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


  • 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
    Search for more papers by this author
  • F. Gök

    Corresponding author
    1. Akdeniz University, Faculty of Sciences, Department of Physics, Antalya 07058, Turkey
    Search for more papers by this author

E-mail: (AS); (FG)


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.