High-resolution X-ray spectroscopy of the supernova remnant N132D

Una Hwang, John P. Hughes, Claude R. Canizares, Thomas H. Markert

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28 Scopus citations

Abstract

We present a joint nonequilibrium ionization analysis of spectral data from the Einstein Observatory of the supernova remnant N132D in the Large Magellanic Cloud. We use high spectral resolution data from the Focal Plane Crystal Spectrometer (FPCS) and the Solid State Spectrometer (SSS), and lower spectral resolution data from the Imaging Proportional Counter (IPC) and Monitor Proportional Counter (MPC). Our updated analysis uses new calibrations for the FPCS and SSS efficiencies and a single-temperature, single-ionization time-scale model for the plasma. The FPCS detected individual emission lines of O VII, O VIII, Ne IX, Ne X, Fe XVII, and possibly Fe XX. Measured line widths for the oxygen lines suggest Doppler broadening that is roughly consistent with optically measured expansion velocities of 2250 kms-1. Constraints on temperature and ionization age from measured FPCS line flux ratios are consistent with results of spectral fits to the SSS and IPC data, which give a temperature of 8.4 (+0.8; -0.6) × 106 K and an ionization age of 6.1 (+5.0; -2.6) × 103 cm-3 yr. At the SSS/IPC temperature, FPCS flux ratios constrain the O/Fe abundance to be at least 1.9 times its solar value and the O/Ne abundance to be 0.2-1.0 times its solar value. The SSS/IPC fits provide constraints of 1.0-4.0 times solar for O/Fe and 0.5-1.5 times solar for O/Ne which are consistent with the FPCS results. We are puzzled to find that the SSS/IPC fits indicate abundances of oxygen and other heavy elements relative to the light elements that are below both their solar values and their mean values for the LMC. We therefore compare abundance ratios to calculations for the composition of ejecta from Type II supernovae including a contribution from swept-up interstellar material with elemental abundances appropriate for the LMC. Models for remnants with progenitor masses of 20 and 25 M are completely consistent with the data, while remnants with progenitor masses of 13 and 15 M can be made consistent if the progenitors are required to eject a large fraction of their iron cores.

Original languageEnglish (US)
Pages (from-to)219-229
Number of pages11
JournalAstrophysical Journal
Volume414
Issue number1
DOIs
StatePublished - Sep 1 1993

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • ISM: individual (LMC N132D)
  • Magellanic Clouds
  • Supernova remnants
  • X-rays: interstellar

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