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Title: Progenitors and explosion properties of supernova remnants hosting central compact objects: I. RCW 103 associated with the peculiar source 1E 161348−5055

Abstract

Herein, we 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 $$n_et ~$$ 10 11–10 12 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 $M$ sw = 16 $$f_\mathrm{ s}^{-1/2}$$ D$$_{3.1}^{5/2}$$ M , and a low explosion energy $$E_*$$ = 3.7 × 10 49 $$f_\mathrm{ s}^{-1/2}$$ D$$_{3.1}^{5/2}$$ 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.

Authors:
ORCiD logo [1];  [1]; ORCiD logo [2]
  1. Univ. of Manitoba, Winnipeg, MB (Canada)
  2. Los Alamos National Lab. (LANL), Los Alamos, NM (United States); Univ. of Arizona, Tucson, AZ (United States); Univ. of New Mexico, Albuquerque, NM (United States); George Washington Univ., Washington, DC (United States)
Publication Date:
Research Org.:
Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Sponsoring Org.:
USDOE Laboratory Directed Research and Development (LDRD) Program; Natural Sciences and Engineering Research Council of Canada (NSERC); USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR) (SC-21). Scientific Discovery through Advanced Computing (SciDAC)
OSTI Identifier:
1599033
Alternate Identifier(s):
OSTI ID: 1563024
Report Number(s):
[LA-UR-19-24543]
[Journal ID: ISSN 0035-8711]
Grant/Contract Number:  
[89233218CNA000001; SC0018297]
Resource Type:
Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
[ Journal Volume: 489; Journal Issue: 3]; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; stars: individual (1E 161348−5055); ISM: supernova remnants; X-rays: individual (RCW 103, G332.4−00.4); X-rays: ISM

Citation Formats

Braun, C., Safi-Harb, S., and Fryer, Christopher Lee. Progenitors and explosion properties of supernova remnants hosting central compact objects: I. RCW 103 associated with the peculiar source 1E 161348−5055. United States: N. p., 2019. Web. doi:10.1093/mnras/stz2437.
Braun, C., Safi-Harb, S., & Fryer, Christopher Lee. Progenitors and explosion properties of supernova remnants hosting central compact objects: I. RCW 103 associated with the peculiar source 1E 161348−5055. United States. doi:10.1093/mnras/stz2437.
Braun, C., Safi-Harb, S., and Fryer, Christopher Lee. Fri . "Progenitors and explosion properties of supernova remnants hosting central compact objects: I. RCW 103 associated with the peculiar source 1E 161348−5055". United States. doi:10.1093/mnras/stz2437.
@article{osti_1599033,
title = {Progenitors and explosion properties of supernova remnants hosting central compact objects: I. RCW 103 associated with the peculiar source 1E 161348−5055},
author = {Braun, C. and Safi-Harb, S. and Fryer, Christopher Lee},
abstractNote = {Herein, we 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 $n_et ~$ 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 $M$sw = 16 $f_\mathrm{ s}^{-1/2}$ D$_{3.1}^{5/2}$ M⊙, and a low explosion energy $E_*$ = 3.7 × 1049 $f_\mathrm{ s}^{-1/2}$ D$_{3.1}^{5/2}$ 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.},
doi = {10.1093/mnras/stz2437},
journal = {Monthly Notices of the Royal Astronomical Society},
number = [3],
volume = [489],
place = {United States},
year = {2019},
month = {8}
}

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