Progenitors and explosion properties of supernova remnants hosting central compact objects: I. RCW 103 associated with the peculiar source 1E 161348−5055
AffiliationUniv Arizona, Dept Astron
Keywordsstars: individual (1E 161348-5055)
ISM: supernova remnants
X-rays: individual (RCW 103, G332.4-00.4)
MetadataShow full item record
PublisherOXFORD UNIV PRESS
CitationC Braun, S Safi-Harb, C L Fryer, Progenitors and explosion properties of supernova remnants hosting central compact objects: I. RCW 103 associated with the peculiar source 1E 161348−5055, Monthly Notices of the Royal Astronomical Society, Volume 489, Issue 3, November 2019, Pages 4444–4463, https://doi.org/10.1093/mnras/stz2437
RightsCopyright © 2019 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)
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AbstractWe present a Chandra and XMM–Newton imaging and spectroscopic study of the supernova remnant (SNR) RCW 103 (G332.4−00.4) containing the central compact object 1E 161348−5055. The high-resolution Chandra X-ray images reveal enhanced emission in the south-eastern and north-western regions. Equivalent width line images of Fe L, Mg, Si, and S using XMM–Newton data were used to map the distribution of ejecta. The SNR was sectioned into 56 regions best characterized by two-component thermal models. The harder component (kT ∼ 0.6 keV) is adequately fitted by the VPSHOCK non-equilibrium ionization model with an ionization time-scale net ∼ 1011–1012 cm−3 s, and slightly enhanced abundances over solar values. The soft component (kT ∼ 0.2 keV), fitted by the APEC model, is well described by plasma in collisional ionization equilibrium with abundances consistent with solar values. Assuming a distance of 3.1 kpc and a Sedov phase of expansion into a uniform medium, we estimate an SNR age of 4.4 kyr, a swept-up mass Msw = 16f−1/2s D5/23.1 M⊙, and a low explosion energy E* = 3.7 × 1049 f−1/2s D5/23.1 erg. This energy could be an order of magnitude higher if we relax the Sedov assumption, the plasma has a low filling factor, the plasma temperature is underestimated, or if the SNR is expanding into the progenitor’s wind-blown bubble. Standard explosion models did not match the ejecta yields. By comparing the fitted abundances to the most recent core-collapse nucleosynthesis models, our best estimate yields a low-mass progenitor of around 12–13 M⊙, lower than previously reported. We discuss degeneracies in the model fitting, particularly the effect of altering the explosion energy on the progenitor mass estimate.
VersionFinal published version
SponsorsNatural Sciences and Engineering Research Council of Canada (NSERC) through the Canada Research ChairsNatural Sciences and Engineering Research Council of Canada; NSERCNatural Sciences and Engineering Research Council of Canada; Canada Graduate Scholarship; University of Manitoba's Graduate Enhancement of Tri-Council Stipends (GETS) program; Laboratory Directed Research and Development program of Los Alamos National Laboratory [20190021DR]; U.S. Department of Energy Office of ScienceUnited States Department of Energy (DOE) [DE-SC0018297]; U.S. Department of Energy Office of Advanced Scientific Computing Research via the Scientific Discovery through Advanced Computing (SciDAC4) program [DE-SC0018297]