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arxiv: 2606.10538 · v1 · pith:KGPD4P46new · submitted 2026-06-09 · 🌌 astro-ph.HE · astro-ph.GA

Updating the PATH framework with FRB host galaxy models

C. W. James , N. Loudas , M. Woodland , B. C. Andersen , J. X. Prochaska , J.L. Hoffmann , L. Marnoch , S. D. Ryder This is my paper

Pith reviewed 2026-06-27 12:35 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords fast radio burstsFRB host galaxiesPATH frameworkBayesian associationmagnitude distributiondispersion measureASKAP ICS
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The pith

Incorporating host magnitude priors into PATH increases confidence in all ASKAP FRB host identifications and shows hosts are fainter than star-formation-weighted models predict.

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

This paper extends the Probabilistic Association of Transients to their Hosts framework by adding three new prior models for the apparent r-band magnitude distribution of FRB host galaxies as a function of redshift. These models are combined with redshift expectations derived from dispersion measure and their parameters are fitted to host galaxy candidates for 32 ASKAP ICS FRBs. The updated method produces higher probabilities for the most likely hosts in every case examined. It also confirms that the observed host magnitude distribution at low redshift is fainter than a star-formation-weighted distribution and even more discrepant from a mass-weighted distribution.

Core claim

By developing three models for the apparent r-band magnitude distribution P(m_r|z) based on an FRB's expected host galaxy redshift and fitting their parameters to 32 ASKAP ICS FRB candidates, the updated PATH framework yields increased confidence in the most probable hosts for all such FRBs. All three models predict similar magnitude distributions at low redshift, confirming that the true FRB host distribution is fainter than expected for a star-formation-weighted distribution (p-value of 0.12%) while a mass-weighted distribution provides a worse fit (p-value of 10^{-9}).

What carries the argument

Three models for the apparent r-band magnitude distribution P(m_r|z) based on an FRB's expected host galaxy redshift, fitted to 32 ASKAP candidates and combined with P(z|DM).

If this is right

  • All ASKAP ICS FRB host galaxies receive increased association probabilities under the new priors.
  • The three models produce similar predicted host magnitude distributions at low redshift (z ~ 0.1).
  • The observed FRB host distribution is fainter than a star-formation-weighted model at the 0.12% level.
  • A mass-weighted host distribution fits the data even more poorly, at the 10^{-9} level.
  • Additional FRBs at z > 0.5 would help distinguish between the three magnitude models.

Where Pith is reading between the lines

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

  • The results suggest FRB progenitors may occur preferentially in lower-luminosity galaxies than star-formation weighting would imply.
  • Incorporating additional host properties such as metallicity could further tighten the priors in future extensions.
  • More reliable host associations would reduce systematic errors when using FRB dispersion measures to map the cosmic ionized gas distribution.

Load-bearing premise

The three models for the apparent r-band magnitude distribution accurately represent the underlying FRB host population when their parameters are fitted to the 32 ASKAP ICS FRB candidates.

What would settle it

A sample of FRBs with secure hosts at redshifts above 0.5, where the three models make different predictions for the magnitude distribution, would test whether the priors match the true population.

Figures

Figures reproduced from arXiv: 2606.10538 by B. C. Andersen, C. W. James, J.L. Hoffmann, J. X. Prochaska, L. Marnoch, M. Woodland, N. Loudas, S. D. Ryder.

Figure 1
Figure 1. Figure 1: Probability distributions P(mr|z) at z = 0.5 for various values of f sfr using the Loudas25 model. Our second model is based on GALFRBa , a package de￾veloped by Loudas et al. (2025) to generate galaxy popula￾tions that trace various physical quantities, such as SFR and/or M∗ , while accounting for redshift evolution. GALFRB is built on the probability density function ρ(SFR, M∗ , z), given by the trained … view at source ↗
Figure 2
Figure 2. Figure 2: Galaxy number density per magnitude bin identified in images about the nominal positions of CRAFT/ICS FRBs. Also shown are the galaxy densities from Driver et al. (2016). compared to expectations from field galaxies, the observations become incomplete beyond magnitude mr = 25, with the dimmest identifiable galaxy being at mr = 27. The excess of galaxies in the 18 ≤ mr ≤ 20 range is due to mis-classified st… view at source ↗
Figure 4
Figure 4. Figure 4: Histograms of VLT/FORS2 colours for ASKAP/ICS FRB hosts identified by Shannon et al. (2025). The VLT/FORS2 photometry used in this work was taken predominantly in either g and I bands, or R band [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Fitted distribution of best-fit absolute magnitudes Mr for the Naive model developed in this work, showing the model parameters, and the interpolation between them. In the case of the Naive model, we find that our numerical procedure produces a peak in P(Mr) near Mr = −21. Our pre￾liminary investigation (see Appendix 1) found no probability of there being an excess population of very dim (Mr ≥ −15) or very… view at source ↗
Figure 6
Figure 6. Figure 6: Fitted log likelihood of the Naive model (this work) as a function of k, log10 L(k), while holding other model parameters fixed at their values given in [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: Cumulative observed (posterior) and prior distributions in P(mr) for ASKAP/CRAFT ICS FRBs according to the Loudas25 model, with f sfr = 0 (mass￾weighted), f sfr = 1 (SFR-weighted), and f sfr = 3.0 (best fit); the Naive model developed in this work; and the Marnoch23 model. See text for explanation of calculation. distributions C(mr) predicted by the models are calculated as C(mr) = N −1 FRB N XFRB i=1 Z mr… view at source ↗
Figure 7
Figure 7. Figure 7: Fitted log likelihood of the Loudas25 model as a function of f sfr, log10 L(f sfr). In the case of the Loudas25 model, we show L(f sfr) in [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 10
Figure 10. Figure 10: Change in posterior confidence ∆P(Oi |x, NO) as a function of posterior values P(Oi |x, NO) calculated from the original PATH methodology, as per the Marnoch23, Loudas25, and Naive models with best-fit values. Positive values indicate increased confidence. In [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Estimated probabilities, P(U|DMEG), of the true host being unseen in an optical image as a function of extragalactic DM, DMEG, for each of the three host models developed in this work, and three optical follow-up sensitivities, shown for: (a) ASKAP ICS observations at 892 MHz; (b) CHIME observations at a declination of δ = 60◦; (c) MeerKAT coherent detection; and (d) DSA-110 [PITH_FULL_IMAGE:figures/full… view at source ↗
Figure 12
Figure 12. Figure 12: Mean, and 67% (±1σ) and 95% confidence (±2σ) intervals, of the FRB r-band host galaxy magnitude distribution, mr, as a function of redshift, using Marnoch23, Loudas25, and Naive models. Also shown are observed magnitudes for probable FRB host galaxies (measured using a variety of filters) for FRBs detected in CRAFT ICS (Shannon et al. 2025), MeerTRAP coherent (Pastor-Marazuela et al. 2026), and DSA (Sharm… view at source ↗
Figure 13
Figure 13. Figure 13: Best fitting distributions P(Mr) found for various combinations of Nbins, Mmin r , and Mmax r . preserves the locations of the original bins in magnitude space, i.e., it produces a nested model. Doing so shows that the increased likelihood with increasing bins is negligible, and would occur at least 96% of the time under the null hypothesis that the 6-bin model correctly describes the data. While Wilks’ t… view at source ↗
read the original abstract

Over a hundred fast radio burst (FRB) host galaxies have now been identified, enabling both comparisons of host redshift with FRB dispersion measure to study the cosmological distribution of ionised gas, and analyses of host properties in order to identify FRB progenitors. The standard method for determining the most likely FRB host galaxy in an optical image is the Bayesian framework Probabilistic Association of Transients to their Hosts (PATH), which accounts for uncertainties in the radio localisation, and simplified prior distributions on the host being observable. In this work we extend PATH, incorporating physically-motivated priors that are based on expectations about FRB host galaxy magnitudes. We develop three different models for the apparent r-band magnitude distribution based on an FRB's expected host galaxy redshift, $P(m_r|z)$ and combine these with expectations for redshift based on an FRB's dispersion measure, $P(z|DM)$. We fit the parameters of these prior models using host galaxy candidates for 32 FRBs detected by the Australian SKA Pathfinder (ASKAP) in incoherent sum (ICS) mode by the Commensal Real-time ASKAP Fast Transients (CRAFT) survey. Employing PATH with the new priors on the host magnitudes, we find increased confidence in the most probable hosts of all ASKAP ICS FRB host galaxies. All three models predict similar distributions of FRB host magnitudes at low redshift $(z \sim 0.1)$, and we confirm previous results that the true FRB host galaxy distribution is fainter than expected for a star-formation-weighted distribution (p-value of 0.12%). However, a mass-weighted distribution provides an even worse fit (p-value of $10^{-9}$). Tests against more FRBs in the $z > 0.5$ range, where the models differ, and extensions of the models to account for e.g. host metallicity, may help to resolve these uncertainties in the FRB host distribution.

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

2 major / 1 minor

Summary. The manuscript updates the Probabilistic Association of Transients to their Hosts (PATH) framework by introducing three new models for the apparent r-band magnitude distribution P(m_r|z) of FRB host galaxies. These models are fitted to the host galaxy candidates associated with 32 ASKAP incoherent sum (ICS) FRBs from the CRAFT survey. When the updated priors are applied back to these same FRBs, the paper reports increased confidence in the most probable host identifications for all of them. Additionally, the resulting host magnitude distribution is compared to star-formation-weighted and mass-weighted expectations, yielding p-values of 0.12% and 10^{-9}, respectively, suggesting FRB hosts are fainter than both but closer to the former.

Significance. If the priors prove robust on independent data, incorporating magnitude-based priors into PATH would improve the reliability of FRB host associations, directly aiding progenitor studies and cosmological analyses that rely on accurate redshifts and host properties. The explicit reporting of p-values for the magnitude distribution comparisons is a strength, providing quantitative grounding for claims about the FRB host population relative to star-formation and stellar-mass weighting.

major comments (2)
  1. [Abstract and model-fitting description] Abstract and the section describing the fitting of the three P(m_r|z) models: the model parameters are fitted directly to the host-galaxy candidates of the identical 32 ASKAP ICS FRBs that are later used both to demonstrate increased association confidence under the new priors and to construct the empirical magnitude histogram for the p-value tests against star-formation-weighted and mass-weighted distributions. Because the fitting sample and evaluation sample coincide, the reported gains in host probability and the statistical comparisons are not independent validations and are vulnerable to in-sample overfitting.
  2. [Abstract] Abstract: the claim that the new priors increase confidence for all ASKAP ICS hosts and enable a robust comparison to reference distributions rests on the assumption that the fitted P(m_r|z) models accurately represent the underlying population; no cross-validation, hold-out sample, or external catalog test is described to support this assumption.
minor comments (1)
  1. [Abstract] The abstract would benefit from a brief statement of the redshift range over which the three models are stated to be similar versus where they diverge, to clarify the domain of the reported conclusions.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which highlight an important limitation in our analysis. We agree that the use of the same sample for model fitting and subsequent evaluation means the reported improvements are not independent validations. We have revised the manuscript to explicitly acknowledge this and to moderate claims accordingly.

read point-by-point responses

  1. Referee: [Abstract and model-fitting description] Abstract and the section describing the fitting of the three P(m_r|z) models: the model parameters are fitted directly to the host-galaxy candidates of the identical 32 ASKAP ICS FRBs that are later used both to demonstrate increased association confidence under the new priors and to construct the empirical magnitude histogram for the p-value tests against star-formation-weighted and mass-weighted distributions. Because the fitting sample and evaluation sample coincide, the reported gains in host probability and the statistical comparisons are not independent validations and are vulnerable to in-sample overfitting.

    Authors: We agree that fitting the P(m_r|z) parameters to the 32 ASKAP ICS FRBs and then applying the resulting priors back to the same events means the reported gains in association confidence and the p-value comparisons are in-sample results rather than independent validations. This approach was adopted because the current sample of securely associated FRB hosts remains small. In the revised manuscript we have updated the abstract and the model-fitting section to state explicitly that the confidence increases are demonstrated on the fitting sample, and we have added a paragraph in the discussion noting the risk of overfitting and the desirability of future validation on independent data sets. revision: yes

  2. Referee: [Abstract] Abstract: the claim that the new priors increase confidence for all ASKAP ICS hosts and enable a robust comparison to reference distributions rests on the assumption that the fitted P(m_r|z) models accurately represent the underlying population; no cross-validation, hold-out sample, or external catalog test is described to support this assumption.

    Authors: We acknowledge that no cross-validation, hold-out testing, or external catalog comparison was performed. With only 32 events the sample is too small to reserve a meaningful hold-out set without compromising the model fits. The revised abstract and discussion now include an explicit caveat that the models have not been tested on independent data and that additional FRBs (especially at z > 0.5) will be required to assess whether the priors generalise. We retain the claim that the new priors increase confidence within the current sample, but we no longer describe the comparison to reference distributions as fully robust without further validation. revision: yes

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central results rest on three magnitude-distribution models whose parameters are calibrated to the 32 ASKAP FRBs; the framework also inherits standard FRB assumptions about DM-to-redshift conversion.

free parameters (1)
  • parameters of the three P(m_r|z) models
    Fitted to host galaxy candidates for the 32 ASKAP ICS FRBs to define the new priors
axioms (2)
  • domain assumption An FRB's dispersion measure supplies a usable prior P(z|DM) on host redshift
    Explicitly combined with the new P(m_r|z) to form the updated PATH prior
  • domain assumption FRB host galaxies follow the modeled apparent-magnitude distribution at their redshift
    Foundation for the three new prior models introduced in the work

pith-pipeline@v0.9.1-grok · 5925 in / 1662 out tokens · 28291 ms · 2026-06-27T12:35:10.441411+00:00 · methodology

discussion (0)

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