Volume 551, March 2013
|Number of page(s)||35|
|Section||Interstellar and circumstellar matter|
|Published online||01 March 2013|
The Earliest Phases of Star Formation (EPoS): a Herschel key project
Max-Planck-Institut für Astronomie (MPIA), Königstuhl 17, 69117
2 Universität zu Köln, Zülpicher Strasse 77, 50937 Köln, Germany
3 ESA/ESTEC, Keplerlaan 1, Postbus 299, 2200 AG Noordwijk, The Netherlands
4 Laboratoire AIM Paris-Saclay, Service d’Astrophysique, CEA/IRFU – CNRS/INSU – Université Paris Diderot, Orme des Merisiers Bat. 709, 91191 Gif-sur-Yvette Cedex, France
5 Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany
6 SRON Netherlands Institute for Space Research, PO Box 800, 9700 AV Groningen, The Netherlands
7 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands
8 Steward Observatory, 933 North Cherry Avenue, Tucson, AZ 85721, USA
9 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany
10 Institut de Planétologie et d’Astrophysique de Grenoble, Université de Grenoble, BP 53, 38041 Grenoble Cedex 9, France
Accepted: 11 December 2012
Context. The temperature and density structure of molecular cloud cores are the most important physical quantities that determine the course of the protostellar collapse and the properties of the stars they form. Nevertheless, density profiles often rely either on the simplifying assumption of isothermality or on observationally poorly constrained model temperature profiles. The instruments of the Herschel satellite provide us for the first time with both the spectral coverage and the spatial resolution that is needed to directly measure the dust temperature structure of nearby molecular cloud cores.
Aims. With the aim of better constraining the initial physical conditions in molecular cloud cores at the onset of protostellar collapse, in particular of measuring their temperature structure, we initiated the guaranteed time key project (GTKP) “The Earliest Phases of Star Formation” (EPoS) with the Herschel satellite. This paper gives an overview of the low-mass sources in the EPoS project, the Herschel and complementary ground-based observations, our analysis method, and the initial results of the survey.
Methods. We study the thermal dust emission of 12 previously well-characterized, isolated, nearby globules using FIR and submm continuum maps at up to eight wavelengths between 100 μm and 1.2 mm. Our sample contains both globules with starless cores and embedded protostars at different early evolutionary stages. The dust emission maps are used to extract spatially resolved SEDs, which are then fit independently with modified blackbody curves to obtain line-of-sight-averaged dust temperature and column density maps.
Results. We find that the thermal structure of all globules (mean mass 7 M⊙) is dominated by external heating from the interstellar radiation field and moderate shielding by thin extended halos. All globules have warm outer envelopes (14–20 K) and colder dense interiors (8–12 K) with column densities of a few 1022 cm-2. The protostars embedded in some of the globules raise the local temperature of the dense cores only within radii out to about 5000 AU, but do not significantly affect the overall thermal balance of the globules. Five out of the six starless cores in the sample are gravitationally bound and approximately thermally stabilized. The starless core in CB 244 is found to be supercritical and is speculated to be on the verge of collapse. For the first time, we can now also include externally heated starless cores in the Lsmm/Lbol vs. Tbol diagram and find that Tbol < 25 K seems to be a robust criterion to distinguish starless from protostellar cores, including those that only have an embedded very low-luminosity object.
Key words: stars: formation / stars: low-mass / stars: protostars / ISM: clouds / dust, extinction / infrared: ISM
Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
Partially based on observations carried out with the IRAM 30 m Telescope, with the Atacama Pathfinder Experiment (APEX), and with the James Clerk Maxwell Telescope (JCMT). IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). APEX is a collaboration between Max Planck Institut für Radioastronomie (MPIfR), Onsala Space Observatory (OSO), and the European Southern Observatory (ESO). The JCMT is operated by the Joint Astronomy Centre on behalf of the Particle Physics and Astronomy Research Council of the United Kingdom, the Netherlands Association for Scientific Research, and the National Research Council of Canada.
Appendices A, B and C are available in electronic form at http://www.aanda.org
© ESO, 2013
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.