EDP Sciences
Free Access
Issue
A&A
Volume 578, June 2015
Article Number A20
Number of page(s) 7
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201526021
Published online 27 May 2015

Online material

Appendix A: Supplementary material

Table A.1 shows the observing log of PACS observations including observations identification numbers (OBSID), observation day (OD), date of observation, total integration time, and pointed coordinates (RA, Dec). Table A.2 shows molecular data and observed lines fluxes and upper limits for all sources that are analyzed in the paper. Figure A.1 shows selected spectral regions to illustrate the quality of the data. Figure A.2 illustrates the patterns of continuum emission at 145 μm and the CO 18–17 line emission at 144 μm toward all the sources.

Table A.1

Log of PACS observations.

Table A.2

Molecular dataa and observed line fluxes.

thumbnail Fig. A.1

Spectral scans covering selected H2O, CO, and OH lines in the intermediate-mass protostars from the WISH program. The rest wavelength of each line is indicated by dashed lines: blue for H2O, red for CO, and light blue for OH.

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thumbnail Fig. A.2

PACS spectral maps in the CO 18-17 line at 144 μm and the continuum emission at 145 μm in orange contours corresponding to 30%, 50%, 70%, and 90% of the peak value written in the bottom left corner of each map. Wavelengths in microns are translated to the velocity scale on the X-axis using laboratory wavelengths (see Table A.2) of the species and cover the range from –600 to 600 km s-1. The Y-axis shows fluxes in Jy normalized to the spaxel with the brightest line on the map in a range from –0.2 to 1.2.

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© ESO, 2015

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