A complete catalogue of dusty supernova remnants in the Galactic plane

Creators: Chawner, H.; Gomez, H. L.; Matsuura, M.; Smith, M. W. L.; Papageorgiou, A.; Rho, J.; Noriega-Crespo, A.; De Looze, I.; Barlow, M. J.; Cigan, P.; Dunne, L.; Marsh, K.

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Abstract

We search for far-infrared (FIR) counterparts of known supernova remnants (SNRs) in the Galactic plane (360° in longitude and b=±1∘⁠) at 70–500 μm with Herschel. We detect dust signatures in 39 SNRs out of 190, made up of 13 core-collapse supernovae (CCSNe), including 4 Pulsar Wind Nebulae (PWNe), and 2 Type Ia SNe. A further 24 FIR detected SNRs have unknown types. We confirm the FIR detection of ejecta dust within G350.1−0.3, adding to the known sample of ∼ 10 SNRs containing ejecta dust. We discover dust features at the location of a radio core at the centre of G351.2+0.1, indicating FIR emission coincident with a possible Crab-like compact object, with dust temperature and mass of T_d = 45.8 K and M_d = 0.18 M⊙, similar to the PWN G54.1+0.3. We show that the detection rate is higher among young SNRs. We produce dust temperature maps of 11 SNRs and mass maps of those with distance estimates, finding dust at temperatures 15 ≲ T_d ≲ 40 K. If the dust is heated by shock interactions the shocked gas must be relatively cool and/or have a low density to explain the observed low grain temperatures.

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© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2020 January 10. Received 2019 November 1; in original form 2019 March 18. Published: 01 February 2020. We are grateful to Aya Bamba, and Hiroya Yamuguchi for providing X-ray data for G298.6−0.0 and G344.7−0.1 respectively, also to Ryan Lau and Matthew Hankins for providing SOFIA data for Sgr A East. We thank Felix Priestley for informative discussions on this topic. We also thank the anonymous referee for their contribution to the paper. HC, HLG, and PC acknowledge support from the European Research Council (ERC) in the form of Consolidator Grant COSMICDUST (ERC-2014-CoG-647939). MJB acknowledges support from the ERC in the form of Advanced Grant SNDUST (ERC-2015-AdG-694520). MM acknowledges support from an STFC Ernest Rutherford fellowship (ST/L003597/1). Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. IDL gratefully acknowledges the support of the Research Foundation Flanders (FWO). This research has made use of data from the Hi-GAL survey (2012hers.prop.2454M, 2011hers.prop.1899M, 2010hers.prop.1172M, 2010hers.prop.358M) and ASTROPY,7 a community-developed core PYTHON package for Astronomy (The Astropy Collaboration 2013, 2018). This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The scientific results reported in this article are based in part on data obtained from the Chandra Data Archive.

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