Discovery of Perun (G329.9−0.5): a new, young, Galactic SNR

Smeaton ZJ, Filipović MD, Lazarević S, Alsaberi RZ, Ahmad A, Araya M, Ball BD, Bordiu C, Buemi CS, Bufano F, Dai S, Haberl F, Hopkins AM, Ingallinera A, Jarrett T, Koribalski BS, Kothes R, Kraan-Korteweg RC, Leahy D, Lundqvist P, Maitra C, Martin P, Payne JL, Rowell G, Sano H, Sasaki M, Soria R, Steyn N, Umana G, Urošević D, Velović V, Vernstrom T, Vukotić B, West J (2024)

Publication Type: Journal article

Publication year: 2024

Journal

Book Volume: 534

Pages Range: 2918-2937

Journal Issue: 3

DOI: 10.1093/mnras/stae2237

Abstract

We present the discovery of possibly the youngest Galactic supernova remnant (SNR) with associated pulsar-wind nebula (PWN), which we name Perun (G329.9−0.5). Perun was serendipitously discovered in the Australian Square Kilometre Array Pathfinder–Evolutionary Map of the Universe survey at 943 MHz, and subsequent follow-up observations were conducted with the Australia Telescope Compact Array observatory at 5500 and 9000 MHz. We combine these with additional radio observations from the MeerKAT, Molonglo Observatory Synthesis Telescope, and Murchison Widefield Array telescopes, infrared (IR) observations from the SpitzerSpace Telescope, and X-ray observations from the Chandra X-ray observatory to perform a multifrequency analysis. The radio morphology shows a small angular size shell (D = 70 arcsec) with a luminous, central PWN. We measure a total spectral index of α = −0.49 ± 0.05, which should be typical for a young, composite SNR. Crucial evidence for Perun’s SNR classification comes from the detection of linear fractional polarization at radio frequencies of ∼7 per cent–10 per cent with both radial and tangential orientations, similar to the young SNR G1.9+0.3. We use data from the Southern Galactic Plane Survey to perform an H I analysis and estimate a favoured distance range of 6–9 kpc, and thus a favoured age range of ∼70–500 yr. We find no high-energy emission in Fermi-Large Area Telescope data. We detect Perun’s outer shell in 24 μm indicating the possible presence of [O IV] and [Fe III] emission, also typical for young SNRs. Overall, these observations and analysis confirm Perun as a young, Galactic SNR with a prominent PWN.

Authors with CRIS profile

Involved external institutions

University of Western Sydney Australia (AU) National Institute for Astrophysics / Istituto Nazionale Astrofisica (INAF) Italy (IT) Max-Planck-Institut für extraterrestrische Physik (MPE) / Max Planck Institute for Extraterrestrial Physics Germany (DE) Macquarie University Australia (AU) National Research Council / Conseil national de recherches Canada Canada (CA) University of Cape Town (UCT) South Africa (ZA) University of Calgary Canada (CA) The Oskar Klein Centre Sweden (SE) Institut de Recherche en Astrophysique et Planétologie (IRAP) France (FR) University of Adelaide Australia (AU) Gifu University / 岐阜大学 Japan (JP) University of Western Australia (UWA) Australia (AU) Universidad de Costa Rica Costa Rica (CR) University of Alberta Canada (CA) University of Belgrade / Универзитет у Београду Serbia (RS) Astronomical Observatory Belgrade Serbia (RS)

How to cite

APA:

Smeaton, Z.J., Filipović, M.D., Lazarević, S., Alsaberi, R.Z., Ahmad, A., Araya, M.,... West, J. (2024). Discovery of Perun (G329.9−0.5): a new, young, Galactic SNR. Monthly Notices of the Royal Astronomical Society, 534(3), 2918-2937. https://doi.org/10.1093/mnras/stae2237

MLA:

Smeaton, Zachary J., et al. "Discovery of Perun (G329.9−0.5): a new, young, Galactic SNR." Monthly Notices of the Royal Astronomical Society 534.3 (2024): 2918-2937.

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