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

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 $\alpha = -0.49\pm 0.05$, 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 $\sim$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 $\sim$70–500 yr. We find no high-energy emission in Fermi-Large Area Telescope data. We detect Perun’s outer shell in 24 $\mu$m 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.

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Journal
Monthly Notices of the Royal Astronomical Society
Published
2024-09-30
DOI
https://doi.org/10.1093/mnras/stae2237
Citations
4
Primary Topic
Astronomical Observations and Instrumentation
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article
Field-Weighted Citation Impact
1.50

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article

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

B. Ball, Miguel Araya, Sanja Lazarević, Gavin Rowell et al.
4 citations
Monthly Notices of the Royal Astronomical Society
Astronomical Observations and Instrumentation
1.50
article

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

B. Ball, Miguel Araya, Sanja Lazarević, Gavin Rowell, F. Bufano, Andrew Hopkins, Miroslav D Filipović, Roberto Soria, Chandreyee Maitra, Hidetoshi Sano, J. L. Payne, R. Z. E. Alsaberi, Adeel Ahmad, C. S. Buemi, R. C. Kraan‐Korteweg, Peter Lundqvist, R. Kothes, Jennifer West, Tessa Vernstrom, Branislav Vukotić, D. A. Leahy, Velibor Velović, M. Sasaki, Cristóbal Bordiú, A. Ingallinera, Shi Dai, F. Haberl, T. H. Jarrett, G. Umana, D. Urošević, B. Koribalski, Nadia Steyn, Zachary J. Smeaton, Pierrick Martin
article en
4 citations

Abstract

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 $\alpha = -0.49\pm 0.05$, 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 $\sim$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 $\sim$70–500 yr. We find no high-energy emission in Fermi-Large Area Telescope data. We detect Perun’s outer shell in 24 $\mu$m 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.

Monthly Notices of the Royal Astronomical SocietyVol. 534(3)
Herzberg Institute of Astrophysics (CA), Commonwealth Scientific and Industrial Research Organisation (AU), Centre National de la Recherche Scientifique (FR), The University of Sydney (AU), Australia Telescope National Facility (AU), University of Alberta (CA), University of Cape Town (ZA), Stockholm University (SE), University of Calgary (CA), The University of Western Australia (AU), Université Fédérale de Toulouse Midi-Pyrénées (FR), Friedrich-Alexander-Universität Erlangen-Nürnberg (DE), Universidad de Costa Rica (CR), University of Belgrade (RS), Max Planck Institute for Extraterrestrial Physics (DE), Osservatorio Astrofisico di Torino (IT), Osservatorio Astrofisico di Catania (IT), AlbaNova (SE), Astronomical Observatory (RS), International Centre for Radio Astronomy Research (AU), Gifu University (JP), The University of Adelaide (AU), Macquarie University (AU)
Science and Industry Endowment Fund, Australian Government, Government of Western Australia
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Astronomical Observations and Instrumentation
1.50
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