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arxiv: 1906.09793 · v1 · pith:CJZUF4LBnew · submitted 2019-06-24 · 🌌 astro-ph.HE

Commensal discovery of four Fast Radio Bursts during Parkes Pulsar Timing Array observations

S. Os{\l}owski , R. M. Shannon , V. Ravi , J. F. Kaczmarek , S. Zhang , G. Hobbs , M. Bailes , C. J. Russell
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W. van Straten C. W. James A. Jameson E. K. Mahony P. Kumar I. Andreoni N. D. R. Bhat S. Burke-Spolaor S. Dai J. Dempsey M. Kerr R. N. Manchester A. Parthasarathy D. Reardon J. M. Sarkissian R. Spiewak L. Toomey J.-B. Wang L. Zhang X.-J. Zhu
This is my paper

Pith reviewed 2026-05-25 17:22 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords fast radio burstsParkes telescopepulsar timing arraycommensal searchradio polarizationdispersion measure
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The pith

Four fast radio bursts were discovered during routine pulsar timing observations at Parkes, including one with the highest signal-to-noise ratio recorded there.

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 four fast radio bursts found while monitoring millisecond pulsars as part of the Parkes Pulsar Timing Array project. These events were identified through a commensal search running in parallel with the primary timing observations. One burst reaches the highest signal-to-noise ratio ever seen at Parkes and displays unusual spectral properties, while all four show high polarization. The work illustrates how ongoing pulsar monitoring programs can contribute to FRB discoveries without requiring separate telescope time.

Core claim

We report the discovery of four FRBs (171209, 180309, 180311 and 180714) during commensal searches in PPTA observations. The detected events include an FRB with the highest signal-to-noise ratio ever detected at the Parkes observatory, which exhibits unusual spectral properties. All four FRBs are highly polarized.

What carries the argument

The commensal FRB search pipeline applied to Parkes Pulsar Timing Array data, which identifies dispersed, polarized pulses in the same observations used for pulsar timing.

If this is right

  • Existing pulsar timing array observations can be used to detect FRBs without dedicated observing time.
  • High signal-to-noise FRBs found this way allow detailed study of spectral and polarization properties.
  • The method can be extended to other telescopes running similar pulsar monitoring programs.
  • Accumulating more such events will improve statistics on FRB rates and sky distribution.

Where Pith is reading between the lines

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

  • Commensal searches may raise the overall FRB detection rate by using time already allocated to other projects.
  • The high polarization fraction could indicate that these bursts share propagation effects or emission physics with other known FRBs.
  • If the unusual spectral properties prove common, they may constrain models of the burst emission region or intervening plasma.

Load-bearing premise

The detected signals are genuine astrophysical fast radio bursts and not terrestrial radio-frequency interference or instrumental artifacts.

What would settle it

Reprocessing the raw voltage data and finding that the signals lack the expected dispersion measure sweep, Faraday rotation, or polarization signature consistent with an astrophysical origin would falsify the claim.

Figures

Figures reproduced from arXiv: 1906.09793 by A. Jameson, A. Parthasarathy, C. J. Russell, C. W. James, D. Reardon, E. K. Mahony, G. Hobbs, I. Andreoni, J.-B. Wang, J. Dempsey, J. F. Kaczmarek, J. M. Sarkissian, L. Toomey, L. Zhang, M. Bailes, M. Kerr, N. D. R. Bhat, P. Kumar, R. M. Shannon, R. N. Manchester, R. Spiewak, S. Burke-Spolaor, S. Dai, S. Os{\l}owski, S. Zhang, V. Ravi, W. van Straten, X.-J. Zhu.

Figure 1
Figure 1. Figure 1: The four sub figures show the polarization position angles (top panels) and polarized pulse profiles (bottom panels, where the black line denotes total intensity, while red and blue show the linear and circular polarization, respectively) for all the four FRBs discovered during PPTA observations. The dashed lines for FRB180309 indicate that caution is needed when interpreting the polarisation. MNRAS 000, 1… view at source ↗
Figure 2
Figure 2. Figure 2: , with the top panel showing the total flux density pulse profile of the burst, while the bottom panel shows the spectrum of the burst6 . The S/N of the burst in these folded data is 46.2. After taking the integration of eight seconds of data and pulsar period as well as extra smearing due to CASPSRs channelisation being twice as coarse into account, we estimate the intrinsic S/N of the burst must have bee… view at source ↗
Figure 3
Figure 3. Figure 3: The time-averaged spectrum during FRB 180309 event. The red line is the baseline spectrum of the observed pulsar (PKS J2124−3358), the dark and light grey bounding boxes signify 1- and 3σ RMS noise, respectively. spectrum as it does not coincide with the brightest parts of the spectrum from other beams and CASPSR. Soon after the detection of this bright burst, we performed follow-up observations using the … view at source ↗
Figure 4
Figure 4. Figure 4: Limits at 95% confidence level on the presence of repeating FRBs from the PPTA observations. Blue, solid line: solid angle Ωlim(z) over which the presence of any FRBs with properties similar to FRB 121102 can be excluded within redshift z. Red, dashed line: differential volume at redshift z within which the presence of such an FRB can be excluded. E0 = 1.7 · 1038 erg, and rate decreasing with energy to the… view at source ↗
read the original abstract

The Parkes Pulsar Timing Array (PPTA) project monitors two dozen millisecond pulsars (MSPs) in order to undertake a variety of fundamental physics experiments using the Parkes 64m radio telescope. Since June 2017 we have been undertaking commensal searches for fast radio bursts (FRBs) during the MSP observations. Here, we report the discovery of four FRBs (171209, 180309, 180311 and 180714). The detected events include an FRB with the highest signal-to-noise ratio ever detected at the Parkes observatory, which exhibits unusual spectral properties. All four FRBs are highly polarized. We discuss the future of commensal searches for FRBs at Parkes.

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 four fast radio bursts (FRBs 171209, 180309, 180311 and 180714) found during commensal searches in Parkes Pulsar Timing Array observations of millisecond pulsars. One event has the highest signal-to-noise ratio yet recorded at Parkes and shows unusual spectral properties; all four are highly polarized. The paper discusses the value of such commensal searches going forward.

Significance. If the detections are confirmed as astrophysical, the work adds four new FRBs to the sample, including a record-S/N event and a set of highly polarized bursts that may constrain emission physics. It also demonstrates an efficient use of existing telescope time for FRB discovery, which could increase detection rates without dedicated allocations.

major comments (1)
  1. [Observations / data processing (methods section describing the search pipeline)] The abstract and methods description provide no quantitative false-positive rate for the commensal pipeline, no blind-injection recovery statistics, and no explicit tests against known Parkes RFI families. These details are load-bearing for the central claim that the four signals are genuine astrophysical FRBs rather than terrestrial interference or artifacts.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive feedback and for identifying a key area where the manuscript can be strengthened. We address the single major comment below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Observations / data processing (methods section describing the search pipeline)] The abstract and methods description provide no quantitative false-positive rate for the commensal pipeline, no blind-injection recovery statistics, and no explicit tests against known Parkes RFI families. These details are load-bearing for the central claim that the four signals are genuine astrophysical FRBs rather than terrestrial interference or artifacts.

    Authors: We agree that these quantitative assessments are important for rigorously supporting the astrophysical nature of the detections. The original manuscript did not include them explicitly. In the revised version we will add a new subsection to the Methods section that reports: (i) the false-positive rate estimated from the total number of independent trials performed across the dataset together with the rate of candidate events in off-beam and off-pulse data; (ii) results from blind-injection tests in which synthetic dispersed pulses with a range of S/N, DM and widths were inserted into the raw filterbank files and the recovery efficiency of the pipeline was measured; and (iii) direct comparisons of the four events against the known families of Parkes RFI (e.g., perytons, narrow-band radar, and persistent narrow-band interference), showing that none of the detected bursts share the temporal, spectral or polarization properties of these contaminants. These additions will be accompanied by a short table or figure summarizing the statistics. revision: yes

Circularity Check

0 steps flagged

No circularity: pure observational discovery report with no derivations or fitted predictions

full rationale

The paper is an empirical report of four FRB detections during commensal PPTA observations. It contains no equations, no fitted parameters, no model predictions, and no derivation chain. Claims rest on direct telescope data, polarization measurements, and DM consistency, which are external to any self-referential construction. No self-citation load-bearing steps exist because there is no mathematical argument to reduce. This matches the default expectation for non-circular observational papers.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a pure observational discovery paper; no free parameters, mathematical axioms, or invented physical entities are introduced.

pith-pipeline@v0.9.0 · 5801 in / 966 out tokens · 45356 ms · 2026-05-25T17:22:08.199544+00:00 · methodology

discussion (0)

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Reference graph

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