Volume 545, September 2012
|Number of page(s)||11|
|Published online||18 September 2012|
The XMM-Newton survey of the Small Magellanic Cloud⋆,⋆⋆,⋆⋆⋆
1 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany
2 Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/SAp, CEA-Saclay, 91191 Gif-sur-Yvette, France
3 Astronomical Institute, Ruhr-University Bochum, Universitätstr. 150, 44780 Bochum, Germany
4 South African Astronomical Observatory, PO Box 9, 7935 Observatory, Cape Town, South Africa
5 School of Physics and Astronomy, University of Southampton, SO17 1BJ, UK
6 University of Maryland, Baltimore County; X-ray Astrophysics Laboratory, Mail Code 662, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
7 XMM-Newton Science Operations Centre, ESAC, ESA, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain
8 University of Western Sydney, Locked Bag 1797, Penrith South DC, NSW 1797, Australia
9 Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Straße 1, 85741 Garching, Germany
10 Physics Department, University of Crete, PO Box 2208, 710 03 Heraklion, Crete, Greece
11 INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica Milano, via E. Bassini 15, 20133 Milano, Italy
12 Laboratory for High Energy Astrophysics, Code 662, NASA/GSFC, Greenbelt, MD 20771, USA
13 Istituto Universitario di Studi Superiori di Pavia, Viale Lungo Ticino Sforza 56, 27100 Pavia, Italy
Received: 5 June 2012
Accepted: 4 July 2012
Context. Although numerous archival XMM-Newton observations existed towards the Small Magellanic Cloud (SMC) before 2009, only a fraction of the whole galaxy had been covered.
Aims. Between May 2009 and March 2010, we carried out an XMM-Newton survey of the SMC, to ensure a complete coverage of both its bar and wing. Thirty-three observations of 30 different fields with a total exposure of about one Ms filled the previously missing parts.
Methods. We systematically processed all available SMC data from the European Photon Imaging Camera. After rejecting observations with very high background, we included 53 archival and the 33 survey observations. We produced images in five different energy bands. We applied astrometric boresight corrections using secure identifications of X-ray sources and combined all the images to produce a mosaic covering the main body of the SMC.
Results. We present an overview of the XMM-Newton observations, describe their analysis, and summarise our first results, which will be presented in detail in follow-up papers. Here, we mainly focus on extended X-ray sources, such as supernova remnants (SNRs) and clusters of galaxies, that are seen in our X-ray images.
Conclusions. Our XMM-Newton survey represents the deepest complete survey of the SMC in the 0.15 − 12.0 keV X-ray band. We propose three new SNRs that have low surface brightnesses of a few 10-14 erg cm-2 s-1 arcmin-2 and large extents. In addition, several known remnants appear larger than previously measured at either X-rays or other wavelengths extending the size distribution of SMC SNRs to larger values.
Key words: Magellanic Clouds / ISM: supernova remnants / X-rays: ISM
Based on observations with XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member states and the USA (NASA).
Table 1 is available in electronic form at http://www.aanda.org
FITS images are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/545/A128
© ESO, 2012
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