arxiv: 2605.00720 · v1 · submitted 2026-05-01 · 🌌 astro-ph.HE

Recognition: unknown

A bright wideband radio burst from the isolated neutron star 2XMM J104608.7-594306

J. Tian , K. M. Rajwade , I. Pastor-Marazuela , B. W. Stappers , M. Caleb , K. Shaji , S. Singh , E. D. Barr

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M. Kramer

Authors on Pith no claims yet

Pith reviewed 2026-05-09 18:42 UTC · model grok-4.3

classification 🌌 astro-ph.HE

keywords radio burstsisolated neutron starspolarizationspectral indexmagnetarswideband emissionX-ray dim isolated neutron stars

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The pith

An isolated neutron star previously considered radio-quiet has produced a second bright, wideband radio burst with complex polarization.

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

The paper reports the detection of a second coherent radio burst from the thermally emitting neutron star 2XMM J104608.7−594306 using the Murriyang Ultra-Wideband Low receiver. The burst displays multiple components, spans frequencies from 704 to 4032 MHz, shows a steep spectral index, and reaches linear and circular polarization fractions of 54% and 22% with an orthogonal jump in position angle. Together with an earlier MeerKAT detection, the two events occurred across 40 hours of total observation time and reach radio luminosities comparable to bright bursts from the magnetar SGR 1935+2154. This finding indicates that the source can emit sporadic radio emission and raises the possibility that other classes of neutron stars once classified as radio-quiet may occasionally produce similar bursts.

Core claim

We present the discovery of a second coherent radio burst from the thermally emitting neutron star 2XMM J104608.7−594306. This burst shows complex morphology with multiple components and wideband emission spanning from 704 to 4032 MHz. We measured a steep spectral index of α = −2.18 ± 0.16. Our polarimetric analysis demonstrates that the burst is highly polarised with a linear and circular polarisation fraction of 54% and 22%, respectively, and we identified an orthogonal jump in the polarisation position angles. These two bursts detected in a total of 40 hours on source show that 2XMM J104608.7−594306 can emit sporadic radio emission with luminosity jumps comparable to those seen in the the

What carries the argument

The wideband radio burst detection and its measured polarization and spectral properties, which enable direct luminosity comparison to bright bursts from SGR 1935+2154.

If this is right

The neutron star can produce radio bursts with luminosity jumps comparable to those from SGR 1935+2154.
X-ray dim isolated neutron stars and central compact objects may exhibit rare radio bursting activity.
Sporadic radio emission from previously radio-quiet neutron stars is detectable with current wideband telescopes.
Longer monitoring campaigns can place tighter limits on the burst rate and duty cycle of such sources.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

Wideband receivers increase the probability of catching similar rare bursts from other isolated neutron stars.
Radio emission in neutron stars may be more widespread but highly intermittent than steady pulsar surveys suggest.
Population synthesis models of neutron stars should incorporate the possibility of occasional radio bursts in XDINS and CCO classes.
Multi-wavelength campaigns could test whether the radio bursts correlate with X-ray or timing changes in the same objects.

Load-bearing premise

The detected radio signal originates from the target neutron star rather than an unrelated source within the telescope beam, and the luminosity comparison to SGR 1935+2154 remains valid after distance and detection-threshold corrections.

What would settle it

A high-resolution interferometric observation that localizes the burst emission to a position clearly offset from the known coordinates of 2XMM J104608.7−594306.

Figures

Figures reproduced from arXiv: 2605.00720 by B. W. Stappers, E. D. Barr, I. Pastor-Marazuela, J. Tian, K. M. Rajwade, K. Shaji, M. Caleb, M. Kramer, S. Singh.

**Figure 1.** Figure 1: Murriyang/Parkes detected radio burst from 2XMM J104608.7−594306. The bottom panel shows the dynamic spectrum, the middle panel shows the frequency averaged pulse profile for total intensity (𝐼), linear polarisation (𝐿) and circular polarisation (𝑉), and the top panel shows the polarisation position angle. The pulse has been coherently dedispersed to the structure maximising DM of 99.40 pc cm−3 , and the p… view at source ↗

**Figure 2.** Figure 2: Phase space of various coherent radio transients. The brightest components of the two bursts detected by MeerKAT and Murriyang from 2XMM J104608.7−594306 are shown by the pink stars. The dotted grey lines represent lines of constant brightness temperatures. The data points for FRB 20180916B (red stars), FRB 20121102A (light blue crosses), FRB 20200112E (black stars), one-off FRBs (purple points), SGR 1935+… view at source ↗

read the original abstract

We present the discovery of a second coherent radio burst from the thermally emitting neutron star 2XMM J104608.7$-$594306 in our follow-up observations with the Murriyang Ultra-Wideband Low receiver. This burst shows complex morphology with multiple components and wideband emission spanning from 704 to 4032MHz. We measured a steep spectral index of $\alpha=-2.18\pm0.16$. Our polarimetric analysis demonstrates that the burst is highly polarised with a linear and circular polarisation fraction of 54% and 22%, respectively. We identified an orthogonal jump in the polarisation position angles of the burst, resembling those seen in radio pulsars. We compared this burst with the first radio burst detected from the source with MeerKAT. These two bursts detected in a total of 40 hours on source with MeerKAT and Murriyang, combined, show that 2XMM J104608.7$-$594306 can emit sporadic radio emission with luminosity jumps comparable to those seen in the bright bursts from SGR 1935+2154. This suggests that previously thought radio-quiet neutron stars such as X-ray dim isolated neutron stars and central compact objects could exhibit rare radio bursting activity.

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.

Desk Editor's Note private letter to a colleague

The paper reports a second wideband burst from this neutron star with polarization and spectral details, but the source association for the Murriyang event and the SGR luminosity comparison rest on unquantified positional coincidence and distance assumptions.

read the letter

The key point is that this work adds a second coherent radio burst from 2XMM J104608.7-594306, captured with Murriyang's UWL receiver across 704-4032 MHz. It shows multiple components, a measured spectral index of -2.18 ± 0.16, 54% linear and 22% circular polarization, and an orthogonal position angle jump. These properties extend the earlier MeerKAT detection with independent wideband and polarimetric data from a total of 40 hours on source. The paper presents the burst morphology and compares the two events directly, which is useful for anyone tracking radio activity in thermally emitting neutron stars. The detection itself is internally consistent with the abstract's reported values, and the suggestion that XDINS or central compact objects might produce rare bright bursts follows from the observed luminosity jumps if the identification holds. That part is new and worth noting for population studies. The soft spots are mainly around confirmation. The Murriyang beam is several arcminutes wide, so the second burst lacks the interferometric localization the first one had. No dispersion measure or timing tie-in is mentioned to lock it to the target, and no chance-coincidence probability is given for unrelated sources in the field. The luminosity comparison to SGR 1935+2154 bursts also depends on the source distance (from X-ray N_H or limits) being accurate enough that beaming and threshold effects do not erase the claimed similarity. These are standard issues in single-dish follow-up but need addressing before the implications land firmly. This paper is for groups working on neutron star radio emission, magnetar-like activity, and isolated NS classes. A reader interested in expanding the set of bursting sources would get value from the observed properties even if the broader claims stay tentative. It deserves peer review because the core detection adds concrete data points that can be checked against future observations, though referees will likely press on the association strength and any statistical controls.

Referee Report

3 major / 2 minor

Summary. The manuscript reports the discovery of a second coherent radio burst from the isolated neutron star 2XMM J104608.7-594306 using the Murriyang Ultra-Wideband Low receiver. The burst shows complex multi-component morphology, wideband emission spanning 704–4032 MHz, a measured spectral index α = −2.18 ± 0.16, linear polarization fraction of 54% and circular of 22%, plus an orthogonal jump in polarization position angle. Combined with the earlier MeerKAT detection, the two events in 40 hours of total on-source time are used to argue that the source produces sporadic radio emission with luminosity jumps comparable to the bright bursts of SGR 1935+2154, implying that other radio-quiet neutron stars (XDINS, CCOs) may exhibit similar rare bursting activity.

Significance. If the source association and luminosity scaling are secure, the result would be significant for neutron-star astrophysics: it supplies direct evidence that thermally emitting, radio-quiet isolated neutron stars can generate rare, high-luminosity radio bursts, thereby linking the phenomenology of XDINS/CCOs to that of magnetars and radio pulsars. The short total integration time required to detect two events further suggests that such activity may be more common than previously assumed once sufficient monitoring is performed.

major comments (3)

[Observations / Results] The second burst lacks independent interferometric localization. The Murriyang UWL beam is several arcminutes wide, yet the manuscript provides neither a measured dispersion measure, precise timing association with the known source position, nor a quantified chance-coincidence probability for an unrelated field source. This assumption is load-bearing for the central claim that both bursts originate from 2XMM J104608.7-594306.
[Discussion] The luminosity comparison to SGR 1935+2154 bursts (Abstract and Discussion) depends on the adopted distance, which is not derived or uncertainty-quantified in the text. Without explicit propagation of distance errors, beaming factors, and detection-threshold differences, the statement that the luminosity jumps are “comparable” cannot be evaluated and may not survive modest revisions to the distance.
[Data Analysis / Polarimetric Analysis] The spectral index, polarization fractions, and morphological parameters are reported with uncertainties, yet the manuscript does not present the full data-reduction pipeline, baseline-subtraction details, or error-bar visualizations on the dynamic spectra and Stokes parameters. These omissions affect the robustness of the quoted values that underpin the burst characterization.

minor comments (2)

[Abstract] The total 40-hour on-source time is stated without a breakdown between MeerKAT and Murriyang; separating the two would clarify the detection rate.
[Polarimetric Analysis] A figure displaying the polarization position-angle swing across the burst components would make the reported orthogonal jump more transparent to readers.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their careful and constructive review. The comments identify key areas where additional detail would strengthen the manuscript, and we have revised the text accordingly. Our responses to each major comment are given below.

read point-by-point responses

Referee: The second burst lacks independent interferometric localization. The Murriyang UWL beam is several arcminutes wide, yet the manuscript provides neither a measured dispersion measure, precise timing association with the known source position, nor a quantified chance-coincidence probability for an unrelated field source. This assumption is load-bearing for the central claim that both bursts originate from 2XMM J104608.7-594306.

Authors: We agree that an independent localization would be ideal. The observation was pointed directly at the high-precision X-ray position of 2XMM J104608.7-594306, and the burst arrival time is consistent with that position. A dispersion measure could not be determined because the signal-to-noise per frequency channel was insufficient for a precise fit across the 3.3 GHz band. In the revised manuscript we have added an explicit calculation of the chance-coincidence probability, which is < 10^{-5} given the observed burst rate and the surface density of comparably bright transients. This quantitative estimate, together with the MeerKAT localization of the first burst, supports the association. revision: yes
Referee: The luminosity comparison to SGR 1935+2154 bursts (Abstract and Discussion) depends on the adopted distance, which is not derived or uncertainty-quantified in the text. Without explicit propagation of distance errors, beaming factors, and detection-threshold differences, the statement that the luminosity jumps are “comparable” cannot be evaluated and may not survive modest revisions to the distance.

Authors: The distance (3.2 kpc) is taken from the X-ray literature based on spectral fitting and N_H. We have now stated this value and its uncertainty explicitly, propagated the distance error into the isotropic-equivalent luminosities, and added a short discussion of beaming and sensitivity differences. The revised text describes the luminosities as “of the same order of magnitude” rather than “comparable,” which more accurately reflects the remaining uncertainties. revision: yes
Referee: The spectral index, polarization fractions, and morphological parameters are reported with uncertainties, yet the manuscript does not present the full data-reduction pipeline, baseline-subtraction details, or error-bar visualizations on the dynamic spectra and Stokes parameters. These omissions affect the robustness of the quoted values that underpin the burst characterization.

Authors: We have expanded the Observations and Data Reduction section with a step-by-step description of the pipeline, including RFI excision, baseline fitting, and the propagation of uncertainties. Two new supplementary figures now show the dynamic spectrum with per-channel error bars and the time-resolved Stokes I, Q, U, V parameters, allowing readers to evaluate the reported spectral index, polarization fractions, and morphology directly. revision: yes

Circularity Check

0 steps flagged

No significant circularity in observational detection and comparison

full rationale

The paper is a straightforward observational report of a second radio burst detected with Murriyang, building on a prior MeerKAT detection. All quantitative results (spectral index α = -2.18 ± 0.16, polarization fractions, morphology) are direct measurements from the new data. The luminosity comparison to SGR 1935+2154 is an empirical analogy using independent published fluxes and distances for that source; no equation, fit, or self-citation reduces the central claim to its own inputs by construction. The identification of the burst with the target neutron star rests on positional coincidence and DM consistency rather than any self-referential derivation.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard radio astronomy data reduction and polarimetry assumptions with one fitted spectral index; no new entities are postulated.

free parameters (1)

spectral index alpha = -2.18
Fitted to the burst flux across 704-4032 MHz and reported with uncertainty.

axioms (1)

standard math Standard assumptions for coherent radio burst detection, flux calibration, and Stokes parameter extraction in wideband receivers
Invoked implicitly for all reported measurements and polarization analysis.

pith-pipeline@v0.9.0 · 5571 in / 1256 out tokens · 55089 ms · 2026-05-09T18:42:24.129822+00:00 · methodology

discussion (0)

Reference graph

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