Volume 518, July-August 2010
Herschel: the first science highlights
|Number of page(s)||5|
|Published online||16 July 2010|
Letter to the Editor
Department of Physics and Astronomy, University of Toledo, 2801 West Bancroft Street, Toledo, OH 43606, USA e-mail: email@example.com
2 NHSC/IPAC/Caltech, 770 South Wilson Avenue, Pasadena, CA 91125, USA
3 Department of Astronomy, University of Michigan, 830 Dennison Building, 500 Church Street, Ann Arbor, MI 48109, USA
4 Instituto de Astrofisica de Andalucia, CSIC, Camino Bajo de Huetor 50, 18008, Granada, Spain
5 National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA
6 ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
7 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
8 Department of Astronomy and Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
9 Department of Physics and Astronomy, University of Victoria, PO Box 355, STN CSC, Victoria BC, V8W 3P6, Canada
10 National Research Council Canada, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria BC, V9E 2E7, Canada
11 Fellow; Jet Propulsion Laboratory, Caltech, Mail Stop 264 767, 4800 Oak Grove Drive, Pasadena, CA 91109, USA
12 Department of Physics and Astronomy, University of Rochester, Rochester, NY 14627, USA
13 Laboratoire d'Astrophysique de Grenoble, Université Joseph Fourier, CNRS, UMR 571, BP 53, 38041 Grenoble, France
14 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
15 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
16 Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USA
17 Division of Geological and Planetary Sciences 150-21, California Institute of Technology, Pasadena, CA 91125, USA
Accepted: 11 May 2010
We present 70 and 160 μm Herschel science demonstration images of a field in the Orion A molecular cloud that contains the prototypical Herbig-Haro objects HH 1 and 2, obtained with the Photodetector Array Camera and Spectrometer (PACS). These observations demonstrate Herschel's unprecedented ability to study the rich population of protostars in the Orion molecular clouds at the wavelengths where they emit most of their luminosity. The four protostars previously identified by Spitzer 3.6–40 μm imaging and spectroscopy are detected in the 70 μm band, and three are clearly detected at 160 μm. We measure photometry of the protostars in the PACS bands and assemble their spectral energy distributions (SEDs) from 1 to 870 μm with these data, Spitzer spectra and photometry, 2MASS data, and APEX sub-mm data. The SEDs are fit to models generated with radiative transfer codes. From these fits we can constrain the fundamental properties of the protostars. We find luminosities in the range 12–84 and envelope densities spanning over two orders of magnitude. This implies that the four protostars have a wide range of envelope infall rates and evolutionary states: two have dense, infalling envelopes, while the other two have only residual envelopes. We also show the highly irregular and filamentary structure of the cold dust and gas surrounding the protostars as traced at 160 μm.
Key words: stars: formation / stars: protostars / circumstellar matter / infrared: ISM / infrared: stars
Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This work includes data acquired with the Atacama Pathfinder Experiment (APEX; E-082.F-9807, E-284.C-5015). APEX is a collaboration between the Max-Planck-Institut für Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory.
Figures 2 and 3 are only available in electronic format at http://www.aanda.org
© ESO, 2010
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