CO J = 31 → 30 line. In blue, we indicate the positions of other lines (CH+ at 90 μm and [O i] at 145 μm; rest are OH doublets).

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thumbnail Fig. A.2

Spectra of HD 36112, centered on the CO lines, indicated in red. The OH line at 84.42 μm blends with the CO J = 31 → 30 line. In blue, we indicate the positions of other lines (CH+ at 90 μm and [O i] at 145 μm; rest are OH doublets).

Open with DEXTER

thumbnail Fig. A.3

Spectra of HD 97048, centered on the CO lines, indicated in red. The OH line at 84.42 μm blends with the CO J = 31 → 30 line. In blue, we indicate the positions of other lines (CH+ at 90 μm and [O i] at 145 μm; rest are OH doublets).

Open with DEXTER

thumbnail Fig. A.4

Spectra of IRS 48, centered on the CO lines, indicated in red. The OH line at 84.42 μm blends with the CO J = 31 → 30 line. In blue, we indicate the positions of other lines (CH+ at 90 μm and [O i] at 145 μm; rest are OH doublets).

Open with DEXTER

thumbnail Fig. A.5

Spectra of AS 205, centered on the CO lines, indicated in red. The OH line at 84.42 μm blends with the CO J = 31 → 30 line. In blue, we indicate the positions of other lines (CH+ at 90 μm and [O i] at 145 μm; rest are OH doublets).

Open with DEXTER

thumbnail Fig. A.6

Spectra of S CrA, centered on the CO lines, indicated in red. The OH line at 84.42 μm blends with the CO J = 31 → 30 line. In blue, we indicate the positions of other lines (CH+ at 90 μm and [O i] at 145 μm; rest are OH doublets).

Open with DEXTER

thumbnail Fig. A.7

Spectra of DG Tau, centered on the CO lines, indicated in red. The OH line at 84.42 μm blends with the CO J = 31 → 30 line. In blue, we indicate the positions of other lines (CH+ at 90 μm and [O i] at 145 μm; rest are OH doublets).

Open with DEXTER

thumbnail Fig. A.8

Spectra of RU Lup, centered on the CO lines, indicated in red. In blue, we indicate the position of OH lines.

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Appendix B: Upper limits

In Tables B.1 and B.2, we give the upper limits at a few key transitions (J36 → 35, 29 → 28, 23 → 22, 18 → 17, and 15 → 14) for those sources where not a single CO emission line was detected.

Table B.1

CO upper limits at selected wavelengths for the sources with full SEDs scans (50–200 μm) in W/m2 × 10-18.

Table B.2

CO upper limits for the sources with the forsterite scans (60–71 μm + 120–143 μm) in W/m2 × 10-18.


© ESO, 2013

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