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arxiv: 2606.18823 · v1 · pith:HAZJM4JDnew · submitted 2026-06-17 · 🌌 astro-ph.HE

Discovery of a 24-millisecond pulsar in a very long orbit with the Murchison Widefield Array

Chia Min Tan , N. D. Ramesh Bhat , Bradley W. Meyers , Christopher P. Lee , Ewan D. Barr , Vivek Venkatraman Krishnan , Paulo C. C. Freire , Garvit Grover
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Samuel J. McSweeney Nicholas A. Swainston Qiuyang Fu Mengyao Xue
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Pith reviewed 2026-06-26 20:08 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords millisecond pulsarbinary pulsarpulsar discoveryMurchison Widefield Arraylong-period binaryhelium white dwarflow-frequency survey
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The pith

A 24 ms pulsar has been found in a binary with an orbital period of roughly 834 days.

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

The paper reports the discovery of PSR J0125−5854, a 24-millisecond pulsar with a dispersion measure of 11.66 pc cm−3, located at high Galactic latitude. Follow-up timing with the MWA and MeerKAT shows the pulsar resides in a binary system whose orbital period is hinted to be 833.60 days, with a projected semi-major axis of 241.36 light-seconds, minimum companion mass of 0.4152 solar masses, and eccentricity of 0.0052. The spectrum is steep, and the companion is conjectured to be a helium white dwarf. The result emerged after processing only a fraction of the SMART survey data and therefore bears on the yield expected from that survey and from future SKA-Low observations.

Core claim

PSR J0125−5854 is a 24 ms pulsar with DM 11.66 pc cm−3 discovered in the ongoing Southern-sky MWA Rapid Two-metre survey. Timing data indicate a binary orbit with period 833.60 days, projected semi-major axis 241.36 light-seconds, minimum companion mass 0.4152 solar masses, and eccentricity 0.0052. The companion is likely a helium white dwarf and the spectrum has index −2.2. Further observations are required to refine the parameters.

What carries the argument

The binary orbital solution obtained by fitting pulse arrival times, which supplies the orbital period, projected semi-major axis, eccentricity, and mass function.

If this is right

  • The system most likely formed via a channel that leaves a helium white dwarf companion after mass transfer.
  • The steep spectrum implies the pulsar will be brighter at frequencies below those already observed.
  • Processing the remainder of the SMART survey data is expected to uncover additional millisecond pulsars.
  • Similar long-period systems should be detectable in planned low-frequency surveys with SKA-Low.

Where Pith is reading between the lines

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

  • If the orbit is confirmed, the object supplies a nearby, low-DM test case for studying wide binary evolution at high Galactic latitude.
  • The discovery shows that wide-field low-frequency arrays can locate pulsars whose long orbits make them hard to find in shorter pointed observations.
  • Confirmation would allow the mass function to be combined with optical or radial-velocity data to constrain the companion mass more tightly.

Load-bearing premise

The existing timing data span enough of the orbit to identify the true 834-day period without aliases from incomplete phase coverage.

What would settle it

New pulse arrival-time measurements over the next several months that fall outside the arrival-time window predicted by the 833.6-day orbital model.

Figures

Figures reproduced from arXiv: 2606.18823 by Bradley W. Meyers, Chia Min Tan, Christopher P. Lee, Ewan D. Barr, Garvit Grover, Mengyao Xue, N. D. Ramesh Bhat, Nicholas A. Swainston, Paulo C. C. Freire, Qiuyang Fu, Samuel J. McSweeney, Vivek Venkatraman Krishnan.

Figure 1
Figure 1. Figure 1: PRESTO detection plot of PSR J0125−5854 from the discovery observation: the top left panel shows the integrated (time-averaged) pulse profile; the bottom left panel displays the signal strength versus pulse phase and time; the middle panel shows signal strength versus pulse phase and frequency; the remainder plots are various diagnostic plots from the search pipeline, showing the best period and dispersion… view at source ↗
Figure 2
Figure 2. Figure 2: Detection plots of PSR J0125−5854 across the frequency range spanning from ∼150 MHz to 2.8 GHz; from left to right, the MWA discovery observation (140–170 MHz) and MeerKAT detections in the UHF, L band, and S1 band. The upper panels show the integrated profiles, and the lower panels the time-averaged signal in pulse phase vs frequency. The integration times are 80 min for the MWA band, 60 min for UHF, and … view at source ↗
Figure 3
Figure 3. Figure 3: Integrated profiles of PSR J0125−5854 from MWA and MeerKAT observations, showing the profile evo￾lution across the frequency range from ∼100 MHz to 3 GHz. The MWA profile is from an 80 min integration, whereas for MeerKAT, it is 60 min in the UHF band, and 30 min each in the L and S1 bands. MeerKAT profiles are at a higher time resolution (1024 phase bins) compared to the MWA profile (128 phase bins). the … view at source ↗
Figure 4
Figure 4. Figure 4: The MWA localization of PSR J0125−5854 from the discovery observation. The nine adjacent detections were able to constrain the pulsar position to within a 2.4 ′ (5σ) confidence region, shown by the dotted ellipse. a maximum-likelihood estimation approach that is sim￾ilar to the method implemented in SeeKAT (M. C. Bezuidenhout et al. 2023) but suitably adapted for MWA, taking into account the complexity of … view at source ↗
Figure 5
Figure 5. Figure 5: The localization plots obtained from SeeKAT on the three MeerKAT observations. The left plot is the localization position obtained from the UHF-band observation. The middle plot is the localization position obtained from the L-band observation and the right plot is the localization position obtained from the S1-band observation. The grid on each plot are drawn at intervals of 10 arcseconds. The boxes in th… view at source ↗
Figure 6
Figure 6. Figure 6: The measured barycentric spin period of PSR J0125−5854 from all the observations where the pulsar is detected. Inset : Zoomed in plot of the measured spin periods from MJD 60550. Blue points are observations from the MWA telescope and orange points are observations from the MeerKAT telescope. The error-bars in the measured spin period are small relative to the scale of the plot. The scatter in the measured… view at source ↗
Figure 7
Figure 7. Figure 7: Top: The solid line shows the variation of the spin period expected from the best-fit orbital model for the PSR J0125−5854 system and the blue dots showing the measured period of the pulsar at all observation epochs. Bottom: The residuals in the measured spin periods compared to the ex￾pected values from the modeled orbit. The rms value and the reduced χ 2 of the fit 5 × 10−6 ms and 7.3 respectively. 3.2.2… view at source ↗
Figure 9
Figure 9. Figure 9: Scatter plot showing the eccentricity and the min￾imum companion mass of the 16 pulsars with known binary orbital period of more than 290 days. The circle points are companions that are most likely to be main sequence stars and the triangle points are companions that are most likely to be white dwarfs. PSR J0125−5854 is shown as a cross. The color of the points shows the spin period of the pulsars in their… view at source ↗
Figure 11
Figure 11. Figure 11: Comparison between the measured eccentricity and the expected eccentricity, as predicted by E. S. Phinney (1992), of PSR J0125−5854 (as a cross) and the 12 pulsars likely with WD companion. The solid line is where the mea￾sured and expected eccentricity is equal and the dash lines are where the measured and expected eccentricity differs by a factor of 2. We plotted the measured eccentricity against the pr… view at source ↗
Figure 10
Figure 10. Figure 10: Scatter plot showing the relationship between the orbital period of a binary pulsar system and the mass of the companion, for different types of companion, all with known masses, obtained from version 2.7.0 of the Australia Telescope National Facility (ATNF) pulsar catalog. The shaded region is the expected relationship between the or￾bital period and the mass of a He WD for the different types of progeni… view at source ↗
Figure 12
Figure 12. Figure 12: The g, r, i and z filter 8′′ × 8 ′′ images cen￾tered on the optical source at (R.A., Dec.) = (01h25m47.20s, -58d54m02.35s), as seen by the DECam of the DESI Legacy Surveys. The white circle is the uncertainty region of the position of PSR J0125−5854 obtained from the localization efforts of MeerKAT telescope. The source is located on the right side of the uncertainty region of the position of PSR J0125−58… view at source ↗
Figure 13
Figure 13. Figure 13: Corner plot for MCMC fit for PSR J0125−5854 orbit, for the case where e = 0.01. Bhat, N. D. R., Swainston, N. A., McSweeney, S. J., et al. 2023b, PASA, 40, e020, doi: 10.1017/pasa.2023.18 Burgay, M., D’Amico, N., Possenti, A., et al. 2003, Nature, 426, 531–533, doi: 10.1038/nature02124 Camilo, F., Lyne, A. G., Manchester, R. N., et al. 2001, ApJL, 548, L187, doi: 10.1086/319120 Camilo, F., Ray, P. S., Ran… view at source ↗
read the original abstract

We report the discovery of PSR J0125$-$5854, a pulsar with a spin period of 24 ms and a dispersion measure of 11.66 pc cm$^-3$ in the ongoing Southern-sky MWA Rapid Two-metre (SMART) survey with the Murchison Widefield Array (MWA). The pulsar is located at a high Galactic latitude of $-57^{\circ}$, and at a distance of 0.5$\text{-}$1 kpc per the Galactic electron density models. Follow-up observations with the MWA and MeerKAT telescopes have revealed that this pulsar is in a binary system with an orbital period of more than 290 days, and a steep spectrum (flux density, $ S \propto \nu^{\alpha} $, where $\nu$ is frequency and $ \alpha = -2.2 \pm 0.3 $). Analysis of current observational data hints at a potential binary configuration with an orbital period of $833.60 \pm 0.04$ days, a projected semi-major axis of $241.36 \pm 0.05$ light-seconds, and a minimum companion mass $0.4152 \pm 0.0001$ M$_\odot$, with a low eccentricity orbit of $0.0052 \pm 0.0006$. We discuss the potential formation channels for this system, and conjecture that the companion is likely a Helium white dwarf. Further observations are required in order to better constrain the orbital and spin parameters. We discuss the implications of this discovery, which emerged after processing a small fraction of survey data, on the prospects of finding more millisecond pulsars with the SMART survey, and with future surveys planned with the low-frequency SKA-Low.

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 / 0 minor

Summary. The manuscript reports the discovery of the 24 ms pulsar PSR J0125−5854 (DM = 11.66 pc cm−3) in the MWA SMART survey at high Galactic latitude. Follow-up MWA and MeerKAT observations establish that the pulsar is in a binary with orbital period >290 days and a steep spectrum (α = −2.2 ± 0.3). Timing analysis of the available data yields a candidate orbital solution (P_orb = 833.60 ± 0.04 d, a sin i = 241.36 ± 0.05 lt-s, e = 0.0052 ± 0.0006, minimum companion mass 0.4152 ± 0.0001 M_⊙) that the authors explicitly label as preliminary; they conjecture a helium white-dwarf companion and note that additional observations are required to confirm the orbit. The discovery is used to highlight prospects for the SMART survey and SKA-Low.

Significance. If the long-period binary solution is verified, the system would be a valuable addition to the small sample of millisecond pulsars with orbital periods of hundreds of days, directly constraining formation channels that produce helium white-dwarf companions. The low DM, high latitude, and steep spectrum are observationally robust and useful for population studies at low frequencies. The fact that the pulsar was found after processing only a small fraction of the survey data provides concrete evidence of the discovery potential of the MWA and future SKA-Low pulsar searches.

major comments (1)
  1. [Abstract and orbital-analysis section] Abstract and orbital-analysis section: the quoted orbital parameters carry formal uncertainties (P_orb to ±0.04 d, companion mass to ±0.0001 M_⊙) that presuppose a unique periodicity, yet the text states that the data only 'hint at a potential binary configuration' and that 'the current observational data' are insufficient to confirm the period. No information is supplied on the total timing baseline, number of independent TOAs, or any search for 1-year aliases (e.g., via a periodogram or χ² landscape), leaving the uniqueness of the 833.6 d solution unverified. Because the title and abstract foreground the 'very long orbit,' this assumption is load-bearing for the central claim.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful and constructive review. We agree that the presentation of the candidate orbital solution requires additional supporting details and clearer caveats to avoid any implication of a confirmed unique periodicity. We will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract and orbital-analysis section] Abstract and orbital-analysis section: the quoted orbital parameters carry formal uncertainties (P_orb to ±0.04 d, companion mass to ±0.0001 M_⊙) that presuppose a unique periodicity, yet the text states that the data only 'hint at a potential binary configuration' and that 'the current observational data' are insufficient to confirm the period. No information is supplied on the total timing baseline, number of independent TOAs, or any search for 1-year aliases (e.g., via a periodogram or χ² landscape), leaving the uniqueness of the 833.6 d solution unverified. Because the title and abstract foreground the 'very long orbit,' this assumption is load-bearing for the central claim.

    Authors: We accept this criticism. The quoted values were obtained from a preliminary least-squares fit to the sparse timing data available at submission, but the formal uncertainties and the foregrounding in the title/abstract do risk overstating the robustness of the 833.6 d solution. In the revised version we will (i) state the total timing baseline and the exact number of independent TOAs used, (ii) include a χ² landscape or periodogram over a wide range of trial periods (including around 1 yr aliases) to demonstrate that the reported solution is preferred, and (iii) rephrase the abstract and orbital-analysis section to describe the parameters explicitly as a candidate solution pending confirmation with additional observations. These changes will be made without altering the scientific claim that the data currently favour a very long orbit. revision: yes

Circularity Check

0 steps flagged

No significant circularity; all quantities are direct observational measurements and standard timing fits.

full rationale

The manuscript is an observational discovery report. Spin period (24 ms), DM (11.66 pc cm^{-3}), spectral index, and candidate binary parameters (P_orb = 833.60 ± 0.04 d, a sin i = 241.36 ± 0.05 lt-s, e = 0.0052 ± 0.0006, m_c,min = 0.4152 ± 0.0001 M_⊙) are obtained by direct detection in SMART survey data followed by least-squares timing fits to MWA + MeerKAT TOAs. No equations, ansatzes, or self-citations reduce any reported value to an input by construction. The text explicitly labels the orbit a 'hint' and states further observations are required, confirming the result is not presented as a closed derivation. The chain is data → standard pulsar timing software → fitted parameters, which is self-contained and externally falsifiable.

Axiom & Free-Parameter Ledger

4 free parameters · 2 axioms · 0 invented entities

The claim rests on standard radio pulsar detection and timing methods plus Galactic electron density models for distance; the main free parameters are the fitted orbital elements derived from the timing data.

free parameters (4)
  • orbital period = 833.60 days
    Fitted value 833.60 days from timing analysis of current data
  • projected semi-major axis = 241.36 light-seconds
    Fitted value 241.36 light-seconds
  • eccentricity = 0.0052
    Fitted value 0.0052
  • minimum companion mass = 0.4152 M_sun
    Derived minimum mass 0.4152 solar masses from orbital parameters
axioms (2)
  • domain assumption Galactic electron density models accurately convert DM to distance
    Used to estimate distance 0.5-1 kpc from DM=11.66 pc cm^-3
  • domain assumption Standard pulsar timing analysis can extract orbital parameters from sparse observations
    Applied to derive the candidate 833-day orbit

pith-pipeline@v0.9.1-grok · 5924 in / 1534 out tokens · 33685 ms · 2026-06-26T20:08:36.820282+00:00 · methodology

discussion (0)

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