Volume 578, June 2015
|Number of page(s)||7|
|Section||Interstellar and circumstellar matter|
|Published online||27 May 2015|
Far-infrared CO and H2O emission in intermediate-mass protostars⋆
1 Astronomical Observatory, Adam Mickiewicz University, Słoneczna 36, 60-268 Poznań, Poland
2 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
3 Kavli Institut for Astronomy and Astrophysics, Yi He Yuan Lu 5, HaiDian Qu, Peking University, 100871 Beijing, PR China
4 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
5 Observatorio Astronómico Nacional (OAN, IGN), Apdo 112, 28803 Alcalá de Henares, Spain
Received: 4 March 2015
Accepted: 13 April 2015
Context. Intermediate-mass young stellar objects (YSOs) provide a link to understanding how feedback from shocks and UV radiation scales from low- to high-mass star forming regions.
Aims. Our aim is to analyze excitation of CO and H2O in deeply embedded intermediate-mass YSOs and compare it with similar studies on low-mass and high-mass YSOs.
Methods. Herschel/PACS spectral maps are analyzed for six YSOs with bolometric luminosities of Lbol ~ 102−103L⊙. The maps cover spatial scales of ~104 AU in several CO and H2O lines located in the ~55–210 μm range.
Results. Rotational diagrams of CO show two temperature components at Trot ~ 320 K and Trot ~ 700–800 K, comparable to low- and high-mass protostars probed at similar spatial scales. The diagrams for H2O show a single component at Trot ~ 130 K, as seen in low-mass protostars, and about 100 K lower than in high-mass protostars. Since the uncertainties in Trot are on the same order as the difference between the intermediate and high-mass protostars, we cannot conclude whether the change in rotational temperature occurs at a specific luminosity or whether the change is more gradual from low- to high-mass YSOs.
Conclusions. Molecular excitation in intermediate-mass protostars is comparable to the central 103 AU of low-mass protostars and consistent within the uncertainties with the high-mass protostars probed at 3 × 103 AU scales, suggesting similar shock conditions in all those sources.
Key words: stars: protostars / ISM: jets and outflows / ISM: molecules
Appendix A is available in electronic form at http://www.aanda.org
© ESO, 2015
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