Volume 565, May 2014
|Number of page(s)||34|
|Section||Interstellar and circumstellar matter|
|Published online||30 April 2014|
Warm gas towards young stellar objects in Corona Australis
Herschel/PACS observations from the DIGIT key programme⋆
Centre for Star and Planet Formation, Natural History Museum of Denmark,
University of Copenhagen,
Øster Voldgade 5-7,
2 Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 København Ø, Denmark
3 The University of Texas at Austin, Department of Astronomy, 2515 Speedway, Stop C1400, Austin TX 78712-1205, USA
4 Kavli Institute for Astronomy and Astrophysics, Peking University, 100871 Beijing, PR China
5 Max Planck Institute for Extraterrestrial Physics, Postfach 1312, 85741 Garching, Germany
6 University of Vienna, Department of Astronomy, Türkenschanzstrasse 17, 1180 Vienna, Austria
Accepted: 27 November 2013
Context. The effects of external irradiation on the chemistry and physics in the protostellar envelope around low-mass young stellar objects are poorly understood. The Corona Australis star-forming region contains the R CrA dark cloud, comprising several low-mass protostellar cores irradiated by an intermediate-mass young star.
Aims. We study the effects of the irradiation coming from the young luminous Herbig Be star R CrA on the warm gas and dust in a group of low-mass young stellar objects.
Methods. Herschel/PACS far-infrared datacubes of two low-mass star-forming regions in the R CrA dark cloud are presented. The distributions of CO, OH, H2O, [C ii], [O i], and continuum emission are investigated. We have developed a deconvolution algorithm which we use to deconvolve the maps, separating the point-source emission from the extended emission. We also construct rotational diagrams of the molecular species.
Results. By deconvolution of the Herschel data, we find large-scale (several thousand AU) dust continuum and spectral line emission not associated with the point sources. Similar rotational temperatures are found for the warm CO (282 ± 4 K), hot CO (890 ± 84 K), OH (79 ± 4 K), and H2O (197 ± 7 K) emission in the point sources and the extended emission. The rotational temperatures are also similar to those found in other more isolated cores. The extended dust continuum emission is found in two ridges similar in extent and temperature to molecular millimetre emission, indicative of external heating from the Herbig Be star R CrA.
Conclusions. Our results show that nearby luminous stars do not increase the molecular excitation temperatures of the warm gas around young stellar objects (YSOs). However, the emission from photodissociation products of H2O, such as OH and O, is enhanced in the warm gas associated with these protostars and their surroundings compared to similar objects not subjected to external irradiation.
Key words: stars: formation / ISM: individual objects: R CrA / ISM: molecules / astrochemistry
Table 9 and appendices are available in electronic form at http://www.aanda.org
© ESO, 2014
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