The MIPSGAL View of Supernova Remnants in the Galactic Plane

Creators: Pinheiro Goncalves, D.; Noriega-Crespo, A.; Paladini, R.; Martin, P. G.; Carey, S. J.

Abstract

We report the detection of Galactic supernova remnants (SNRs) in the mid-infrared (at 24 and 70 μm), in the coordinate ranges 10° < l < 65° and 285° < l < 350°, |b| < 1°, using MIPS aboard the Spitzer Space Telescope. We search for infrared counterparts to SNRs in Green's catalog and identify 39 out of 121, i.e., a detection rate of about 32%. Such a relatively low detection fraction is mainly due to confusion with nearby foreground/background sources and diffuse emission. The SNRs in our sample show a linear trend in [F_8/F_(24)] versus [F_(70)/F_(24)]. We compare their infrared fluxes with their corresponding radio flux at 1.4 GHz and find that most remnants have a ratio of 70 μm to 1.4 GHz which is similar to those found in previous studies of SNRs (with the exception of a few that have ratios closer to those of H II regions). Furthermore, we retrieve a slope close to unity when correlating infrared (24 and 70 μm) with 1.4 GHz emission. Our survey is more successful in detecting remnants with bright X-ray emission, which we find is well correlated with the 24 μm morphology. Moreover, by comparing the power emitted in the X-ray, infrared, and radio, we conclude that the energy released in the infrared is comparable to the cooling in the X-ray range.

Additional Information

© 2011 The American Astronomical Society. Received 2010 August 3; accepted 2011 April 4; published 2011 July 1. This work was based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory (JPL), California Institute of Technology under a contract with NASA. Support for this work was provided by NASA in part through an award issued by JPL/Caltech and by the Natural Sciences and Engineering Research Council of Canada. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research is supported as part of the International Galactic Plane Survey through a Collaborative Research Opportunities grant from the Natural Sciences and Engineering Research Council of Canada. MOST is operated by the University of Sydney with support from the Australian Research Council and the Science Foundation for Physics within the University of Sydney. This paper benefited from VLA archival data from the Multi-Array Galactic Plane Imaging Survey (MAGPIS) as well as Chandra archival data which were obtained in the online Chandra Supernova Remnant Catalog and aremaintained by Fred Seward (SAO). The authors thank Crystal Brogan for the 20 and 90 cm high-resolution VLA images of the SNR G39.2−0.3 and Dae-SikMoon and Luís Be¸ca for useful discussions. Finally, we acknowledge the referee for valuable comments and corrections that improved this manuscript.

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