Volume 594, October 2016
|Number of page(s)||25|
|Section||Catalogs and data|
|Published online||13 October 2016|
Herschel-PACS observations of far-IR lines in young stellar objects
1 European Space Astronomy Centre (ESA), PO Box 78, 28691 Villanueva de la Cañada, Spain
2 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands
3 Dep. de Física Teórica, Fac. de Ciencias, UAM Campus Cantoblanco, 28049 Madrid, Spain
4 Depto. Astrofísica, Centro de Astrobiología (CAB, INTA–CSIC), PO Box 78, ESAC Campus, 28691 Villanueva de la Cañada, Madrid, Spain
Received: 25 November 2015
Accepted: 28 July 2016
Context. Gas plays a major role in the dynamical evolution of young stellar objects (YSOs). Its interaction with the dust is the key to our understanding planet formation later on in the protoplanetary disc stage. Studying the gas content is therefore a crucial step towards understanding YSO and planet formation. Such a study can be made through spectroscopic observations of emission lines in the far-infrared, where some of the most important gas coolants emit, such as the [OI] transition at 63.18 μm.
Aims. We provide a compilation of observations of far-IR lines in 362 YSOs covering all evolutionary stages, from Class 0 to Class III with debris discs. In the present paper we focus on [OI] and o-H2O emission at 63 μm.
Methods. We retrieved all the available Herschel-PACS spectroscopic observations at 63 μm that used the dominant observing mode, the chop-nod technique. We provide measurements of line fluxes for the [OI] and o-H2O808 → 717 transitions at 63 μm computed using different methods. Taking advantage of the PACS IFU, we checked for spatially extended emission and also studied multiple dynamical components in line emission.
Results. The final compilation consists of line and continuum fluxes at 63 μm for a total of 362 young stellar objects (YSOs). We detect [OI] line emission at 63 μm in 194 sources out of 362, and line absorption in another five sources. o-H2O was detected in 42 sources. We find evidence of extended [OI] emission in 77 sources, and detect 3σ residual emission in 71 of them. The number of sources showing extended emission decays from Class 0 to Class II. We also searched for different components contributing to the line emission, and found evidence for multiple components in 30 sources. We explored correlations between line emission and continuum emission and found a clear correlation between WISE fluxes from 4.6 to 22 μm and [OI] line emission. We conclude that the observed emission is typically a combination of disc, envelope and jet emission.
Key words: astrochemistry / circumstellar matter / stars: evolution / stars: protostars
The catalogue of observations and fluxes (Tables B.1–B.3) is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/594/A59
© ESO, 2016
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