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arxiv: 2604.19897 · v1 · submitted 2026-04-21 · 🌌 astro-ph.HE

Radio detection of supernova remnant G310.7-5.4 with γ-ray counterpart: Abeona SNR

Christopher Burger-Scheidlin , Brianna D. Ball , Sanja Lazarevi\'c , Roland Kothes , Robert Brose , Jonathan Mackey , Miroslav D. Filipovi\'c , Zachary J. Smeaton
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Andrew M. Hopkins Denis Leahy Mehrnoosh Tahani Jennifer L. West Tayyaba Zafar
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Pith reviewed 2026-05-10 01:20 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords supernova remnantradio shellgamma-ray emissionAbeona SNRhigh Galactic latitudeASKAP observationsFermi-LAT
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The pith

Radio observations confirm G310.7-5.4 as the supernova remnant Abeona with a gamma-ray counterpart

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper uses new ASKAP radio continuum data at 943.5 MHz to confirm the SNR candidate G310.7-5.4 as a real supernova remnant, which the authors name Abeona. The data show a faint bilateral radio shell about 30 arcminutes across with a flux density of 1.5 Jy, linear polarization in the northern part, and no infrared counterparts. The shell coincides with the GeV source 4FGL J1413.9-6705 detected by Fermi-LAT over 16.5 years. The remnant has one of the lowest radio surface brightness values recorded for any SNR and is estimated at a distance of roughly 4.9 kpc. A sympathetic reader would care because the work shows how modern wide-field surveys can verify faint, high-latitude SNR candidates and link them to their gamma-ray emission.

Core claim

We confirm the SNR candidate as a new supernova remnant, dubbed Abeona. We detect the presence of a faint, extended, bilateral radio shell of the size of around 30' diameter and ASKAP radio flux density of 1.5 Jy with no obvious infrared counterparts. The northern part of the shell shows linearly polarised radio emission, characteristic of synchrotron emission in SNRs. The physical size of the SNR is estimated to be around 42 pc, which would give a distance of around 4.9 kpc. Furthermore, the spatially coincident gamma-ray source 4FGL J1413.9-6705 shows an energy flux of 1.26 x 10^{-6} MeV cm^{-2} s^{-1} with a significance of 5.7 sigma.

What carries the argument

The faint bilateral radio shell detected at 943.5 MHz, showing linear polarization in the north and no infrared counterparts while spatially matching a GeV gamma-ray source

Load-bearing premise

That radio morphology, linear polarization, lack of infrared emission, and gamma-ray coincidence together suffice to identify the object as a supernova remnant rather than a planetary nebula or H II region

What would settle it

A measurement of zero angular expansion in the radio shell over several years or the discovery of infrared emission tightly following the radio structure would undermine the supernova remnant identification

Figures

Figures reproduced from arXiv: 2604.19897 by Andrew M. Hopkins, Brianna D. Ball, Christopher Burger-Scheidlin, Denis Leahy, Jennifer L. West, Jonathan Mackey, Mehrnoosh Tahani, Miroslav D. Filipovi\'c, Robert Brose, Roland Kothes, Sanja Lazarevi\'c, Tayyaba Zafar, Zachary J. Smeaton.

Figure 1
Figure 1. Figure 1: ASKAP 943.5 MHz total intensity image of Abeona (G310.7–5.4). The synthesised beam of the image is 15 [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Top: Polarised intensity image, overlaid with total in￾tensity contours (white). Centre: Rotation measure, overlaid with total intensity contours (black) in the range of −350 to +350 rad m−2 , masking pixels with significances below a 6σ threshold. Bottom: Same as the middle, except with a 10σ threshold cut instead of 6σ. logue source, 4FGL J1413.9–6705, subsequently referred to as J1413. Due to large-scal… view at source ↗
Figure 3
Figure 3. Figure 3: RGB intensity image of WISE infrared (IR) data at 4.6 [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Left: Significance maps of the G310.7–5.4 region as seen with Fermi–LAT with the optimised position of J1413 at l, b = 310.75◦ , −5.55◦ (blue cross) in the energy range of 100 MeV–1 TeV. The blue dashed circle indicates positional uncertainty for the new position of J1413. White circles indicate the 68 % containment radii of respective sources. Thin black contours show radio excess, while dashed black line… view at source ↗
read the original abstract

G310.7-5.4 is a supernova remnant (SNR) candidate identified as a faint shell in the second epoch Molonglo Galactic Plane Survey (MGPS-2), but this has not been followed up with multi-wavelength observations until now. It is an example of an SNR at high Galactic latitude showing spatially coinciding $\gamma$-ray emission. Here, we make the first detailed investigation of the radio emission from the G310.7-5.4 region, aiming to characterise the radio structure, polarisation measurements and the coinciding GeV emission. We used recent radio continuum observations at 943.5 MHz from the EMU and the POSSUM surveys with ASKAP, as well as 16.5 years of Fermi-LAT observations. We furthermore considered the multiwavelength context of the object by investigating observations previously conducted with other instruments, such as infrared and X-ray surveys. We confirm the SNR candidate as a new supernova remnant, dubbed Abeona. We detect the presence of a faint, extended, bilateral radio shell of the size of around 30' diameter and ASKAP radio flux density of $1.5^{+1.5}_{-0.1}$ Jy with no obvious infrared counterparts. With a radio surface brightness of about $2.4^{+2.4}_{-0.1}\times10^{-22}$ W m$^{-2}$ Hz$^{-1}$ sr$^{-1}$, this SNR is one of the faintest radio SNRs known. The northern part of the shell shows linearly polarised radio emission, characteristic of synchrotron emission in SNRs. The physical size of the SNR is estimated to be around $42^{+42}_{-21}$ pc, which would give a distance of around $4.9^{+4.9}_{-2.5}$ kpc. Furthermore, the spatially coincident $\gamma$-ray source 4FGL J1413.9-6705 shows an energy flux of $1.26\pm0.35\times 10^{-6}$ MeV cm$^{-2}$ s$^{-1}$ with a significance of 5.7 $\sigma$ between 100 MeV and 100 GeV. The SNR is also put in context with known high-latitude SNRs with $\gamma$-ray counterparts and compared with their observational properties.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 3 minor

Summary. The paper reports the confirmation of the SNR candidate G310.7-5.4 as a new supernova remnant (Abeona) based on ASKAP/EMU and POSSUM radio continuum observations at 943.5 MHz. It identifies a faint, extended bilateral radio shell ~30 arcmin in diameter with integrated flux density 1.5^{+1.5}_{-0.1} Jy, linear polarization in the northern shell indicative of synchrotron emission, no obvious infrared counterparts, and spatial coincidence with the Fermi-LAT GeV source 4FGL J1413.9-6705 at 5.7 sigma significance. Additional estimates include a radio surface brightness of ~2.4 x 10^{-22} W m^{-2} Hz^{-1} sr^{-1}, physical size ~42 pc, and distance ~4.9 kpc, with the object placed in context among other high-latitude gamma-ray SNRs.

Significance. If the identification is robust, the result adds a new faint, high-latitude SNR with a gamma-ray counterpart to the known population. Such objects are rare and useful for constraining SNR evolution, particle acceleration, and the completeness of the Galactic SNR census in low-density environments. The work also illustrates the value of wide-field, high-sensitivity surveys like ASKAP for detecting low-surface-brightness emission that may have been missed in earlier surveys.

major comments (1)
  1. The distance and physical-size estimates (abstract and §4) are obtained by assuming a typical SNR diameter of ~42 pc to convert the observed 30 arcmin angular size; the justification for this fiducial size and the propagation of its uncertainty into the reported distance (4.9^{+4.9}_{-2.5} kpc) should be stated explicitly, as the large symmetric errors suggest the assumption dominates the result.
minor comments (3)
  1. The asymmetric flux-density uncertainty (+1.5/-0.1 Jy) is unusually large; a brief description of the aperture integration, background estimation, and error budget (likely in §3) would clarify whether the measurement is limited by confusion or noise.
  2. Figure captions and text should explicitly reference the exact ASKAP frequency (943.5 MHz) and survey names when presenting the radio images and polarization maps to avoid ambiguity with other frequencies in the literature.
  3. The 5.7 sigma gamma-ray significance is quoted for 100 MeV–100 GeV; adding the test-statistic value or the precise positional offset between the radio shell centroid and 4FGL J1413.9-6705 would strengthen the association claim.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their positive assessment of the work and for the constructive comment, which we address below. We agree that greater explicitness is warranted.

read point-by-point responses

  1. Referee: The distance and physical-size estimates (abstract and §4) are obtained by assuming a typical SNR diameter of ~42 pc to convert the observed 30 arcmin angular size; the justification for this fiducial size and the propagation of its uncertainty into the reported distance (4.9^{+4.9}_{-2.5} kpc) should be stated explicitly, as the large symmetric errors suggest the assumption dominates the result.

    Authors: We agree that the manuscript should state the basis for the adopted fiducial diameter more explicitly. The value of ~42 pc was selected as representative of the typical physical diameters of known SNRs (particularly those in the Sedov phase or with similar radio surface brightness), drawing on the observed distribution in the Green (2019) catalogue and related compilations. The reported uncertainties (roughly a factor of two) are intended to encompass the broad range of SNR sizes (tens of pc) when no independent distance indicators are available; this produces the quoted distance errors. In the revised manuscript we will add a concise justification paragraph in §4, cross-reference it from the abstract, and clarify how the uncertainty is propagated from the angular size. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper reports direct observational measurements from public surveys (ASKAP EMU/POSSUM at 943.5 MHz, Fermi-LAT 16.5-year data) including radio flux (1.5^{+1.5}_{-0.1} Jy), surface brightness, linear polarization in the northern shell, absence of IR counterparts, and 5.7σ positional coincidence with 4FGL J1413.9-6705. Angular size (~30') and physical size/distance estimates (~42 pc at ~4.9 kpc) are simple geometric conversions using standard SNR assumptions without author-fitted parameters or self-referential loops. No equations reduce inputs to outputs by construction, no self-citation load-bearing uniqueness theorems are invoked, and all quantities are externally verifiable from survey data. The central confirmation as SNR Abeona rests on standard multi-wavelength diagnostics rather than any circular derivation.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard radio-astronomy interpretations of shell morphology and polarization as SNR signatures plus the assumption that spatial coincidence with a Fermi source is physically meaningful. No new free parameters or invented entities are introduced.

axioms (2)
  • domain assumption Linearly polarized radio emission from an extended shell indicates synchrotron radiation typical of supernova remnants
    Invoked when interpreting the northern shell polarization as evidence for SNR nature
  • domain assumption Absence of infrared counterparts supports an old, low-density SNR rather than other Galactic objects
    Used to rule out alternative identifications

pith-pipeline@v0.9.0 · 5803 in / 1409 out tokens · 30640 ms · 2026-05-10T01:20:20.931977+00:00 · methodology

discussion (0)

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