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Suzaku study of the centrally brightened supernova remnant G272.2−3.2

Authors

  • A. Sezer,

    Corresponding author
    1. TÜBİTAK Space Technologies Research Institute, ODTU Campus, Ankara 06531, Turkey
    2. Bog̃aziçi University, Faculty of Art and Sciences, Department of Physics, Istanbul 34342, Turkey
      E-mail: aytap.sezer@uzay.tubitak.gov.tr (AS); gok@akdeniz.edu.tr (FG)
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  • F. Gök

    Corresponding author
    1. Akdeniz University, Faculty of Sciences, Department of Physics, Antalya 07058, Turkey
      E-mail: aytap.sezer@uzay.tubitak.gov.tr (AS); gok@akdeniz.edu.tr (FG)
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E-mail: aytap.sezer@uzay.tubitak.gov.tr (AS); gok@akdeniz.edu.tr (FG)

ABSTRACT

In this paper, we present the results from a Suzaku observation of the Galactic supernova remnant G272.2−3.2. The spectra of G272.2−3.2 are well fitted by a single-temperature variable abundance non-equilibrium ionization (VNEI) model with an electron temperature kTe∼ 0.77 keV, an ionization time-scale τ∼ 6.5 × 1010 cm−3 s and an absorbing column density NH∼ 1.1 × 1022 cm−2. We have detected enhanced abundances of Si, S, Ca, Fe and Ni in the centre region, indicating that the X-ray emission has an ejecta origin. We estimate that the electron density is ne∼ 0.48f−1/2 cm−3, the age is ∼4300f1/2 yr and the X-ray total mass is Mx= 475f1/2 M by taking the distance to be d= 10 kpc. To understand the origin of the centrally peaked X-ray emission of the remnant, we have studied the radial variations of the electron temperature and surface brightness. The relative abundances in the centre region suggest that G272.2−3.2 is the result of a Type Ia supernova explosion.

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