CHIME/Slow overview and pilot survey: A new backend to search for second-duration radio transients with the CHIME telescope

Afrokk Khan; Arvind Balasubramanian; B. M. Gaensler; Bradley W. Meyers; Charanjot Brar; Chia Min Tan; David Spear; Emmanuel Fonseca; Fengqiu Adam Dong; Ingrid Stairs

REVIEW 3 major objections 6 minor 1 cited by

A new CHIME backend finds seconds-long radio bursts that the standard search misses, and a pilot survey estimates their all-sky rate at 184 to 4556 bursts per sky per day.

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2026-08-02 23:42 UTC pith:52XMXX56

load-bearing objection Solid instrument paper with two new detections the standard CHIME/FRB search missed; the all-sky rate is a one-event, highly model-dependent estimate that should not be quoted as tight. the 3 major comments →

arxiv 2602.12793 v2 pith:52XMXX56 submitted 2026-02-13 astro-ph.IM astro-ph.HE

CHIME/Slow overview and pilot survey: A new backend to search for second-duration radio transients with the CHIME telescope

Sujay Mate , Kevin Luke , Yash Bhusare , Arvind Balasubramanian , Ziggy Pleunis , Paul Scholz , Shriharsh P. Tendulkar , Mohit Bhardwaj

show 18 more authors

Charanjot Brar Fengqiu Adam Dong Emmanuel Fonseca B. M. Gaensler Jason Hessels Jeff Huang Naman Jain Ronniy C. Joseph Victoria M. Kaspi Afrokk Khan Robert Main Bradley W. Meyers Nikola Milutinovic Kenzie Nimmo Kaitlyn Shin David Spear Ingrid Stairs Chia Min Tan

This is my paper

classification astro-ph.IM astro-ph.HE

keywords fast radio burstsradio transientslong-duration radio burstsCHIMEtransient searchpulse widthscatteringall-sky rate

verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper argues that CHIME/Slow, a new search backend for the CHIME telescope, recovers wide and highly scattered fast radio bursts that the standard CHIME/FRB search is biased against. Testing a prototype on 17 days of archival data, it detected nine bursts: a new non-repeating FRB and eight bursts from the repeater FRB 20220912A, two of which CHIME/FRB missed. From these detections and injection-based completeness measurements, the paper estimates the all-sky rate of transients with pulse widths between 16 ms and 5 s, fluence above 5 Jy ms, and at 600 MHz to be 184–4556 bursts sky^-1 day^-1. If the estimate is right, current millisecond-tuned surveys are missing a sizable population of wide or scattered radio transients.

Core claim

CHIME/Slow is a pipeline that downsamples the CHIME/FRB intensity stream and searches it with parameters optimized for long-duration transients, and the pilot survey demonstrates that this recovers bursts invisible to the standard search. The central result is that in 17 days of data covering roughly 13 square degrees at a time, the pipeline found nine bursts, including FRB 20230204C — one of the most highly scattered FRBs seen by CHIME — and two bursts from FRB 20220912A that CHIME/FRB did not detect. Using the single one-off detection and a power-law population model with marginalization over width dependence, the paper derives an all-sky rate of 184–4556 bursts sky^-1 day^-1 for transient

What carries the argument

The pipeline: a 3-bit intensity data stream from CHIME/FRB is downsampled to 16-ms, 128-ms, and 512-ms filterbanks; each is searched with PRESTO single-pulse search with RFI cleaning tuned for long-duration events; events are clustered in DM-time with HDBSCAN and classified with FETCH. The rate estimate uses a population model R(F,w) ∝ F^(α−1) w^β with α fixed to −1.5 and β marginalized over −1, −2, −3, combined with an exposure model cut at 10% of peak beam sensitivity and a constant completeness of 0.8, fit via a binned Poisson likelihood in an MCMC.

Load-bearing premise

The rate estimate assumes the one-off detection FRB 20230204C is representative of a single underlying population that is Euclidean in fluence (α = −1.5) and has a constant 80% completeness across all widths, without propagating the systematic uncertainty in these choices.

What would settle it

A dedicated month-long real-time CHIME/Slow survey with the same thresholds: if the number of one-off bursts detected is inconsistent with the Poisson expectation from the 184–4556 rate (e.g., zero bursts or dozens), then the population model or completeness estimate is wrong. Alternatively, a direct measurement of the width distribution of bursts from a larger sample can falsify the fixed α and β assumptions.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

If this is right

The standard CHIME/FRB search misses a measurable number of wide or highly scattered bursts; CHIME/Slow detects them.
The all-sky rate of 184–4556 bursts sky^-1 day^-1 implies that large-field, millisecond-tuned surveys may be incomplete by a factor that could show up in comparisons with wider-width searches.
The two repeater bursts detected only by CHIME/Slow show that even a known active repeater produces bursts that standard searches overlook, so burst-rate estimates for repeaters may need upward revision.
The new non-repeating source FRB 20230204C, with a scattering timescale of about 98 ms, demonstrates that at least some FRBs are heavily scattered at 400 MHz, informing models of local environments.
Once the real-time CHIME/Slow backend is fully operational, it can deliver low-latency alerts for these events, enabling follow-up of a population currently invisible to FRB searches.

Where Pith is reading between the lines

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

If the 184–4556 rate holds, then across the whole sky several hundred to a few thousand wide or scattered bursts occur each day above 5 Jy ms, comparable to the known FRB rate — suggesting that wide bursts are not rare outliers but an integral part of the FRB phenomenon.
The width-dependence parameter β is only marginalized over three discrete values; a dedicated measurement of the width distribution from a larger sample could break degeneracies and either widen or narrow the credible interval.
A natural testable extension: the same 16 ms–5 s search applied to data from other wide-field instruments (e.g., ASKAP/CRACO or uGMRT) should find similar bursts if the population is truly ubiquitous; a null result there would point to CHIME-specific sensitivity effects.
Because completeness was measured only on a limited dataset and set constant at 0.8, a more thorough injection campaign across different RFI conditions and sky positions could revise the rate, especially if completeness drops at long widths.

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

Solid instrument paper with two new detections the standard CHIME/FRB search missed; the all-sky rate is a one-event, highly model-dependent estimate that should not be quoted as tight.

read the letter

Short version: this is a solid instrument paper showing the CHIME/Slow prototype works and finds bursts the standard CHIME/FRB search misses. The headline all-sky rate, though, is a one-detection estimate with a few modeling choices—fixed α = −1.5, β marginalized over three values, constant completeness 0.8, and a 10%-of-peak sensitivity cutoff—whose systematic effects are not propagated into the quoted credible interval. Treat the rate as a broad hint, not a measurement.

What’s new: two FRB 20220912A bursts seen only by CHIME/Slow, and FRB 20230204C, a highly scattered one-off burst detected in the CHIME/FRB sidelobe with a narrower width in that search. That is genuinely interesting for the scattered-population hypothesis. The pipeline description is detailed, the injection/completeness study is careful, and the paper is unusually transparent about its limitations—constant completeness, limited injection sampling, the 10% cutoff.

The soft spot is the rate. The stress-test note about the exposure function is right: they collapse the S-dependent exposure into a single step at 10% sensitivity, but the detected burst itself requires a relative sensitivity of roughly 0.4 from Eq. A2, so using the ≥10% footprint overcounts its effective exposure. That by itself shifts the rate normalization; the fixed α does too. They also treat completeness as a flat 0.8, which is fine for a conservative lower bound but not as a central value. The 184–4556 sky⁻¹ day⁻¹ interval is a Poisson posterior for one particular model, not a robust population measurement. The paper says this openly, but the abstract and Figure 6 still present it as the CHIME/Slow rate, so a reader could over-interpret it.

Nothing circular here; the rate is an explicit fit to one event with external anchors from CHIME/FRB. The burst properties and the pipeline performance are the real contribution.

This paper deserves a serious referee—the instrumentation and the detections are worth publishing. The rate section needs revision: either propagate the systematic choices (α, β, completeness, exposure step) or present the interval as conditional on them. I’d suggest the authors run a few sensitivity tests and report the rate under alternative assumptions, or clearly label it as model-dependent.

Referee Report

3 major / 6 minor

Summary. The paper describes CHIME/Slow, a new backend for the CHIME telescope designed to search for radio transients with pulse widths between 16 ms and 5 s. The prototype pipeline, built on PRESTO, HDBSCAN, and FETCH, was applied to 17 days of archival data covering an instantaneous FoV of about 13 deg^2. Nine bursts were detected: one new non-repeating FRB (FRB 20230204C) with a scattering timescale of ~98 ms, and eight bursts from the repeater FRB 20220912A, two of which were not detected by CHIME/FRB. The paper reports an all-sky rate of 184–4556 bursts sky^-1 day^-1 (95% credible region) for transients with fluence >5 Jy ms and widths 16 ms–5 s at 600 MHz, based on the single non-repeater detection and a parameterized population model. It also presents injection-based completeness measurements and outlines plans for a real-time backend.

Significance. The instrument description and the pilot detections are valuable: CHIME/Slow demonstrates that a substantial fraction of wide or highly scattered bursts are missed by standard CHIME/FRB searches, and the two bursts recovered only in CHIME/Slow are concrete evidence of this capability. The completeness study is carefully designed and the authors are generally explicit about limitations. However, the headline all-sky rate is an extrapolation from one detection and is conditional on several unpropagated modeling choices, so the quoted 95% credible interval should be interpreted as the result of one model rather than a robust measurement. If the systematic uncertainties are addressed, the paper would make a solid contribution to the emerging study of second-duration radio transients.

major comments (3)

[§5, Eq. (2)] The all-sky rate is derived from a single detection, yet the fluence power-law index α is fixed to -1.5, adopted from CHIME/FRB Catalog 1. That catalog is restricted to bursts with scattering times <10 ms and widths <100 ms, so applying its α to the 16 ms–5 s population is an unsupported prior. With one event, α is essentially unconstrained. Changing α from -1.5 to -1.0 or -2.0 changes the fluence integral ∫_5^100 F^(α−1) dF by factors of roughly 3, which would shift the posterior substantially relative to the quoted interval. The paper should either marginalize over a sensible prior on α or present the rate as a function of α.
[§5 and Appendix A, Eq. (A1)–(A2)] The exposure E(S) is defined as the cumulative sky area with relative sensitivity above S, where S = S/N_thr / S/N_max. The analysis replaces E(S_req) with a step function at 10% of peak sensitivity for all bursts. This is not equivalent to Eq. (A1). For the detected burst FRB 20230204C, Eq. (A2) gives S/N_max ≈ 24, so S_req ≈ 0.4 and the correct exposure is E(0.4), which is smaller than E(0.1) used by the step. For a bright 100 Jy ms burst, S_req can be <0.1, so E(0.1) undercounts the exposure. Thus the step simultaneously overestimates exposure for moderate-S_req bursts and underestimates it for bright bursts, biasing the inferred rate in opposite directions. The systematic effect should be quantified by computing E(S_req) directly or by demonstrating insensitivity to the threshold.
[§5, completeness] The completeness fraction is set to a constant 0.8 for all widths and S/N values above threshold. Figure 4 suggests that for widths ≳1 s the completeness at S/N=10 may be lower, and the injection data are limited (about 4 hours over 10 days in 64 beams). The statement that this choice 'will only lead to an underprediction of the all-sky rate' is logically incorrect: if the true completeness is higher than 0.8, assuming 0.8 lowers the expected count and hence raises the fitted R0; if the true completeness is lower, R0 is lowered. The direction of bias is therefore not guaranteed. A completeness function C(w) with associated uncertainties, or at least a sensitivity test with different C(w), is needed to support the quoted credible interval.

minor comments (6)

[§2.2.1] The rfifind parameters list '12-ms' for one of the time samplings; this should be '128-ms'.
[Figure 4] The completeness curves for CHIME/FRB and CHIME/Slow use different width bins; the reader should be told whether the comparison is at matched total (intrinsic+scattering) widths.
[Eq. (A2)] The symbols w and w_b are easy to confuse. Define explicitly, e.g., w is the intrinsic width including scattering, and w_b is the broadened width including sampling and DM smearing.
[§5] When marginalizing over β, the paper does not state whether equal prior weights are used for the three values. This should be made explicit.
[§6] Typo: 'curicial' should be 'crucial'.
[Figure 5] The red dashed line marking the CHIME/FRB Catalog 1 rate is not labeled inside the plot; please label it in the figure for clarity.

Circularity Check

0 steps flagged

No load-bearing circularity: the all-sky rate is a one-event Poisson fit under stated assumptions, with only minor same-collaboration inheritance from CHIME/FRB products.

full rationale

The paper's central quantitative claim, the all-sky rate of 184–4556 bursts sky^-1 day^-1, is obtained by fitting the single non-repeating detection FRB 20230204C with the population model of Eq. (2), a binned Poisson likelihood (Eq. 3), and an exposure/completeness model computed from injections and the CHIME/FRB beam model. This is an inference from data, not a restatement of an input: the detection count enters as Nd in Eq. (3), and R0 is the free parameter being estimated. The fixed value α=−1.5, the three trial values of β, the constant completeness 0.8, and the 10%-sensitivity exposure cut are explicitly stated assumptions (Section 5 and Appendix A); their systematic uncertainty is not propagated, but that is a statistical-robustness caveat rather than a circular reduction. The self-citations to CHIME/FRB products (beam model, calibration, Catalog-1 rate) are used as external data products from a separate instrument backend; although several authors overlap, the load-bearing logic does not depend on those citations for the detection or for the rate fit. The manuscript itself flags limited injection statistics (footnote 8) and the poorly constrained width dependence (Section 6), further indicating that the quoted interval should be read as conditional on the stated model. Accordingly, no step in the derivation reduces to its own inputs by construction; the low score reflects minor same-collaboration inheritance rather than circularity.

Axiom & Free-Parameter Ledger

5 free parameters · 8 axioms · 0 invented entities

The paper does not introduce new physical entities. Its central rate estimate depends on a small set of fitted or hand-chosen quantities: R0 fitted to one detection, α and β chosen from prior/assumed population models, and completeness/sensitivity cutoffs chosen conservatively. The axioms are mostly domain assumptions inherited from CHIME/FRB analysis and the pilot-survey design; the most fragile are the single-detection Poisson anchor and the unpropagated systematic choices.

free parameters (5)

R0 (all-sky rate normalization) = 95% credible interval 184–4556 sky^-1 day^-1, marginalized over β
Fitted by MCMC/MLE to the single one-off detection FRB 20230204C using Eq. (1)–(3). This is the central reported number.
α (fluence power-law index) = -1.5
Not fitted in this paper; adopted from CHIME/FRB Catalog 1 and the Euclidean-uniform source assumption. Drives how the 5 Jy ms threshold maps to the all-sky rate.
β (width power-law index) = -1, -2, -3
Assumed values for the width distribution; the posterior for R0 is marginalized over them because one detection cannot constrain β.
Completeness fraction C(w) = 0.8 (constant)
Chosen by hand as a conservative constant from injection completeness curves (Fig. 4), rather than propagated as a function of width.
Relative sensitivity cutoff = 10% of peak beam sensitivity
Used in Appendix A to define sky area and exposure; changing this cutoff changes the exposure and therefore the inferred rate normalization.

axioms (8)

domain assumption The intrinsic population of radio transients depends only on fluence and broadened width; DM and scattering dependencies are ignored.
Stated in Section 5: 'we assume that the intrinsic model only depends on fluence and width, and ignore the dependence on other parameters.' This directly shapes Eq. (1)–(2).
domain assumption The source population is uniformly distributed in a flat Euclidean Universe, giving N(>F) ∝ F^-1.5 and α = −1.5.
Adopted from CHIME/FRB Catalog 1 in Section 5. It is load-bearing for scaling the rate to the 5 Jy ms threshold and for comparison with other surveys.
domain assumption FRB 20220912A bursts can be excluded from the all-sky rate because the repeater was hyperactive during the survey.
Section 5 states the repeater 'contributed significantly to the all-sky rate of FRBs' and is discarded, leaving one one-off detection. If repeaters contribute substantially to the 16 ms–5 s population, the quoted rate would be understated.
domain assumption Scattering index is −4 in the fitburst models.
Section 3: 'We assume scattering index of -4.' Affects the burst width and scattering timescale estimates.
domain assumption CHIME/FRB beam model and daily pulsar-based sensitivity factors accurately describe CHIME/Slow sensitivity.
Appendix A uses the CHIME/FRB beam model and daily sensitivity factor to compute the exposure; the rate is directly proportional to this exposure.
ad hoc to paper The completeness fraction can be treated as a constant 0.8 for all relevant widths and S/N values above threshold.
Footnote 8: the injection analysis was done on limited data and did not fully sample intrinsic noise; 0.8 is a conservative constant. This enters Eq. (1) directly.
domain assumption DM search range 50–3000 pc cm^-3 captures the extragalactic transient population relevant to the rate estimate.
Section 2.2.2 sets the lower DM limit to avoid Galactic sources and the upper limit by available compute; the rate is defined over this DM range.
domain assumption The default FETCH classifier, untrained on CHIME data, is adequate for separating astrophysical bursts from RFI in this analysis.
Section 2.3 footnote: 'we have not trained FETCH on CHIME data yet, and for this analysis we have used the default models.'

pith-pipeline@v1.3.0-alltime-deepseek · 17148 in / 13175 out tokens · 123882 ms · 2026-08-02T23:42:19.750779+00:00 · methodology

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read the original abstract

We present an overview of CHIME/Slow, a real-time transient search backend under development to search for second-duration radio transients using the CHIME telescope, and results obtained from a pilot survey carried out using the prototype version of the search pipeline. The prototype CHIME/Slow pipeline was tested on archival data obtained in December 2022, January 2023 and February 2023 with a total on-sky time of 17 days with an instantaneous Field of View (FoV) of $\sim$13 deg$^2$ . In this pilot survey, we detected nine bursts, one from a new non-repeating source and eight from the known hyperactive repeating source FRB 20220912A. Out of these nine bursts, two bursts from the repeater were not detected by CHIME/FRB, while the non-repeater was detected in the side-lobe of a beam in the CHIME/FRB exhibiting shorter pulse width and narrower bandwidth compared to the CHIME/Slow detection. Here we report properties of the bursts, discuss the sensitivity and completeness of the current version of the CHIME/Slow pipeline, and outline future development to improve its performance. Finally, based on these results, we report the all-sky rate (95% credible region) of radio transients with pulse widths between 16 ms to 5 s, fluence above 5 Jy ms and observing frequency of 600 MHz to be between 184 and 4556 bursts sky$^{-1}$ day$^{-1}$.

Figures

Figures reproduced from arXiv: 2602.12793 by Afrokk Khan, Arvind Balasubramanian, B. M. Gaensler, Bradley W. Meyers, Charanjot Brar, Chia Min Tan, David Spear, Emmanuel Fonseca, Fengqiu Adam Dong, Ingrid Stairs, Jason Hessels, Jeff Huang, Kaitlyn Shin, Kenzie Nimmo, Kevin Luke, Mohit Bhardwaj, Naman Jain, Nikola Milutinovic, Paul Scholz, Robert Main, Ronniy C. Joseph, Shriharsh P. Tendulkar, Sujay Mate, Victoria M. Kaspi, Yash Bhusare, Ziggy Pleunis.

**Figure 1.** Figure 1: Radio transients associated with compact objects in the pseudo-luminosity vs. pseudo pulse width parameter space. The parts of the parameter space covered by CHIME/FRB and CHIME/Slow are highlighted in light gray and light yellow colors, respectively. The green points near the FRB population show the CHIME/Slow detections from the pilot survey with the circles indicating bursts from FRB 20220912A and the t… view at source ↗

**Figure 2.** Figure 2: Overview of the CHIME/Slow pipeline: The diagram shows the major steps in the pipeline and the tools used to perform these steps. carrying out injections of wide duration bursts into test data using the built-in injection routine and recovering them back with the pipeline. The same routine was also used to estimate the completeness and sensitivity of the current version (see Section 4), and will be used t… view at source ↗

**Figure 3.** Figure 3: Dynamic spectra (“waterfall” plots), frequency-averaged time series, and time-averaged spectra of bursts detected in the CHIME/Slow pilot survey. The bursts are plotted in order of their arrival times (topocentric) from top-left to bottom-right. Each plot is corrected for the best-fit DM obtained from fitburst. The blue lines in the time-profile and spectrum plot show the best-fit frequency-averaged model … view at source ↗

**Figure 4.** Figure 4: CHIME/Slow and CHIME/FRB completeness as a function of detected S/N for different total (intrinsic + scattering) pulse widths. intrinsic model only depends on fluence and width, and ignore the dependence on other parameters. Also, we consider width as the broadened width, which includes scattering, as completeness analysis was carried out on limited data, making it difficult to disentangle the two effects … view at source ↗

**Figure 5.** Figure 5: Posterior distribution of the all-sky rate R0 in log space, marginalized over three different β values (-1, -2 and -3). The light blue and dark blue shaded regions show the 95% and 68% credible interval respectively. The red vertical dashed line shows the all-sky rate of FRBs estimated by CHIME/FRB Catalog 1 (CHIME/FRB Collaboration et al. 2021) for bursts with fluence above 5 Jy ms and scattering time be… view at source ↗

**Figure 6.** Figure 6: CHIME/Slow pilot survey all-sky rate of radio transients plotted along with the all-sky rate estimated by other surveys with center frequencies close to CHIME. All the rates are scaled to the CHIME/Slow and CHIME/FRB fluence threshold of 5 Jy ms assuming a Euclidean distribution of sources (i.e. N(> F) ∝ F −1.5 ). The data are taken from Farah et al. (2019)(UTMOST), Parent et al. (2020)(GBNCC), CHIME/FR… view at source ↗

**Figure 7.** Figure 7: Relative sensitivity as a function of sky position for all 64 beams in the CHIME/Slow data. The X and Y axes represent angles in telescope coordinates, and are aligned in the North–South and East–West directions respectively. We then assume that the total area of each sampled point is dA, which is given by A/N, where A is the total area sampled and N is the number of points sampled. To calculate the cumula… view at source ↗

**Figure 8.** Figure 8: Left: Sky area (in deg2 ) above the relative sensitivity of S. The horizontal and vertical lines mark the area above the 10% relative sensitivity threshold used for the exposure calculation. This area corresponds to 13.10 deg2 . Right: The total exposure (sky × days) above the relative sensitivity S. The horizontal and vertical lines mark the total exposure above the 10% relative sensitivity threshold. con… view at source ↗

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