A new long period radio transient: Discovery of pulses repeating every 1.16 hours from ASKAP J175534.9-252749.1

Akash Anumarlapudi; Angie Waszewski; Csan\'ad Horv\'ath; David L. Kaplan; Dougal Dobie; John Morgan; Kovi Rose; Natasha Hurley-Walker; Samuel J. McSweeney; Ziteng Wang

REVIEW 1 major objections 1 minor 1 cited by

A new long period radio transient: Discovery of pulses repeating every 1.16 hours from ASKAP J175534.9-252749.1

T0 review · 1 major / 1 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Radio pulses from J1755−2527 repeat every 1.16 hours, confirming it as a long-period transient whose timing and polarisation point toward a white dwarf binary.

desk verdict A solid, transparent confirmation of a ~1.16-hour LPT period that deserves peer review, but the authors should rule out or explicitly discuss the P/2 alias before the headline period is taken at face value. read the letter →

arxiv 2507.14448 v1 pith:OWDWEECO submitted 2025-07-19 astro-ph.HE astro-ph.SR

Samuel J. McSweeney , Natasha Hurley-Walker , Csanád Horváth , Akash Anumarlapudi , Angie Waszewski , Dougal Dobie , David L. Kaplan , John Morgan

show 2 more authors

Kovi Rose Ziteng Wang

This is my paper

classification astro-ph.HEastro-ph.SR

keywords radiotransientslongperiodpulsartimingpulsescatteringpolarisationwhitedwarfbinariescontinuum:dwarfs

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper reports new detections of radio pulses from ASKAP J175534.9−252749.1, a source previously seen only once, and shows that they repeat every 1.16 hours ($P = 4186.3285 \pm 0.0002$ s) with a phase-stable timing solution spanning about 1.5 years. The pulses are broad and asymmetric at low frequencies, and the paper accounts for this by modelling each burst as a Gaussian convolved with a thin-screen scattering tail. On that basis it derives a dispersion measure of $733 \pm 22$ pc cm$^{-3}$ and a scattering timescale near 70 ms at 1 GHz. The paper interprets the many historical non-detections as intrinsic intermittency on month-long timescales, and conjectures that the source may be a white dwarf in a binary orbit, with a period slightly shorter than the canonical minimum for cataclysmic variables. If correct, this turns a single enigmatic pulse into a member of the growing class of long-period radio transients and gives a concrete target for testing what those systems are.

What carries the argument

The load-bearing device is the exponentially modified Gaussian (EMG) pulse model, an intrinsic Gaussian of width $\sigma$ convolved with a one-sided exponential scattering kernel of timescale $\tau(\nu) = 0.07\,(\nu/\mathrm{GHz})^{-4}$ s (Equation 1). Fitting this shape to each pulse and taking the fitted centre $\mu$ as the time of arrival removes the frequency-dependent delay that scattering introduces at low frequencies, so that pulses from 170 MHz to 2.1 GHz can be folded into a single ephemeris. The same model yields a closed-form scattering delay $\Delta t_{\mathrm{sc}}(\nu)$ (Equation 5) that the paper adds to the usual dispersion delay when predicting future pulse arrival times below about 300 MHz.

What would settle it

A single high-signal-to-noise observation that catches the same pulse simultaneously at a low frequency (around 185–200 MHz) and a high frequency (around 800–900 MHz) would break the DM–scattering degeneracy: if the low-frequency time of arrival cannot be reconciled with DM = 733 pc cm$^{-3}$ using $\tau_{\mathrm{sc},1\,\mathrm{GHz}} = 0.07$ s and a $\nu^{-4}$ scaling, the assumed scattering law is wrong. Equivalently, measuring an in-band DM from subband times of arrival at 185 MHz (Appendix B reports $1221 \pm 257$ pc cm$^{-3}$) and finding the residual after applying the EMG correction to exceed the model's prediction of a few hundred pc cm$^{-3}$ would falsify the fixed thin-screen model.

Watch

Extended reading notes

Core claim

The central claim is that J1755−2527 is a genuine long-period transient whose pulses arrive coherently every $P = 4186.3285 \pm 0.0002$ s (about 1.16 hours), established by fitting roughly sixty pulses detected across MWA, ASKAP, MeerKAT and ATCA between 2023 and 2024. The timing solution treats the observed pulse shape as an intrinsically Gaussian burst scattered by a thin screen, fixes the scattering timescale to $\tau_{\mathrm{sc},1\,\mathrm{GHz}} \simeq 0.07$ s scaling as $\nu^{-4}$, and identifies the unscattered Gaussian centre as the true time of arrival. With that assumption the paper derives DM = 733 ± 22 pc cm$^{-3}$, finds no significant period derivative, and predicts arrival times through an ephemeris that includes both dispersion and scattering delays. The paper further reports that the source is intermittent on month-long timescales and that its three bright pulses show strikingly different polarisation-angle behaviour: only the original 2023 ASKAP pulse follows the rotating vector model, while the 2024 ASKAP pulse has a flat polarisation angle curve and the 2024 MeerKAT pulse shows a curved, non-RVM pattern. Taken together, the authors argue, the properties are consistent with a white dwarf in a binary orbit, though the period is marginally shorter than the canonical orbital-period minimum of cataclysmic variables.

Load-bearing premise

The timing solution stands or falls on the assumption that each pulse is intrinsically Gaussian and scattered by a single thin screen with a fixed $\nu^{-4}$ timescale of 0.07 s at 1 GHz, so that the fitted unscattered centre is the true arrival time; if that shape law is wrong, the arrival times carry frequency-dependent biases that could shift the DM and slightly bias the period.

Editorial extensions

If this is right

J1755−2527 becomes a confirmed long-period transient with the fifth-longest period known in the class, extending the observed period–duty-cycle phase space.
Future observations can predict pulse arrival times to within seconds at low frequencies and better at high frequencies, so monitoring campaigns know when to point.
The historical non-detections are reclassified as intrinsic month-long intermittency, implying that other long-period transient candidates with single detections deserve repeated monitoring.
A white-dwarf binary interpretation places J1755−2527 below the canonical ~1.3-hour orbital-period minimum of polars, making it a test case for binary evolution models.
The different polarisation-angle behaviours across three bright pulses show that a single rotating-vector-model fit is not universal for this source, cautioning against interpreting individual pulses as complete geometric models.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

Editorial inference: If the intermittency window is itself periodic on month-long timescales, it could be the beat pattern of a spin–orbit resonance close to, but not exactly, a small-integer ratio; this is testable with a long, regular monitoring campaign.
Editorial inference: The reported dispersion measure may carry a systematic bias from the assumed $\nu^{-4}$ thin-screen scattering law; a simultaneous multi-frequency detection of one pulse would measure DM and scattering jointly and either confirm the ephemeris or revise it.
Editorial inference: The same exponentially-modified-Gaussian timing technique could be applied to other single-pulse transients awaiting confirmation; phase-coherent repeat pulses would immediately classify them as long-period transients and grow the population available for population-level tests.
Editorial inference: If the flat and non-RVM polarisation curves of the 2024 pulses are caused by changes in the local plasma environment rather than geometry, monitoring polarisation over an active window could trace those changes directly.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Bottom line up front: this is a solid paper that does what Paper I could not — it turns a single 2-minute pulse into a timed, multi-telescope periodic source. Roughly 60 detections across MWA, ASKAP, MeerKAT, and ATCA give a coherent timing solution over 1.5 years. The scattering-aware ToA formula (Eqs. 3–5) is a genuine small methodological contribution, and the authors are transparent about the DM–scattering degeneracy and the fixed tau_sc. The public data products on GitHub are a plus. I believe the central claim: J1755-2527 is a repeating LPT with a well-defined period. The one caveat that should keep you from taking the headline period at face value is harmonic ambiguity. All same-band interpulse intervals in Table C1 are integer multiples of the quoted P = 4186.3285 s, so they are also even multiples of P/2. A model with a fundamental period of 2093.16 s and every other pulse missing or below threshold predicts exactly the same ToAs. The paper does not report a period search, an alias check, or a direct search for pulses at odd half-cycles. I don't think this is a deal-breaker: the 2024 GPM blind detections all fall at one phase, which argues against equal-amplitude alternating pulses, and the timing solution is a real description of the observed pulses. But the physical interpretation — sitting just below the CV orbital period minimum — changes if the true fundamental is half the quoted value. The authors should either run the half-cycle search or explicitly state that the factor-of-two ambiguity is unresolved. Other soft spots are minor and acknowledged: the fixed tau_sc = 70 ms leaves systematic DM errors of up to tens of seconds, and the re-reduction of the 2023 MeerKAT data happened after the ephemeris was known, though the pulses landed at predicted times and later detections were blind. The citation pattern looks appropriate; the paper engages the recent LPT and WD-binary literature without excessive self-reference. Who this is for: anyone working on long-period radio transients or WD binary evolution. It is a useful data point, not a field-reshaping result. I would send it to peer review rather than desk reject, and I would accept after a moderate revision that addresses the half-period alias.

Referee Report

1 major / 1 minor

Summary. The paper reports new radio pulses from the long-period transient candidate ASKAP J175534.9-252749.1, detected with MWA, ASKAP, MeerKAT, and ATCA over a 1.5-year baseline. The authors fit a timing solution with period P = 4186.3285 ± 0.0002 s (~1.16 h), DM = 733 ± 22 pc cm^-3, and a fixed scattering timescale of 70 ms at 1 GHz, using ToAs derived from exponentially modified Gaussian fits to the pulse profiles. The paper also presents polarimetry for three bright pulses, finding that only the original ASKAP pulse shows an RVM-like PA curve, and interprets historical non-detections as month-long intermittent activity. The authors conjecture that J1755-2527 may be a white-dwarf binary system with a period marginally shorter than the canonical CV orbital period minimum.

Significance. If the claimed 1.16-h period is correct, this source is an important addition to the growing LPT population and provides a potentially interesting data point for models of WD+M-dwarf binaries near the orbital period minimum. The paper's strengths include a multi-telescope detection campaign, a coherent timing solution spanning ~1.5 years with ~60 pulses, a blind detection in the 2024 GPM data, and public release of dynamic spectra and timing products. The detailed Appendix B analysis of scattering-induced timing biases is a useful contribution. However, the central period claim is undermined by an unaddressed harmonic ambiguity: all observed ToA separations are integer multiples of P and hence even multiples of P/2, so the data cannot distinguish P from a fundamental period of P/2 with alternating missing pulses. This ambiguity directly affects the headline result and the physical interpretation, so the paper requires revision before the central claim can be accepted.

major comments (1)

[§3.2, Table 2, Fig. 1] The paper should provide a version of the manuscript with line numbers, to facilitate refereeing.

minor comments (1)

[§4] In Appendix B, 'pmcm−3' should be 'pc cm−3'.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: timing solution is self-contained and externally anchored; P/2 harmonic is a non-circular degeneracy caveat.

full rationale

The paper's central claim—that J1755−2527 repeats with P = 4186.3285 s—is produced by a conventional timing fit (Section 3.2) to barycentred ToAs taken as the μ parameter of EMG fits. The scattering timescale τ_sc,1GHz = 0.07 s is fixed from external NE2001/YMW16 models (Eq. 2), not fitted to the target result, so the ToA correction is not circular. The 2024 GPM MWA detection was blind; the subsequent DDT and archival MeerKAT detections were checked against an ephemeris derived from other data, giving an independent (if not fully blind) confirmation. Self-citations (Paper I; Hurley-Walker et al. 2022, 2023, 2024; Horváth et al. submitted) supply survey context, detection methodology, and comparative LPT nomenclature; none of them is the load-bearing premise for the measured period. The paper does contain a real underdetermination that is not circularity: all reported ToA separations are integer multiples of P and therefore even multiples of Q = P/2, so a model with fundamental period Q and pulses appearing only at alternate cycles reproduces the same ToAs exactly. Table 2 reports P without testing or excluding Q; this is an aliasing/degeneracy concern (a correctness risk for the physical interpretation), not a self-referential derivation, and does not raise the circularity score.

Assumptions & free parameters 5 free parameters · 5 assumptions · 0 invented entities

The timing solution rests on the fitted period, epoch, DM, and assumed scattering timescale. The scattering model is the main external input that could bias the derived quantities. No new physical entities are introduced.

free parameters (5)

Period P = 4186.3285 ± 0.0002 s
Fitted to all barycentred ToAs; this is the central claim of the paper.
PEPOCH = MJD 59965.03792 ± 0.00003
Reference epoch of the timing ephemeris (Table 2).
DM = 733 ± 22 pc cm^-3
Fitted from frequency-dependent ToAs, but partially degenerate with the assumed scattering timescale.
Scattering timescale tau_sc,1GHz = 0.07 s (assumed)
Fixed from NE2001/YMW16 predictions, not fitted; used in Eq. 2 to correct all ToAs for scattering.
Pdot = (-10 ± 92) x 10^-12 s s^-1
Fitted spin-down rate, consistent with zero.

assumptions (5)

domain assumption The intrinsic pulse shape is Gaussian before scattering.
Used in Eq. 1 for the exponentially modified Gaussian fit; Section 3.1.
domain assumption Scattering follows a single thin-screen model with a one-sided exponential kernel and tau(nu) = 0.07 (nu/GHz)^-4 s.
Eq. 2 and Appendix B; underlies the ToA extraction and the timing solution.
domain assumption NE2001 and YMW16 Galactic electron density models give the scattering timescale at the source position.
Section 3.1; the assumed tau_sc,1GHz = 70 ms comes from these models.
standard math Standard pulsar timing corrections (barycentring, dispersion law) apply.
Section 3.2 and Eq. 4.
domain assumption The rotating vector model describes the expected PA swing for a rotating dipolar magnetosphere.
Section 3.3; used to interpret the PA curves, not load-bearing for the periodicity claim.

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Cite this review

Pith. "Pith review of A new long period radio transient: Discovery of pulses repeating every 1.16 hours from ASKAP J175534.9-252749.1." pith.science (2026). https://pith.science/paper/OWDWEECO

@misc{pith2026250714448,
  author       = {Pith},
  title        = {Pith review of: A new long period radio transient: Discovery of pulses repeating every 1.16 hours from ASKAP J175534.9-252749.1},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OWDWEECO}},
  note         = {Machine review of arXiv:2507.14448}
}

read the original abstract

We report the discovery of several new pulses from the source ASKAP J175534.9-252749.1 (J1755-2527), originally identified from a single 2-min long pulse, confirming it as a long period transient (LPT) with a period of ~1.16 hours. The pulses are significantly scattered, consistent with Galactic electron density models. Two of the new pulses also had measurable polarisation, but unlike the originally detected pulse, the polarisation angle does not behave as expected from the rotating vector model. We interpret historical non-detections of J1755-2527 as an intrinsic intermittency that occurs on month-long timescales, and discuss possible causes. We conjecture that, like some other LPTs with periods >~ 1 hour, J1755-2527 may host a white dwarf in a binary orbit, but note that its period is marginally shorter than the canonical orbital period minimum of cataclysmic variables. Our work highlights the importance of additional observations in establishing the nature of unusual radio-emitting objects.

Figures

Figures reproduced from arXiv: 2507.14448 by the authors.

**Figure 1.** Pulsestack of barycentred, dedispersed profiles from the ephemeris. The dashed green vertical line marks zero phase. Baselines have been fitted and subtracted from each lightcurve. The red curves are fits of the normalised pulses to Equation 1, and the blue curves are the inferred Gaussian pulses without scattering, also normalised (see main text for details). MNRAS 000, 1–12 (2025) [PITH_FULL_IMAGE:figures/full_fi… view at source ↗

**Figure 2.** Stacked (semi-transparent) dynamic spectra, where each rectangle indicates the observing campaign whose spectra were barycentred and folded according to the ephemeris. The spectra have not been dedispersed, but the cyan dashed lines indicate where the two components seen in the MeerKAT (2024) observation would appear due to dispersion. The white curve in the top panel is the dedispersed profile of the MeerKAT (2024)… view at source ↗

**Figure 3.** Timing residuals (top panel) and other pulse properties derived from the fits of Equation 1 to the individual light curves (second and third panels). The peak flux, 𝑆peak, equivalent to the 𝐴 parameter in equation 1, is the peak flux of the modelled unscattered pulse. The bottom panel displays 𝑆peak,1GHz = 𝑆peak (𝜈/GHz) −𝛼, where 𝛼 = −2 has been assumed. Notable features of interest include the relative brightness o… view at source ↗

Figures from the paper (2 more)

**Figure 4.** Figure 4: Polarisation of the 2023 and 2024 ASKAP pulses (left and middle) and the 2024 MeerKAT pulse (right). The top two rows show the RM and 𝛼lin parameters fitted to Equation 7 for each time bin independently. Only bins for which the uncertainty on 𝛼lin is less than 1.4 are …

**Figure 5.** Figure 5: Duty cycle vs radio pulse period for various long period radio emitters (de Ruiter et al. 2025; Hurley-Walker et al. 2022, 2023; Caleb et al. 2024; Hyman et al. 2005; de Ruiter et al. 2025; Lee et al. 2025; Wang et al. 2024). The duty cycles are derived from the report…

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Rapid Response Triggering for Radio Transients with the SKA Observatory
astro-ph.IM 2026-07 accept novelty 3.0 of 10

SKA-Low and SKA-Mid should implement automated rapid-response triggering on external and internal alerts to enable early radio observations of diverse transients.

Reference graph

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write newline

" write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.stat...

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.

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