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arxiv: 1906.11476 · v1 · pith:QG3GUBZUnew · submitted 2019-06-27 · 🌌 astro-ph.HE · astro-ph.CO

A single fast radio burst localized to a massive galaxy at cosmological distance

K. W. Bannister , A. T. Deller , C. Phillips , J.-P. Macquart , J. X. Prochaska , N. Tejos , S. D. Ryder , E. M. Sadler
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R. M. Shannon S. Simha C. K. Day M. McQuinn F. O. North-Hickey S. Bhandari W. R. Arcus V. N. Bennert J. Burchett M. Bouwhuis R. Dodson R. D. Ekers W. Farah C. Flynn C. W. James M. Kerr E. Lenc E. K. Mahony J. O'Meara S. Os{\l}owski H. Qiu T. Treu V. U T. J. Bateman D. C.-J. Bock R. J. Bolton A. Brown J. D. Bunton A. P. Chippendale F. R. Cooray T. Cornwell N. Gupta D. B. Hayman M. Kesteven B. S. Koribalski A. Macleod N. M. McClure-Griffiths S. Neuhold R. P. Norris M. A. Pilawa R.-Y. Qiao J. Reynolds D. N. Roxby T. W. Shimwell M. A. Voronkov C. D. Wilson
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Pith reviewed 2026-05-25 14:48 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.CO
keywords fast radio burstFRB 180924host galaxydispersion measureintergalactic mediumcosmic webradio interferometrybaryonic matter
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The pith

A non-repeating fast radio burst is localized to a massive galaxy at redshift 0.3214 with electron column density matching intergalactic medium models.

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

The paper reports the interferometric localization of the single-pulse FRB 180924 to a position 4 kpc from the center of a luminous galaxy at redshift 0.3214. The burst shows no repetition and differs in properties from the only previously localized FRB. Its integrated electron column density aligns closely with predictions from intergalactic medium models. A sympathetic reader would care because this indicates that some FRBs can serve as clean probes of the baryonic component of the cosmic web without major host-galaxy contamination.

Core claim

The interferometric localization places FRB 180924 4 kpc from the center of a luminous galaxy at redshift 0.3214. The burst has not been observed to repeat. The properties of the burst and its host are markedly different from the only other accurately localized FRB source. The integrated electron column density along the line of sight closely matches models of the intergalactic medium, indicating that some FRBs are clean probes of the baryonic component of the cosmic web.

What carries the argument

Interferometric localization of the burst position to associate it with a specific host galaxy, followed by direct comparison of the observed dispersion measure to intergalactic medium electron-density models.

If this is right

  • Non-repeating FRBs can originate in massive galaxies at cosmological distances.
  • The dispersion measure of at least some FRBs is dominated by the intergalactic medium.
  • FRBs can be used as direct tracers of the baryonic matter distributed in the cosmic web.
  • Host-galaxy properties of FRBs are not uniform across all detected events.

Where Pith is reading between the lines

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

  • A statistical sample of similarly localized FRBs could map the three-dimensional distribution of baryons on large scales.
  • This technique offers an independent route to addressing the missing-baryons problem by measuring the total electron column density along many sight lines.
  • Repeated application would allow tests of how galaxy feedback and large-scale structure affect the observed dispersion measures.

Load-bearing premise

The localization is accurate enough to identify the correct host galaxy unambiguously and the measured dispersion measure receives negligible contribution from the host galaxy's interstellar or circumgalactic medium.

What would settle it

A higher-resolution observation that places the burst outside the identified galaxy or additional data showing that the host galaxy contributes a large fraction of the total dispersion measure.

Figures

Figures reproduced from arXiv: 1906.11476 by A. Brown, A. Macleod, A. P. Chippendale, A. T. Deller, B. S. Koribalski, C. D. Wilson, C. Flynn, C. K. Day, C. Phillips, C. W. James, D. B. Hayman, D. C.-J. Bock, D. N. Roxby, E. K. Mahony, E. Lenc, E. M. Sadler, F. O. North-Hickey, F. R. Cooray, H. Qiu, J. Burchett, J. D. Bunton, J. O'Meara, J.-P. Macquart, J. Reynolds, J. X. Prochaska, K. W. Bannister, M. A. Pilawa, M. A. Voronkov, M. Bouwhuis, M. Kerr, M. Kesteven, M. McQuinn, N. Gupta, N. M. McClure-Griffiths, N. Tejos, R. D. Ekers, R. Dodson, R. J. Bolton, R. M. Shannon, R. P. Norris, R.-Y. Qiao, S. Bhandari, S. D. Ryder, S. Neuhold, S. Os{\l}owski, S. Simha, T. Cornwell, T. J. Bateman, T. Treu, T. W. Shimwell, V. N. Bennert, V. U, W. Farah, W. R. Arcus.

Figure 1
Figure 1. Figure 1: Spectral and polarimetric properties of FRB 180924. (A) Integrated pulse pro￾file. (B) Burst discovery dynamic spectrum, dedispersed by the measured dispersion measure (DM=361.42 pc cm−3 ). The white bands are regions flagged due to radio-frequency interfer￾ence in the high time resolution data. (C) Burst fluence spectrum (Eν) averaged over the pulse. For this lower time resolution spectrum we partially mi… view at source ↗
Figure 2
Figure 2. Figure 2: Panel A: Host galaxy of FRB 180924. (A) VLT/FORS2 g 0 -band image showing the host galaxy of FRB 180924, labeled A. The burst location uncertainty is shown by the black circle. Two background faint background galaxies, labeled B and C, can be seen to the right and upper left are also visible (see supplementary text). 11 [PITH_FULL_IMAGE:figures/full_fig_p011_2.png] view at source ↗
Figure 2
Figure 2. Figure 2: Panels B-D: Host galaxy of FRB 180924. (B) Keck Cosmic Web Imager (KCWI) spectrum (17) of the FRB 180924 host, showing the detection of forbidden-line ionized oxygen emission [OII], and Calcium absorption which set the FRB redshift z = 0.3214. fλ is relative flux. The oxygen emission is attributed to gas ionized by a hard ionizing spectrum. The ab￾sorption lines are stellar. (C) Section of Gemini Multi Obj… view at source ↗
Figure 3
Figure 3. Figure 3: Spectrophotometric properties of FRB 180924 host galaxy. (A) photometric mea￾surements of the host galaxy. Spectral energy distribution (SED) modeling yields an estimated stellar mass of M∗ = 2.2 × 1010M dominated by a modestly reddened, old stellar population (tage > 4 Gyr). (B-D) Nebular line emission of the FRB 180924 host from the VLT/MUSE data cube. Penalised Pixel Fitting (pPXF) models fitted to thes… view at source ↗
Figure 4
Figure 4. Figure 4: Diagnostic plot for characterizing emission line galaxies. The green points show the distribution of ≈ 75, 000 nearby (0.02 < z < 0.4) emission-line galaxies from the Sloan Digital Sky survey, restricted to have S/N > 5. The intensity scaling is logarithmic to accentuate regions away from the dominant, star-forming locus. Black lines separate the star-forming galaxies (solid; (25)) from sources dominated b… view at source ↗
read the original abstract

Fast Radio Bursts (FRBs) are brief radio emissions from distant astronomical sources. Some are known to repeat, but most are single bursts. Non-repeating FRB observations have had insufficient positional accuracy to localize them to an individual host galaxy. We report the interferometric localization of the single pulse FRB 180924 to a position 4 kpc from the center of a luminous galaxy at redshift 0.3214. The burst has not been observed to repeat. The properties of the burst and its host are markedly different from the only other accurately localized FRB source. The integrated electron column density along the line of sight closely matches models of the intergalactic medium, indicating that some FRBs are clean probes of the baryonic component of the cosmic web.

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

0 major / 2 minor

Summary. The manuscript reports the interferometric localization of the single-pulse FRB 180924 to a position 4 kpc from the center of a luminous galaxy at redshift 0.3214. The burst has not repeated, and its properties and host differ from the only other accurately localized FRB. The integrated electron column density (DM) along the line of sight closely matches models of the intergalactic medium, indicating that some FRBs are clean probes of the baryonic component of the cosmic web.

Significance. If the localization precision and DM decomposition hold, this is a significant result: it supplies the first precise host-galaxy association for a non-repeating FRB at cosmological distance and demonstrates that the observed DM can be accounted for by the IGM with negligible host contribution. The manuscript provides the explicit position, redshift, DM value, and direct comparison to IGM predictions, enabling verification. This strengthens the case for using FRBs as cosmological tools and highlights source diversity relative to the repeating FRB 121102.

minor comments (2)
  1. [Abstract] Abstract: the abstract states the DM match but omits the numerical DM value, redshift, and localization uncertainty; including these would allow immediate assessment of the central claim.
  2. [Discussion] The host-galaxy DM contribution modeling should be expanded with an explicit upper limit or uncertainty budget to confirm it is negligible within the quoted errors on the IGM comparison.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their supportive summary and recommendation of minor revision. No specific major comments were provided in the report, so we have no individual points to address point-by-point. We will proceed with minor revisions to the manuscript as appropriate.

Circularity Check

0 steps flagged

No significant circularity

full rationale

The paper is an observational report of FRB localization, redshift, and DM measurement, followed by direct comparison to pre-existing IGM models. No equations, fitted parameters, or derivations appear in the provided text. The central claim is an empirical match, not a prediction generated from inputs defined within the paper. No self-citations, ansatzes, or uniqueness theorems are invoked as load-bearing steps. This is a standard observational result with independent external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Review performed on abstract only; no explicit free parameters, invented entities, or ad-hoc axioms are stated in the provided text. The work relies on standard radio-astronomy localization techniques and existing IGM models.

axioms (1)
  • domain assumption Interferometric localization can achieve sufficient accuracy to associate an FRB with a galaxy at cosmological distance
    Invoked to support the 4 kpc offset claim.

pith-pipeline@v0.9.0 · 5978 in / 1124 out tokens · 31130 ms · 2026-05-25T14:48:26.832973+00:00 · methodology

discussion (0)

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The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
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Forward citations

Cited by 3 Pith papers

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Reference graph

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