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Alsaberi, Rami Z E; Filipović, M D; Dai, S; Sano, H; Kothes, R; Payne, J L; Bozzetto, L M; Brose, R; Collischon, C; Crawford, E J; Haberl, F; Hill, T; Kavanagh, P J; Knies, J; Leahy, D; Macgregor, P J; Maggi, P; Maitra, C; Manojlović, P; Martín, S; Matthew, C; Ralph, N O; Rowell, G; Ruiter, A J; Sasaki, M; Seitenzahl, I R; Tokuda, K; Tothill, N F H; Urošević, D; van Loon, J Th; Velović, V; Vogt, F P A
Monthly notices of the Royal Astronomical Society, 01/2024, Letnik: 527, Številka: 1Journal Article
ABSTRACT We present new and archival Australia Telescope Compact Array and Atacama Large Millimeter/submillimeter Array data of the Small Magellanic Cloud supernova remnant 1E 0102.2–7219 at 2100, 5500, 9000, and 108 000 MHz; as well as H i data provided by the Australian Square Kilometre Array Pathfinder. The remnant shows a ring-like morphology with a mean radius of 6.2 pc. The 5500 MHz image reveals a bridge-like structure, seen for the first time in a radio image. This structure is also visible in both optical and X-ray images. In the 9000 MHz image, we detect a central feature that has a flux density of 4.3 mJy but rule out a pulsar wind nebula origin, due to the lack of significant polarization towards the central feature with an upper limit of 4 per cent. The mean fractional polarization for 1E 0102.2–7219 is 7 ± 1 and 12 ± 2 per cent for 5500 and 9000 MHz, respectively. The spectral index for the entire remnant is −0.61 ± 0.01. We estimate the line-of-sight magnetic field strength in the direction of 1E 0102.2–7219 of ∼44 µG with an equipartition field of $65\pm 5\, \mu$G. This latter model uses the minimum energy of the sum of the magnetic field and cosmic ray electrons only. We detect an H i cloud towards this remnant at the velocity range of ∼160–180 km s−1 and a cavity-like structure at the velocity of 163.7–167.6 km s−1. We do not detect CO emission towards 1E 0102.2–7219.
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