<i>SRG</i>/eROSITA discovery of a radio-faint X-ray candidate supernova remnant SRGe J003602.3+605421 = G121.1−1.9

Khabibullin, Ildar; Churazov, E.; Bykov, A. M.; Чугай, Н. Н.; Sunyaev, R.

doi:10.1093/mnras/stad818

Cited by 8 publications

(1 citation statement)

References 106 publications

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“…With their improved capabilities and low surface brightness sensitivity, the latest generation of radio telescopes, including ASKAP, MeerKAT, Murchison Widefield Array (MWA), and Low-Frequency Array (LOFAR), are expected to discover many of these missing Galactic SNRs. Indeed, several recent discoveries such as the intergalactic SNR J0624-6948 (Filipović et al 2022a) and the Galactic SNRs G181.1-9.5 (Kothes et al 2017), Hoinga (Becker et al 2021), G118.4 +37.0 (Calvera; Arias et al 2022), J1818.0-1607 (Ibrahim et al 2023), and G121.1-1.9 (Khabibullin et al 2023) confirm this expectation. These SNRs are mainly located well outside the Galactic plane, where they can preserve their typical circular SNR shape for longer time frames, in the presumably low-density environment, while also becoming lower surface brightness as compared to typical SNRs.…”

Section: Introductionmentioning

confidence: 84%

EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3

Filipović,

Dai,

Arbutina

et al. 2023

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We present the serendipitous detection of a new Galactic supernova remnant (SNR), G288.8–6.3, using data from the Australian Square Kilometre Array Pathfinder (ASKAP) Evolutionary Map of the Universe (EMU) survey. Using multifrequency analysis, we confirm this object as an evolved Galactic SNR at high Galactic latitude with low radio surface brightness and typical SNR spectral index of α = − 0.41 ± 0.12. To determine the magnetic field strength in SNR G288.8–6.3, we present the first derivation of the equipartition formulae for SNRs with spectral indices α > − 0.5. The angular size is 1.°8 × 1.°6 (107.′6 × 98.′4), and we estimate that its intrinsic size is ∼40 pc, which implies a distance of ∼1.3 kpc and a position of ∼140 pc above the Galactic plane. This is one of the largest in angular size and closest Galactic SNRs. Given its low radio surface brightness, we suggest that it is about 13,000 yr old.

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Section: Introductionmentioning

confidence: 84%

EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3

Filipović,

Dai,

Arbutina

et al. 2023

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Diprotodon on the sky. The Large Galactic Supernova Remnant (SNR) G278.94+1.35

Filipović,

Lazarević,

Araya

et al. 2024

Publ. Astron. Soc. Aust.

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We present a re-discovery of G278.94+1.35a as possibly one of the largest known Galactic supernova remnants (SNRs) – that we name Diprotodon. While previously established as a Galactic SNR, Diprotodon is visible in our new Evolutionary Map of the Universe (EMU) and GaLactic and Extragalactic All-sky MWA (GLEAM) radio continuum images at an angular size of $3{{{{.\!^\circ}}}}33\times3{{{{.\!^\circ}}}}23$ , much larger than previously measured. At the previously suggested distance of 2.7 kpc, this implies a diameter of 157 $\times$ 152 pc. This size would qualify Diprotodon as the largest known SNR and pushes our estimates of SNR sizes to the upper limits. We investigate the environment in which the SNR is located and examine various scenarios that might explain such a large and relatively bright SNR appearance. We find that Diprotodon is most likely at a much closer distance of $\sim$ 1 kpc, implying its diameter is 58 $\times$ 56 pc and it is in the radiative evolutionary phase. We also present a new Fermi-LAT data analysis that confirms the angular extent of the SNR in gamma rays. The origin of the high-energy emission remains somewhat puzzling, and the scenarios we explore reveal new puzzles, given this unexpected and unique observation of a seemingly evolved SNR having a hard GeV spectrum with no breaks. We explore both leptonic and hadronic scenarios, as well as the possibility that the high-energy emission arises from the leftover particle population of a historic pulsar wind nebula.

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Discovery of an old supernova remnant candidate through carbon monoxide line emission

Zhou,

Su,

Yang

et al. 2024

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Most old supernova remnants (SNRs) in the Milky Way have not yet been identified. Considering their high potential number and the sufficient momentum-energy transfer to the interstellar medium (ISM), they are a key part of our understanding of the overall role of SNRs in the ISM. Here, we report our discovery of an expanding molecular shell identified by CO line observations, namely It covers a known SNR, specifically G16.0$-$0.5, and is larger in size (i.e.,\ 0.56$^ over 0.20$^ Based on its spatial and kinematic structures, weak nonthermal radio-continuum emission, and derived physical properties, we suggest that it is an old SNR. At a systemic velocity of +41.3 the best estimated kinematic distance of is sim 3.2 kpc, implying its radius of about 15.6 pc. The age of is estimated to be greater than sim $ yr, and, in a dense molecular environment, it has formed dense and thin shell layers. The kinetic energy of the expanding molecular gas of is about $6.4 $ erg, accounting for approximately six percent of the initial SN explosion energy. Although old SNRs have essentially become cold and hard to detect, our discovery suggests that they can be found by searching for CO line emissions.

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SRG/eROSITA discovery of a radio-faint X-ray candidate supernova remnant SRGe J003602.3+605421 = G121.1−1.9

Cited by 8 publications

References 106 publications

EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3

EMU Detection of a Large and Low Surface Brightness Galactic SNR G288.8–6.3

Diprotodon on the sky. The Large Galactic Supernova Remnant (SNR) G278.94+1.35

Discovery of an old supernova remnant candidate through carbon monoxide line emission

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