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The MIPSGAL View of Supernova Remnants in the Galactic Plane

Pinheiro Goncalves, D. and Noriega-Crespo, A. and Paladini, R. and Martin, P. G. and Carey, S. J. (2011) The MIPSGAL View of Supernova Remnants in the Galactic Plane. Astronomical Journal, 142 (2). Art. No. 47. ISSN 0004-6256.

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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.

Item Type:Article
Related URLs:
URLURL TypeDescription
Paladini, R.0000-0002-5158-243X
Carey, S. J.0000-0002-0221-6871
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.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Associated Universities, Inc.UNSPECIFIED
International Galactic Plane SurveyUNSPECIFIED
Australian Research CouncilUNSPECIFIED
Science Foundation for PhysicsUNSPECIFIED
Subject Keywords:infrared: ISM; ISM: supernova remnants; shock waves
Issue or Number:2
Classification Code:PACS: 95.80.+p; 98.58.Hf; 98.58.Mj; 98.58.Ca; 95.85.Hp
Record Number:CaltechAUTHORS:20110808-113711037
Persistent URL:
Official Citation:The MIPSGAL View of Supernova Remnants in the Galactic Plane D. Pinheiro Gonçalves et al. 2011 The Astronomical Journal 142 47
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:24733
Deposited By: Ruth Sustaita
Deposited On:09 Aug 2011 16:03
Last Modified:03 Oct 2019 02:59

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