2013AJ....146...62M
The HERSCHEL Inventory of The Agents of Galaxy Evolution in the Magellanic Clouds, a Herschel Open Time Key Program
Meixner, M. ( Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ; Department of Physics and Astronomy, The Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA; ); Panuzzo, P. ( CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France ; CNRS, Observatoire de Paris-Lab. GEPI, Bat. 11, 5, Place Jules Janssen, F-92195 Meudon Cedex, France ); Roman-Duval, J. ( Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ); Engelbracht, C. ( Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA ; Raytheon Company, 1151 East Hermans Road, Tucson, AZ 85756, USA ); Babler, B. ( Department of Astronomy, 475 North Charter Street, University of Wisconsin, Madison, WI 53706, USA ); Seale, J. ( Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ); Hony, S. ( CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France ); Montiel, E. ( Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA ; Department of Physics and Astronomy, Louisiana State University, 233-A Nicholson Hall, Tower Drive, Baton Rouge, LA 70803-4001, USA ); Sauvage, M. ( CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France ); Gordon, K. ( Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ); Misselt, K. ( Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA ); Okumura, K. ( CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France ); Chanial, P. ( CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France ); Beck, T. ( Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ); Bernard, J. -P. ( CNRS, IRAP, 9 Av. Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France ; Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse Cedex 4, France ); Bolatto, A. ( Department of Astronomy, Laboratory for Millimeter-Wave Astronomy, University of Maryland, College Park, MD 20742-2421, USA ); Bot, C. ( Université de Strasbourg, Observatoire Astronomique de Strasbourg, 11, Rue de l'Universite, F-67000 Strasbourg, France ; CNRS, Observatoire Astronomique de Strasbourg, UMR7550, F-67000 Strasbourg, France ); Boyer, M. L. ( Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; Observational Cosmology Laboratory, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA ; Oak Ridge Associated Universities (ORAU), Oak Ridge, TN 37831, USA ); Carlson, L. R. ( Sterrewacht Leiden, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands ); Clayton, G. C. ( Department of Physics and Astronomy, Louisiana State University, 233-A Nicholson Hall, Tower Drive, Baton Rouge, LA 70803-4001, USA ); Chen, C. -H. R. ( Max-Planck-Institut für Radioastronomie Auf dem Hügel 69, D-53121 Bonn, Germany ); Cormier, D. ( CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France ); Fukui, Y. ( Department of Astrophysics, Nagoya University, Chikusa-ku, Nagoya 464-8602, Japan ); Galametz, M. ( Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK ); Galliano, F. ( CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France ); Hora, J. L. ( Center for Astrophysics, 60 Garden Street, MS 67, Harvard University, Cambridge, MA 02138, USA ); Hughes, A. ( Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ); Indebetouw, R. ( Department of Astronomy, University of Virginia, and National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA ); Israel, F. P. ( Sterrewacht Leiden, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands ); Kawamura, A. ( National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan ); Kemper, F. ( Academia Sinica, Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan ); Kim, S. ( Department of Astronomy and Space Science, Sejong University, 98 Gunja-dong, Gwangjin-gu, 143-747 Seoul, Korea ); Kwon, E. ( Department of Astronomy and Space Science, Sejong University, 98 Gunja-dong, Gwangjin-gu, 143-747 Seoul, Korea ); Lebouteiller, V. ( CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France ); Li, A. ( Department of Physics and Astronomy, 314 Physics Building, University of Missouri, Columbia, MO 65211, USA ); Long, K. S. ( Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ); Madden, S. C. ( CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, F-91191 Gif-sur-Yvette, France ); Matsuura, M. ( Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK ); Muller, E. ( National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo 181-8588, Japan ); Oliveira, J. M. ( School of Physical and Geographical Sciences, Lennard-Jones Laboratories, Keele University, Staffordshire ST5 5BG, UK ); Onishi, T. ( Department of Physical Science, Osaka Prefecture University, Gakuen 1-1, Sakai, Osaka 599-8531, Japan ); Otsuka, M. ( Academia Sinica, Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan ); Paradis, D. ( CNRS, IRAP, 9 Av. Colonel Roche, BP 44346, F-31028 Toulouse Cedex 4, France ; Université de Toulouse, UPS-OMP, IRAP, F-31028 Toulouse Cedex 4, France ); Poglitsch, A. ( Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany ); Reach, W. T. ( Stratospheric Observatory for Infrared Astronomy, Universities Space Research Association, Mail Stop 232-11, Moffett Field, CA 94035, USA ); Robitaille, T. P. ( Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ); Rubio, M. ( Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile ); Sargent, B. ( Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; Center for Imaging Science and Laboratory for Multiwavelength Astrophysics, Rochester Institute of Technology, 54 Lomb Memorial Drive, Rochester, NY 14623, USA ); Sewiło, M. ( Department of Physics and Astronomy, The Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA ); Skibba, R. ( Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA ); Smith, L. J. ( Space Telescope Science Institute and European Space Agency, 3700 San Martin Drive, Baltimore, MD 21218, USA ); Srinivasan, S. ( Academia Sinica, Institute of Astronomy and Astrophysics, P.O. Box 23-141, Taipei 10617, Taiwan; UPMC-CNRS UMR7095, Institute d'Astrophysique de Paris, F-75014 Paris, France ); Tielens, A. G. G. M. ( Sterrewacht Leiden, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands ); van Loon, J. Th. ( School of Physical and Geographical Sciences, Lennard-Jones Laboratories, Keele University, Staffordshire ST5 5BG, UK ); Whitney, B. ( Department of Astronomy, 475 North Charter Street, University of Wisconsin, Madison, WI 53706, USA ) and 45 coauthors show affiliations
The Astronomical Journal, Volume 146, Issue 3, article id. 62, 35 pp. (2013).
Published in Sep 2013
We present an overview of the HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) in the Magellanic Clouds project, which is a Herschel Space Observatory open time key program. We mapped the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) at 100, 160, 250, 350, and 500 μm with the Spectral and Photometric Imaging Receiver (SPIRE) and Photodetector Array Camera and Spectrometer (PACS) instruments on board Herschel using the SPIRE/PACS parallel mode. The overriding science goal of HERITAGE is to study the life cycle of matter as traced by dust in the LMC and SMC. The far-infrared and submillimeter emission is an effective tracer of the interstellar medium (ISM) dust, the most deeply embedded young stellar objects (YSOs), and the dust ejected by the most massive stars. We describe in detail the data processing, particularly for the PACS data, which required some custom steps because of the large angular extent of a single observational unit and overall the large amount of data to be processed as an ensemble. We report total global fluxes for the LMC and SMC and demonstrate their agreement with measurements by prior missions. The HERITAGE maps of the LMC and SMC are dominated by the ISM dust emission and bear most resemblance to the tracers of ISM gas rather than the stellar content of the galaxies. We describe the point source extraction processing and the criteria used to establish a catalog for each waveband for the HERITAGE program. The 250 μm band is the most sensitive and the source catalogs for this band have ~25,000 objects for the LMC and ~5500 objects for the SMC. These data enable studies of ISM dust properties, submillimeter excess dust emission, dust-to-gas ratio, Class 0 YSO candidates, dusty massive evolved stars, supernova remnants (including SN1987A), H II regions, and dust evolution in the LMC and SMC. All images and catalogs are delivered to the Herschel Science Center as part of the community support aspects of the project. These HERITAGE images and catalogs provide an excellent basis for future research and follow up with other facilities.
Keywords:
Free Keywords: Magellanic Clouds; catalogs; dust; extinction; infrared: galaxies; submillimeter: general; surveys
Astronomy: Magellanic Clouds; catalogs; dust; extinction; infrared: galaxies; submillimeter: general; surveys
Feedback