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A catalogue of Galactic supernova remnants in the far-infrared: revealing ejecta dust in pulsar wind nebulae

Chawner, H., Marsh, K. ORCID:, Matsuura, M. ORCID:, Gomez, H. L. ORCID:, Cigan, P., De Looze, I., Barlow, M. J., Dunne, L. ORCID:, Noriega-Crespo, A. and Rho, J. 2019. A catalogue of Galactic supernova remnants in the far-infrared: revealing ejecta dust in pulsar wind nebulae. Monthly Notices of the Royal Astronomical Society 483 (1) , pp. 70-118. 10.1093/mnras/sty2942

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We search for far-infrared (FIR) counterparts of known supernova remnants (SNRs) in the Galactic plane (10° < ∣l∣ < 60°) at 70 – 500 μm using the Herschel Infrared Galactic Plane Survey (Hi-GAL). Of 71 sources studied, we find that 29 (41 %) SNRs have a clear FIR detection of dust emission associated with the SNR. Dust from 8 of these is in the central region, and 4 indicate pulsar wind nebulae (PWNe) heated ejecta dust. A further 23 have dust emission in the outer shell structures which is potentially related to swept up material. Many Galactic SNe have dust signatures but we are biased towards detecting ejecta dust in young remnants and those with a heating source (shock or PWN). We estimate the dust temperature and mass contained within three PWNe, G11.2−0.3, G21.5−0.9, and G29.7−0.3 using modified blackbody fits. To more rigorously analyse the dust properties at various temperatures and dust emissivity index β, we use point process mapping (PPMAP). We find significant quantities of cool dust (at 20-40 K) with dust masses of Md = 0.34 ± 0.14 M⊙, Md = 0.29 ± 0.08 M⊙, and Md = 0.51 ± 0.13 M⊙ for G11.2−0.3, G21.5−0.9, and G29.7−0.3 respectively. We derive the dust emissivity index for the PWN ejecta dust in G21.5−0.3 to be β = 1.4 ± 0.5 compared to dust in the surrounding medium where β = 1.8 ± 0.1.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Advanced Research Computing @ Cardiff (ARCCA)
Physics and Astronomy
Publisher: Oxford University Press
ISSN: 0035-8711
Date of First Compliant Deposit: 7 November 2018
Date of Acceptance: 26 October 2018
Last Modified: 04 Dec 2023 13:43

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