Pith. sign in

REVIEW 2 major objections 4 minor 100 references

Evidence for Enhancement in the Rate of Fast Radio Bursts Toward Galaxy Clusters

T0 review · 2 major / 4 minor · reviewed 2026-08-15 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read Fast radio bursts arrive 3-sigma too often behind galaxy clusters

desk verdict A careful but flawed first measurement: the claimed 3-sigma cluster excess probably shrinks once you include the background FRBs the null simulation throws away. read the letter →

arxiv 2608.10358 v1 pith:6QDMHMIO submitted 2026-08-11 astro-ph.CO astro-ph.HE

Mawson W. Sammons , Airene Ahuja , Matt Dobbs , Zarif Kader , Evan Davies-Velie , Mohit Bhardwaj , Charanjot Brar , Amanda M. Cook
show 20 more authors
Alice P. Curtin Bryan M. Gaensler Affan Khadir Victoria M. Kaspi Afrokk Khan Adam Lanman Calvin Leung Lluis Mas-Ribas Kiyoshi W. Masui Kyle McGregor Daniele Michilli Ayush Pandhi Aaron B. Pearlman Ziggy Pleunis Sachin Pradeep E. T. Aniket Prasad J. Xavier Prochaska Paul Scholz Kaitlyn Shin Kendrick Smith
This is my paper · ORCID
classification astro-ph.COastro-ph.HE
keywords fastradioburstsgalaxyclustersgravitationallensingdispersionmeasureintraclustermediumCHIME/FRBFRBpopulationrateenhancement
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

Galaxy clusters sit in front of or around a small fraction of fast radio burst (FRB) lines of sight, and the paper argues that these special sight lines carry information that average-sky surveys wash out. It builds a statistical association score that combines how closely a burst lines up with known clusters and how likely its dispersion measure places it behind the cluster, then runs Monte Carlo simulations of a cluster-blind sky. Applying this to the arcminute-localized subset of the second CHIME/FRB baseband catalog yields 26 cluster-associated bursts where about 13 to 14 are expected by chance, a 3-sigma excess corresponding to 1.4% ± 0.4% of the catalog. The authors propose that the extra bursts come about equally from FRBs emitted by cluster member galaxies and from gravitational lensing magnification of background sources, with the member-galaxy channel sensitive to non-star-forming progenitor channels and the lensing channel sensitive to high-redshift evolution. If right, cluster-aligned FRBs become a way to constrain parts of the FRB population that are otherwise invisible to current surveys.

What carries the argument

The load-bearing object is a per-burst association score L = Σs(RA,Dec)/P(z < z_clust|DM). Σs is an all-sky map of projected cluster density built from Navarro-Frenk-White profiles with concentration c = 6, truncated and normalized by each cluster's M500 mass; the denominator uses a redshift-dispersion population model to estimate how likely a burst with a given extragalactic dispersion measure lies foreground to the most distant aligned cluster. The score is large for high-dispersion bursts closely aligned with nearby clusters. Converting L into a probability of chance coincidence Pcc through Monte Carlo simulations of cluster-blind skies, and then comparing the 26 observed low-Pcc bursts against the interloper count from mock catalogs, is what turns a set of alignments into a rate excess.

What would settle it

Locate host galaxies for all 26 candidate cluster FRBs with sub-arcsecond precision and measure their redshifts: if essentially every host lies foreground to its aligned cluster (z_host < z_cluster) and no excess dispersion remains in the cluster sample, the claimed rate enhancement would be ruled out. A second, independent check is to repeat the same Monte Carlo association test on a different arcminute-localized FRB catalog; if no low-Pcc excess appears there, the enhancement does not generalize.

Watch

Extended reading notes

Core claim

The paper's central claim is that the rate of FRBs is enhanced toward massive galaxy clusters at the 3-sigma level. Using a cluster catalog from DECaLS and a score L = Σs(RA,Dec)/P(z < z_clust|DM), where Σs is a projected Navarro-Frenk-White density map of cluster matter and P(z < z_clust|DM) is the model-dependent probability that a burst lies foreground to its most distant aligned cluster, the authors identify 26 FRBs with chance-coincidence probability below 1/892. Monte Carlo realizations of a cluster-blind sky predict 13.4 ± 3.7 such associations for the fiducial energy-function slope γ = −0.5 (14.1 ± 3.7 for γ = 0, and 11.6 ± 3.4 for γ = −1.0), so the probability that all 26 are interlopers is p = 0.0008, 0.0016, and ≤0.0001, respectively. They conclude that clusters cause 1.4% ± 0.4% of detections in the second CHIME/FRB baseband catalog, split roughly evenly between member-galaxy emission and lensing magnification, and they flag FRB 20211113A behind the strong lens Abell 2218 as a candidate lensed burst.

Load-bearing premise

The whole analysis leans on the assumed redshift-versus-dispersion relation of the FRB population: if the model's P(z|DM) is biased for the actual second CHIME/FRB baseband catalog in ways not covered by the tested energy-function and star-formation slopes, the low chance-coincidence scores and the 3-sigma excess could be an artifact of that bias rather than a real cluster effect.

Editorial extensions

If this is right

  • If the excess is real, cluster-aligned FRBs constrain the fraction of FRBs from non-star-forming progenitor channels, because cluster member galaxies have suppressed star formation while still producing some bursts.
  • The lensing component makes cluster sight lines sensitive to high-redshift evolution of the FRB energy function; a steeper high-z slope (γ′ ≈ −2.5) nearly reconciles simulations with the observed 26 associations.
  • A repeating FRB (FRB 20200929C / FRB 20201125B) aligned with a foreground cluster could, with long-term monitoring, probe intracluster-medium variations and, if strongly lensed, provide time-delay cosmology.
  • Even unlocalized bursts carry statistical information about cluster dispersion and ICM temperature: the paper measures a mean ICM temperature of 3.25 ± 1.44 × 10^7 K from the DM–y_sz relation in the highest-purity subsample.
  • The cluster DM contribution, though small per burst, is detectable at the population level and should be accounted for in precision cosmological uses of FRB dispersion measures.

Reading between the lines

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

  • We infer that the same score could be applied to future arcsecond-localized FRB samples to test the member-versus-lensing decomposition directly: member bursts should sit at the cluster redshift with small excess DM, while lensed bursts should be high-DM, background, and magnified.
  • The claimed 1.4% excess predicts a specific cumulative signal: in a larger catalog of several thousand arcminute-localized bursts, the number of cluster-associated FRBs should grow faster than the interloper expectation, and the excess fraction should stay near 1%; a null result at that scale would falsify the enhancement.
  • The DM–y_sz temperature measurement, if extended to individual well-localized cluster FRBs, offers a per-sight-line ICM gas temperature probe independent of X-ray or SZ data alone, once host redshifts are available.
  • The authors' own simulation implies that an FRB aligned within r500 of a M500 ≥ 10^14 M_sun cluster is about equally likely to be a member burst or a background interloper, a prediction that differs from earlier claims and is testable with higher-mass cluster samples.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. The paper analyzes the second CHIME/FRB baseband catalog against the DECaLS cluster catalog of Wen & Han (2024), using a score L = Σ_s / P(z < z_clust | DM) that combines a projected NFW density map with the probability that a burst is foreground to an aligned cluster. Monte Carlo simulations are used to assign each FRB a probability of chance coincidence P_cc, yielding a sample of 26 cluster-associated FRBs. The authors then simulate mock FRB catalogs to estimate the expected number of interloper (unmagnified background) associations, obtaining 13.4±3.7 for γ=−0.5, and compare with 26 observed associations to claim a 3σ rate enhancement that constitutes 1.4±0.4% of the second baseband catalog. The paper also studies cluster DM contributions, identifies a repeating FRB and two Coma-cluster intersections, and highlights FRB 20211113A aligned with Abell 2218 as a possible gravitationally lensed burst.

Significance. If the claimed enhancement is real, the result would demonstrate that cluster sightlines contain a measurable excess of FRBs, providing a new probe of FRB progenitors, cluster environments, and gravitational lensing of fast transients. The paper is clearly written, uses a well-defined masked sample, and is commendably transparent about the DM-based selection bias in the cluster sample (Section 3.1). It also tests a grid of population parameters (γ, n_SFR) and provides a concrete candidate for gravitational lensing with a path toward follow-up. However, the central statistical claim depends on a null simulation that appears to omit a physical population, and the significance estimate is therefore not currently supported.

major comments (2)
  1. [Appendix B, step 5; Section 3.4] The null Monte Carlo rejects every simulated FRB with a redshift greater than that of a cluster within 3×r500, i.e., it removes unmagnified background FRBs from the mock catalogs. Yet Section 3.4 defines interlopers as 'unmagnified background FRBs that happen to be aligned with a foreground cluster.' Under the no-cluster-effect null, these background FRBs are a physical population that must be present in the mock catalogs; because they have low P(z<z_clust|DM) and therefore high association scores, excluding them lowers the expected interloper count (13.4±3.7 for γ=−0.5) and inflates the claimed excess (26 associations; p=0.0008). The same foreground-only conditioning enters the P_cc Monte Carlo in Section 2 and the Anderson-Darling test in Figure 1. The robustness tests in Section 3.4 vary γ, n_SFR, host parameters, and completeness, but none of them alter the z>z_clust rejection in Appendix B. The argument that applying the same search to mock and real data cancels modeling error does not apply here, because the null distribution itself is missing a physical population.
  2. [Section 2, Table 1; Appendix B] Both the association score L = Σ_s / P(z<z_clust|DM) and the null Monte Carlo are generated from the same z-DM population model, but the predicted DM distribution of this model is not validated against the second CHIME/FRB baseband catalog; Appendix B states that the default parameters are consistent only with the first CHIME catalog. If the true DM–redshift relation differs from the model in a way not spanned by the γ and n_SFR grids (for example, in the host-galaxy DM distribution or the local rate normalization), then the P_cc distribution and the interloper counts would be jointly biased, potentially creating a spurious excess. I recommend a direct two-sample comparison of the simulated and observed DM distributions (for example, a Kolmogorov–Smirnov or Anderson–Darling test) and a rerun of the null Monte Carlo with a model re-fit to the second catalog's DM distribution.
minor comments (4)
  1. [Tables 2 and 3] Table 2 lists an entry as 'FRB Unknown' while Table 3 lists FRB 20191220C; the one-to-one correspondence between the cluster-association table and the FRB property table should be made explicit.
  2. [Figure 14] The label 'DESI' in Figure 14 appears to be a typo for 'DECaLS,' since the text and catalog refer to DECaLS; please correct the label.
  3. [Section 3.2] For the highest-purity subsample (P(z<z_clust|DM)<0.01) the best-fit concentration is c=0.8±1.2, which is still below the expected c=2.6; the sentence claiming agreement with the 'characteristic expectation' should be qualified to reflect the large uncertainty.
  4. [Appendix B, step 2] Step 2 resamples each FRB's declination from a Normal distribution with standard deviation equal to the baseband localization uncertainty, but the text in Section 2 describes localization to approximately 1 arcminute; the exact uncertainty model and its validation should be stated.

Circularity Check

1 steps flagged · score 6.0 of 10

Expected interloper count is generated from a null that excludes the background FRBs it is supposed to count, inflating the 3σ excess by construction.

  1. self definitional [Section 3.4 (interloper definition and mock generation) and Appendix B, step 5]
    "either they will be unmagnified background FRBs that happen to be aligned with a foreground cluster, which we term interlopers, or they will be additional FRBs detected only due to the presence of the cluster, constituting a cluster rate excess. To evaluate the number of expected interlopers we simulate 10000 mock FRB samples using z-DM and distribute them on the sky, uninformed by the location of known clusters, consistently with the spatial distribution expected for CHIME/FRB, as detailed in Appendix B. ..."

    The paper defines interlopers as unmagnified background FRBs aligned with foreground clusters, but the Appendix B Monte Carlo used to count expected interlopers rejects exactly those FRBs: step 5 resamples any simulated FRB with z greater than that of a cluster within 3×r500, i.e., background FRBs. Under the no-cluster-effect null, FRB positions are independent of clusters, so such z_FRB > z_clust events should be present and can receive high association scores because P(z<z_clust|DM) is small. By removing them, the mock catalogs contain only foreground FRBs near clusters, lowering the expected interloper count (13.4±3.7 for γ=-0.5) relative to the 26 observed associations and producing p=0.0008 and the claimed 3σ.

full rationale

The central detection claim is not circular in the sense of fitting a parameter and renaming it a prediction: the observed 26 associations, the DECaLS cluster catalog, and the z-DM population inputs are external to the paper, and the authors test a grid of population parameters. However, the specific number against which the excess is measured is internally inconsistent. Section 3.4 states that interlopers are unmagnified background FRBs aligned with foreground clusters, yet Appendix B step 5 rejects simulated FRBs with redshift greater than that of a cluster within 3×r500. This removes the very population the mock is intended to count. The expected interloper count is therefore biased low by construction, and the p=0.0008 / 3σ statement reduces to a comparison against a null that excludes the events it is supposed to allow. The paper's robustness tests (varying γ, n_SFR, threshold, profile concentration) do not alter this exclusion, so the significance inflation persists across all variants. Because the analysis still contains independent external data and a real search pipeline, the circularity is partial rather than total; the claim that 'the probability that all our associations are interlopers is p=0.0008' is, however, structurally forced by the foreground-only null. Score 6: one central prediction reduces by construction, while other parts of the paper (DM profile, lensing candidate discussion) retain independent content.

Assumptions & free parameters 6 free parameters · 5 assumptions · 0 invented entities

The central claim rests on a population model inherited from prior fits and on a heuristic association score, with gamma, n_SFR, Phi0, concentration c, epsilon and f_star as the main free or explored parameters. No new physical entities are introduced. The Phi0 normalization is fitted to the global CHIME rate, not to the cluster excess.

free parameters (6)
  • gamma (FRB energy function index) = -0.5 fiducial; grid {0.0, -0.5, -1.0}
    Slope of the cumulative FRB energy function. It sets P(z|DM) and the expected interloper rate. Adopted from prior fits and varied across a grid in this work.
  • n_SFR (redshift distribution index) = 1.0 fiducial; grid {0.5, 1.0, 1.5}
    Index n in rho(z) proportional to psi(z)^n. It shapes the redshift distribution in P(z|DM) and in the interloper simulations.
  • Phi0 (local volumetric FRB rate) = 2.43e4 Gpc^-3 yr^-1
    Normalized to approximately yield the observed CHIME/FRB detection rate. This is a fit to the global rate, not to the cluster excess.
  • Sigma_s NFW concentration c = 6
    Chosen by hand for the association score to balance member galaxy and lensed FRB contributions. Lower concentrations produce more interlopers.
  • epsilon (cluster star formation efficiency relative to field) = 0.2 fiducial; explored grid
    Used in modeling FRB emission from cluster member galaxies. Poorly constrained and explored over a grid.
  • f_star (fraction of FRBs tracing stellar mass) = explored {0.0, 0.2, 0.4, 0.6, 0.8, 1.0}
    Mixture fraction of stellar-mass-tracing FRB progenitors. It changes the predicted member galaxy contribution, not the interloper count.
assumptions (5)
  • domain assumption FRB population follows the z-DM model with a single power-law energy function and log-normal host DM distribution
    Used throughout Section 2, Section 3.4 and Appendix B to compute P(z|DM) and generate mock catalogs. Parameters are from James et al. 2022b and Shin et al. 2023.
  • domain assumption The Wen & Han 2024 DECaLS cluster catalog is complete within the unmasked footprint with unbiased masses, radii, and redshifts
    Used to compute Sigma_s and cluster associations. Galactic plane incompleteness is masked, but other incompleteness is assumed negligible.
  • domain assumption The NE2025 Galactic electron density model correctly predicts the Milky Way DM contribution for each line of sight
    Extragalactic DM is obtained by subtracting NE2025 (Ocker & Cordes 2026). Errors in this model propagate into P(z|DM).
  • ad hoc to paper The association score L = Sigma_s / P(z < z_clust|DM) is a valid ranking statistic for cluster association probability
    The score is heuristic; no optimality is proven. The null distribution is generated by Monte Carlo under this specific definition (Section 2).
  • ad hoc to paper Cluster halos follow a projected NFW profile with concentration c=6 for the score map, truncated at 3r500
    The c=6 concentration balances member and lensed populations but is not derived from data and is not varied in the central analysis.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Evidence for Enhancement in the Rate of Fast Radio Bursts Toward Galaxy Clusters." pith.science (2026). https://pith.science/paper/6QDMHMIO

@misc{pith2026260810358,
  author       = {Pith},
  title        = {Pith review of: Evidence for Enhancement in the Rate of Fast Radio Bursts Toward Galaxy Clusters},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6QDMHMIO}},
  note         = {Machine review of arXiv:2608.10358}
}
abstract

Massive galaxy clusters can introduce gravitational lensing and populations of suppressed star formation member galaxies into the line of sight, potentially changing the distribution of observable sources toward them from that of the average sky. As a result, Fast Radio Bursts (FRBs) aligned with galaxy clusters can provide a unique window into parameter spaces of the FRB population that other lines of sight do not afford. In this study, we demonstrate that the second CHIME/FRB baseband catalog contains FRBs emitted from within or behind clusters identified from the latest DECaLS data release; we isolate a sample of 26 FRBs where this is likely, including one repeating FRB and two FRBs that intersect the Coma cluster. Comparing our results against a range of simulated FRB populations, we conclude that the number of these associations represents a $3\sigma$ rate enhancement toward galaxy clusters, constituting $1.4\pm0.4\%$ of the FRBs detected in the second CHIME/FRB baseband catalog. We suggest that this enhancement is caused by an equal proportion of member galaxies hosting additional FRBs, and gravitational lensing magnifying background sources. We demonstrate that such contributions are sensitive to alternative progenitor channels and high redshift evolution in the FRB population, providing a future avenue for constraining these features. Considering the redshifts and masses of the associated clusters, we identify FRB 20211113A, which is aligned with the strong gravitational lens Abell 2218 as a potential lensed candidate for further consideration.

Figures

Figures reproduced from arXiv: 2608.10358 by the authors.

Figure 1
Figure 1. Cumulative distributions of the probability of chance coincidence (Pcc) of FRB samples under the null hypothesis that all FRBs are emitted foreground to the most distantly aligned cluster. Plotted distributions correspond to the FRBs from the second CHIME/FRB baseband catalog that lie within the DECaLS footprint and to associated Monte Carlo realisations under the null hypothesis, in comparison to realisations of a … view at source ↗
Figure 2
Figure 2. Size of the FRB subsample satisfying Pcc < X as a function of X for both the second baseband catalog (red), and 100 independent Monte Carlo realisations (black). Also shown is the purity of the baseband catalog 2 sample when compared against the false positive rate in each Monte Carlo realisation (pink) and averaged over all realisations (purple). The dotted line marks where X = 1/N where N is the size of the unmask… view at source ↗
Figure 3
Figure 3. Comparison of FRB morphology amongst cluster and non-cluster FRB samples. Specifically, we display extragalactic DM as a function of both scattering time (left) and intrinsic width (right) estimated from the intensity fits published in CHIME/FRB catalog 2 (CHIME/FRB Collaboration et al. 2026). FRBs for which a scattered profile was disfavoured are binned at τ = 10−5 s for visual distinction. Marginalized distributio… view at source ↗
Figures from the paper (14 more)
Figure 4
Figure 4. Figure 4: Extragalactic DM as a function of physical impact parameter normalized by the r500 scale radius of nearby galaxy clusters measured by (Z. L. Wen & J. L. Han 2024). DM mean and variance as a function of impact parameter, shown by the dark grey points, are calculated fro…
Figure 5
Figure 5. Figure 5: Extragalactic DM as a function of ysz calculated from the Planck map of the thermal Sunyaev-Zel’dovich effect as the weighted mean over the localization region (P. a. R. Ade et al. 2016). DM mean and variance as a function of ysz, shown as dark grey points, are calcula…
Figure 6
Figure 6. Figure 6: CHIME/FRB observation of FRB 20211113A. Left: Dynamic spectrum of the FRB dedispersed to the DM listed in the top left. As noted in the text, much of the high frequency bandwidth is missing, due to baseband ring buffer losses of early times at high dispersive delays. R…
Figure 7
Figure 7. Figure 7: As in [PITH_FULL_IMAGE:figures/full_fig_p012_7.png]
Figure 8
Figure 8. Figure 8: Arrival times and baseband localizations for all repetitions of FRB 20201125B. Left: The S/N of the time integrated burst spectra as a function of arrival time. Right: Burst localizations with respect to aligned clusters, as in above figures. mock cluster associated sa…
Figure 9
Figure 9. Figure 9: Expected rate contribution from the member galaxies of a M500 = 1015 M⊙ galaxy cluster compared to the blank field as a function of the clusters redshift. Rates are evaluated for the characteristic case where star formation efficiency in galaxy clusters is equivalent t…
Figure 10
Figure 10. Figure 10: Expected number of cluster associations (⟨N⟩) in our search contributed by FRBs from galaxy cluster member galaxies as a function of f⊙ (the fraction of FRBs tracing stellar mass), and ϵ (the relative efficiency of star formation in galaxy clusters compared to the fie…
Figure 11
Figure 11. Figure 11: The expected number of cluster associations (⟨N⟩) contributed by lensing from massive galaxy clusters (M500 ≳ 5 × 101 4 M⊙) for varying evolutions of the FRB population at redshifts z ≥ 1 from the baseline populations shown in [PITH_FULL_IMAGE:figures/full_fig_p018_11.png]
Figure 12
Figure 12. Figure 12: Properties of FRB associated clusters decomposed by source. Red contours highlight contributions from gravi￾tational lensing, blue contours highlight FRBs emitted from within a galaxy cluster, and grey represent those of unmagnified interlopers randomly intercepting f…
Figure 13
Figure 13. Figure 13 [PITH_FULL_IMAGE:figures/full_fig_p027_13.png]
Figure 14
Figure 14. Figure 14: Galaxy cluster properties (left: M500, right: redshift) from DECaLS compared to our representative model population in red. 5. For samples in the masked region of the DECaLS map or with a redshift greater than that of a cluster within 3 × r500, repeat the above. Itera…
Figure 15
Figure 15. Figure 15: Significance of the residual between the number of cluster associations made in the observed sample and the mean of those in the mock catalogs for γ = 0. The number of mock associations are calculated as the total number of associations from interlopers, member and le…
Figure 16
Figure 16. Figure 16: Significance of the residual between the observed sample and mock catalogs as in [PITH_FULL_IMAGE:figures/full_fig_p030_16.png]
Figure 17
Figure 17. Figure 17: Significance of the residual between the observed sample and mock catalogs as in [PITH_FULL_IMAGE:figures/full_fig_p031_17.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

100 extracted references · 7 canonical work pages

  1. [1]

    Ade, P. a. R. and Aghanim, N. and Arnaud, M. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Banday, A. J. and Barreiro, R. B. and Barrena, R. and Bartlett, J. G. and Bartolo, N. and Battaner, E. and Battye, R. and Benabed, K. and Beno. Planck 2015 Results -. Astronomy & Astrophysics , volume =. doi:10.1051/0004-6361/201525823 , urldate =

    doi:10.1051/0004-6361/201525823 2015

  2. [2]

    and Arnaud, M

    Aghanim, N. and Arnaud, M. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Banday, A. J. and Barreiro, R. B. and Bartlett, J. G. and Bartolo, N. and Battaner, E. and Battye, R. and Benabed, K. and Beno. Planck 2015 Results -. Astronomy & Astrophysics , volume =. doi:10.1051/0004-6361/201525826 , urldate =

    doi:10.1051/0004-6361/201525826 2015

  3. [3]

    doi:10.3847/1538-4365/ad323f , urldate =

    Bahk, Hyeonguk and Hwang, Ho Seong , year = 2024, month = apr, journal =. doi:10.3847/1538-4365/ad323f , urldate =

    doi:10.3847/1538-4365/ad323f 2024

  4. [4]

    and Prochaska, J

    Bhandari, Shivani and Sadler, Elaine M. and Prochaska, J. Xavier and Simha, Sunil and Ryder, Stuart D. and Marnoch, Lachlan and Bannister, Keith W. and Macquart, Jean-Pierre and Flynn, Chris and Shannon, Ryan M. and Tejos, Nicolas and. The Host Galaxies and Progenitors of. The Astrophysical Journal , volume =. doi:10.3847/2041-8213/ab672e , urldate =. arX...

    arXiv

  5. [5]

    and Donahue, Megan and Voit, G

    Cavagnolo, Kenneth W. and Donahue, Megan and Voit, G. Mark and Sun, Ming , year = 2009, month = may, journal =. Intracluster. doi:10.1088/0067-0049/182/1/12 , urldate =

    doi:10.1088/0067-0049/182/1/12 2009

  6. [6]

    The Astrophysical Journal , volume =

    Coe, Dan and Salmon, Brett and Brada. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/ab412b , urldate =

    doi:10.3847/1538-4357/ab412b

  7. [7]

    and Amouyal, Daniel and Andersen, Bridget C

    Collaboration, The CHIME/FRB and Abbott, Thomas C. and Amouyal, Daniel and Andersen, Bridget C. and Andrew, Shion E. and Bandura, Kevin and Bhardwaj, Mohit and Bhopi, Kalyani and Bhusare, Yash and Brar, Charanjot and Cai, Alice and Cassanelli, Tomas and Chatterjee, Shami and Cliche, Jean-Fran. The Astrophysical Journal Letters , volume =. doi:10.3847/2041...

    doi:10.3847/2041-8213/adf62f

  8. [8]

    , keywords =

    The Interaction of Matter and Radiation in a Hot-Model Universe. , keywords =. doi:10.1007/BF00661821 , adsurl =

    doi:10.1007/bf00661821

Show all 100 references
  1. [9]

    , keywords =

    Updating the First CHIME/FRB Catalog of Fast Radio Bursts with Baseband Data. , keywords =. doi:10.3847/1538-4357/ad464b , archivePrefix =. 2311.00111 , primaryClass =

    arXiv

  2. [10]

    , keywords =

    Probabilistic Association of Transients to their Hosts (PATH). , keywords =. doi:10.3847/1538-4357/abe8d2 , archivePrefix =. 2102.10627 , primaryClass =

    arXiv

  3. [11]

    , keywords =

    The Second CHIME/FRB Catalog of Fast Radio Bursts. , keywords =. doi:10.3847/1538-4365/ae3828 , archivePrefix =. 2601.09399 , primaryClass =

  4. [12]

    and Lamb, James W

    Connor, Liam and Ravi, Vikram and Catha, Morgan and Chen, Ge and Faber, Jakob T. and Lamb, James W. and Hallinan, Gregg and Harnach, Charlie and Hellbourg, Greg and Hobbs, Rick and Hodge, David and Hodges, Mark and Law, Casey and Rasmussen, Paul and Sayers, Jack and Sharma, Kr...

  5. [13]

    Nature Astronomy , volume =

    A Gas-Rich Cosmic Web Revealed by the Partitioning of the Missing Baryons , author =. Nature Astronomy , volume =. doi:10.1038/s41550-025-02566-y , urldate =

    doi

  6. [14]

    , keywords =

    First Constraints on Compact Dark Matter from Fast Radio Burst Microstructure. , keywords =. doi:10.3847/1538-4357/aba7bb , archivePrefix =. 2002.12533 , primaryClass =

    2002 arXiv

  7. [15]

    , keywords =

    Ram pressure stripping in high-density environments. , keywords =. doi:10.1007/s00159-022-00140-3 , archivePrefix =. 2109.13614 , primaryClass =

    arXiv

  8. [16]

    , keywords =

    Ram Pressure Stripping in Clusters and Groups. , keywords =. doi:10.1086/505614 , archivePrefix =. astro-ph/0610088 , primaryClass =

    arXiv

  9. [17]

    arXiv e-prints , keywords =

    A 4200-hour HyperFlash and \'E CLAT campaign on the hyperactive FRB 20240114A: constraining energetics with the most brilliant bursts. arXiv e-prints , keywords =. doi:10.48550/arXiv.2605.18513 , archivePrefix =. 2605.18513 , primaryClass =

    doi arXiv

  10. [18]

    , keywords =

    Morphology of 35 Repeating Fast Radio Burst Sources at Microsecond Time Scales with CHIME/FRB. , keywords =. doi:10.3847/1538-4357/adf844 , archivePrefix =. 2411.02870 , primaryClass =

    arXiv

  11. [19]

    , keywords =

    Wave Optics, Interference, and Decoherence in Strong Gravitational Lensing. , keywords =. doi:10.1007/s11214-025-01157-7 , archivePrefix =. 2304.01202 , primaryClass =

    arXiv

  12. [20]

    , keywords =

    Simulating FRB morphologies and coherent phase correlation signatures from multiplane astrophysical lensing. , keywords =. doi:10.1103/PhysRevD.110.123027 , archivePrefix =. 2407.04097 , primaryClass =

    arXiv

  13. [21]

    , keywords =

    Star formation efficiency in galaxy clusters. , keywords =. doi:10.1051/0004-6361:20079168 , archivePrefix =. 0804.1102 , primaryClass =

    arXiv

  14. [22]

    , keywords =

    Constraining primordial black holes using fast radio burst gravitational-lens interferometry with CHIME/FRB. , keywords =. doi:10.1103/PhysRevD.106.043017 , archivePrefix =. 2204.06001 , primaryClass =

    arXiv

  15. [23]

    , keywords =

    A Probable z -0.5ex 7 Galaxy Strongly Lensed by the Rich Cluster A2218: Exploring the Dark Ages. , keywords =. doi:10.1086/386281 , archivePrefix =. astro-ph/0402319 , primaryClass =

    arXiv

  16. [24]

    Cordes, J. M. and Lazio, T. J. W. , year = 2003, month = jan, number =. doi:10.48550/arXiv.astro-ph/0207156 , urldate =. arXiv , keywords =:astro-ph/0207156 , publisher =

    2003 doi arXiv

  17. [25]

    and Schaye, Joop and Kay, Scott T

    Duffy, Alan R. and Schaye, Joop and Kay, Scott T. and Dalla Vecchia, Claudio , year = 2008, month = oct, journal =. Dark Matter Halo Concentrations in the. doi:10.1111/j.1745-3933.2008.00537.x , urldate =

    2008

  18. [26]

    Gal, R. R. and de Carvalho, R. R. and Odewahn, S. C. and Djorgovski, S. G. and Mahabal, A. and Brunner, R. J. and Lopes, P. a. A. , year = 2004, month = dec, journal =. The. doi:10.1086/344941 , urldate =

    2004 doi

  19. [27]

    and Pierini, D

    Giodini, S. and Pierini, D. and Finoguenov, A. and Pratt, G. W. and Boehringer, H. and Leauthaud, A. and Guzzo, L. and Aussel, H. and Bolzonella, M. and Capak, P. and Elvis, M. and Hasinger, G. and Ilbert, O. and Kartaltepe, J. S. and Koekemoer, A. M. and Lilly, S. J. and Mass...

  20. [28]

    and Fong, Wen-fai and Kilpatrick, Charles D

    Gordon, Alexa C. and Fong, Wen-fai and Kilpatrick, Charles D. and Eftekhari, Tarraneh and Leja, Joel and Prochaska, J. Xavier and Nugent, Anya E. and Bhandari, Shivani and Blanchard, Peter K. and Caleb, Manisha and Day, Cherie K. and Deller, Adam T. and Dong, Yuxin and Glowack...

    2023

  21. [29]

    and Fong, Wen-fai and Deller, Adam T

    Gordon, Alexa C. and Fong, Wen-fai and Deller, Adam T. and Marnoch, Lachlan and Lim, Sungsoon and Peng, Eric W. and Bannister, Keith W. and Bera, Apurba and Bhat, N. D. R. and Dial, Tyson and Dong, Yuxin and Eftekhari, Tarraneh and Glowacki, Marcin and Gourdji, Kelly and Gupta...

    doi

  22. [30]

    and James, C

    Hoffmann, J. and James, C. W. and Glowacki, M. and Prochaska, J. X. and Gordon, A. C. and Deller, A. T. and Shannon, R. M. and Ryder, S. D. , year = 2024, month = dec, journal =. Modelling. doi:10.1017/pasa.2024.127 , urldate =

    2024 doi

  23. [31]

    Horowicz, Asaf and Margalit, Ben , year = 2026, month = jan, journal =. The. doi:10.3847/1538-4357/ae1f11 , urldate =

    2026 doi

  24. [32]

    Monthly Notices of the Royal Astronomical Society , issn =

    The Fast Radio Burst Population Evolves, Consistent with the Star-Formation Rate , author =. Monthly Notices of the Royal Astronomical Society , issn =. doi:10.1093/mnrasl/slab117 , urldate =

    doi

  25. [33]

    A Measurement of

    James, C W and Ghosh, E M and Prochaska, J X and Bannister, K W and Bhandari, S and Day, C K and Deller, A T and Glowacki, M and Gordon, A C and Heintz, K E and Marnoch, L and Ryder, S D and Scott, D R and Shannon, R M and Tejos, N , year = 2022, month = nov, journal =. A Meas...

    2022 doi

  26. [34]

    , year = 2023, journal =

    James, C.W. , year = 2023, journal =. Modelling Repetition in. doi:10.1017/pasa.2023.51 , urldate =

    2023 doi

  27. [35]

    James, C W and Prochaska, J X and Macquart, J-P and. The z--. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stab3051 , urldate =

    doi

  28. [36]

    Astronomy & Astrophysics , volume =

    Deep View of the Intracluster Light in the. Astronomy & Astrophysics , volume =. doi:10.1051/0004-6361/202452384 , urldate =

    doi

  29. [37]

    and Sharon, Keren and Bayliss, Matthew B

    Johnson, Traci L. and Sharon, Keren and Bayliss, Matthew B. and Gladders, Michael D. and Coe, Dan and Ebeling, Harald , year = 2014, month = nov, journal =. doi:10.1088/0004-637X/797/1/48 , urldate =

    2014 doi

  30. [38]

    Nature , volume =

    A Repeating Fast Radio Burst Source in a Globular Cluster , author =. Nature , volume =. doi:10.1038/s41586-021-04354-w , urldate =

    doi

  31. [39]

    and Mohr, J

    Klein, M. and Mohr, J. J. and Davies, C. T. , year = 2024, month = oct, journal =. The. doi:10.1051/0004-6361/202451203 , urldate =

    2024 doi

  32. [40]

    Monthly Notices of the Royal Astronomical Society , volume =

    Klein, Matthias and. Monthly Notices of the Royal Astronomical Society , volume =. doi:10.1093/mnras/stad2729 , urldate =

    doi

  33. [41]

    and Comparat, J

    Kluge, M. and Comparat, J. and Liu, A. and Balzer, F. and Bulbul, E. and Chitham, J. Ider and Ghirardini, V. and Garrel, C. and Bahar, Y. E. and Artis, E. and Bender, R. and Clerc, N. and Dwelly, T. and Fabricius, M. H. and Grandis, S. and. The. Astronomy & Astrophysics , volu...

    doi

  34. [42]

    Astronomy Letters , volume =

    Stellar Mass -- Halo Mass Relation and Star Formation Efficiency in High-Mass Halos , author =. Astronomy Letters , volume =. doi:10.1134/S1063773717120015 , urldate =. arXiv , keywords =:1401.7329 , primaryclass =

    arXiv

  35. [43]

    and Simha, Sunil and Masui, Kiyoshi W

    Lanman, Adam E. and Simha, Sunil and Masui, Kiyoshi W. and Prochaska, J. Xavier and Darlinger, Rachel and Dong, Fengqiu Adam and Gaensler, B. M. and Joseph, Ronniy C. and Kaczmarek, Jane and Kahinga, Lordrick and Khan, Afrokk and Leung, Calvin and. Constraining. doi:10.48550/a...

    doi arXiv

  36. [44]

    The Astrophysical Journal , volume =

    The Integrated Stellar Content of Dark Matter Halos , author =. The Astrophysical Journal , volume =. doi:10.1088/0004-637X/746/1/95 , urldate =. arXiv , keywords =:1109.0010 , primaryclass =

    arXiv

  37. [45]

    Gravitational Microlensing Time Delays at High Optical Depth: Image Parities and the Temporal Properties of Fast Radio Bursts , shorttitle =

    Lewis, Geraint F , year = 2020, month = sep, journal =. Gravitational Microlensing Time Delays at High Optical Depth: Image Parities and the Temporal Properties of Fast Radio Bursts , shorttitle =. doi:10.1093/mnras/staa2044 , urldate =

    2020 doi

  38. [46]

    Li, Changhua and Zhang, Yanxia and Cui, Chenzhou and Wei, Shirui and Zhang, Jingyi and Zhao, Yongheng and Wu, Xue-Bing and Tao, Yihan and Li, Shanshan and Wang, Youfen and Kang, Zihan , year = 2024, month = nov, journal =. A. doi:10.3847/1538-3881/ad7c52 , urldate =

    2024 doi

  39. [47]

    and Prochaska, J

    Macquart, J.-P. and Prochaska, J. X. and McQuinn, M. and Bannister, K. W. and Bhandari, S. and Day, C. K. and Deller, A. T. and Ekers, R. D. and James, C. W. and Marnoch, L. and Oslowski, S. and Phillips, C. and Ryder, S. R. and Scott, D. R. and Shannon, R. M. and Tejos, N. , ...

    2020 arXiv

  40. [48]

    Madau, Piero and Dickinson, Mark , year = 2014, month = aug, journal =. Cosmic. doi:10.1146/annurev-astro-081811-125615 , urldate =. arXiv , keywords =:1403.0007 , pages =

    2014 arXiv

  41. [49]

    and Shin, Kaitlyn and Andersen, Bridget and Josephy, Alexander and Good, Deborah and Dong, Fengqiu Adam and Masui, Kiyoshi W

    Merryfield, Marcus and Tendulkar, Shriharsh P. and Shin, Kaitlyn and Andersen, Bridget and Josephy, Alexander and Good, Deborah and Dong, Fengqiu Adam and Masui, Kiyoshi W. and Lang, Dustin and M. An. The Astronomical Journal , volume =. doi:10.3847/1538-3881/ac9ab5 , urldate =

    doi

  42. [50]

    and Masui, K

    Michilli, D. and Masui, K. W. and Mckinven, R. and Cubranic, D. and Bruneault, M. and Brar, C. and Patel, C. and Boyle, P. J. and Stairs, I. H. and Renard, A. and Bandura, K. and Berger, S. and Breitman, D. and Cassanelli, T. and Dobbs, M. and Kaspi, V. M. and Leung, C. and. A...

    doi

  43. [51]

    Lensing of

    Mu. Lensing of. Physical Review Letters , volume =. doi:10.1103/PhysRevLett.117.091301 , urldate =. arXiv , keywords =:1605.00008 , pages =

    arXiv

  44. [52]

    Science , keywords =

    Multiple images of a highly magnified supernova formed by an early-type cluster galaxy lens. Science , keywords =. doi:10.1126/science.aaa3350 , archivePrefix =. 1411.6009 , primaryClass =

    arXiv

  45. [53]

    , keywords =

    SN H0pe: The First Measurement of H _ 0 from a Multiply Imaged Type Ia Supernova, Discovered by JWST. , keywords =. doi:10.3847/1538-4357/ad9928 , archivePrefix =. 2403.18902 , primaryClass =

    arXiv

  46. [54]

    , keywords =

    Lensed Type Ia Supernova ``Encore'' at z = 2: The First Instance of Two Multiply Imaged Supernovae in the Same Host Galaxy. , keywords =. doi:10.3847/2041-8213/ad4648 , archivePrefix =. 2404.02139 , primaryClass =

    arXiv

  47. [55]

    Jain, Naman , title =. in prep. , note =

  48. [56]

    , keywords =

    A New Electron-density Model for Estimation of Pulsar and FRB Distances. , keywords =. doi:10.3847/1538-4357/835/1/29 , archivePrefix =. 1610.09448 , primaryClass =

    arXiv

  49. [57]

    Canadian Long Range Plan for Astronomy and Astrophysics White Papers , year = 2019, volume =

    The Canadian Hydrogen Observatory and Radio-transient Detector (CHORD). Canadian Long Range Plan for Astronomy and Astrophysics White Papers , year = 2019, volume =. doi:10.5281/zenodo.3765414 , archivePrefix =. 1911.01777 , primaryClass =

    2019 arXiv

  50. [58]

    Planck 2018 results. VI. Cosmological parameters. , keywords =. doi:10.1051/0004-6361/201833910 , archivePrefix =. 1807.06209 , primaryClass =

    2018 arXiv

  51. [59]

    , keywords =

    The Coma/A1367 supercluster and its environs. , keywords =. doi:10.1086/156198 , adsurl =

    doi

  52. [60]

    , keywords =

    Modeling the Morphology of Fast Radio Bursts and Radio Pulsars with fitburst. , keywords =. doi:10.3847/1538-4365/ad27d6 , archivePrefix =. 2311.05829 , primaryClass =

    arXiv

  53. [61]

    , keywords =

    A Search for Persistent Radio Sources toward Repeating Fast Radio Bursts Discovered by CHIME/FRB. , keywords =. doi:10.3847/1538-4357/ad808e , archivePrefix =. 2409.11533 , primaryClass =

    arXiv

  54. [62]

    , keywords =

    The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors. , keywords =. doi:10.3847/1538-4357/ace5aa , archivePrefix =. 2302.05465 , primaryClass =

    arXiv

  55. [63]

    , keywords =

    Unveiling the Origin of Fast Radio Bursts by Modeling the Stellar Mass and Star Formation Distributions of Their Host Galaxies. , keywords =. doi:10.3847/1538-4357/adf555 , archivePrefix =. 2502.15566 , primaryClass =

    arXiv

  56. [64]

    , keywords =

    CHIME/FRB Outriggers: Design Overview. , keywords =. doi:10.3847/1538-4357/adfdcc , archivePrefix =. 2504.05192 , primaryClass =

    arXiv

  57. [65]

    2009 , note =

    The Astrophysical Journal , author =. 2009 , note =. doi:10.1088/0004-637X/706/2/1201 , abstract =

    2009 doi

  58. [66]

    , keywords =

    The radial distribution of galaxies in groups and clusters. , keywords =. doi:10.1111/j.1365-2966.2012.20663.x , archivePrefix =. 1201.5491 , primaryClass =

    2012

  59. [67]

    , keywords =

    Temporal Smearing of Transient Radio Sources by the Intergalactic Medium. , keywords =. doi:10.1088/0004-637X/776/2/125 , archivePrefix =. 1308.4459 , primaryClass =

    arXiv

  60. [68]

    The Astronomy and Astrophysics Review , author =

    Cluster lenses , volume =. The Astronomy and Astrophysics Review , author =. 2011 , keywords =. doi:10.1007/s00159-011-0047-3 , abstract =

    2011 doi

  61. [69]

    , keywords =

    FRB 20250316A: A Brilliant and Nearby One-off Fast Radio Burst Localized to 13 pc Precision. , keywords =. doi:10.3847/2041-8213/adf62f , archivePrefix =. 2506.19006 , primaryClass =

  62. [70]

    arXiv e-prints , keywords =

    Evidence for a Delayed Progenitor Population for CHIME non-repeating Fast Radio Bursts using a Self-Consistent Forward and Backward Inference Framework. arXiv e-prints , keywords =. doi:10.48550/arXiv.2607.04792 , archivePrefix =. 2607.04792 , primaryClass =

    doi arXiv

  63. [71]

    , keywords =

    CHIME/FRB Discovery of 25 Repeating Fast Radio Burst Sources. , keywords =. doi:10.3847/1538-4357/acc6c1 , archivePrefix =. 2301.08762 , primaryClass =

    arXiv

  64. [72]

    arXiv e-prints , keywords =

    Discovery of 30 Repeating Fast Radio Burst Sources and Uniform Population Statistics of 80 Repeating Sources from CHIME/FRB. arXiv e-prints , keywords =. doi:10.48550/arXiv.2605.08410 , archivePrefix =. 2605.08410 , primaryClass =

    doi arXiv

  65. [73]

    Commentary on: Cavaliere A

    The -model of the intracluster medium. Commentary on: Cavaliere A. and Fusco-Femiano R., 1976, A&A, 49, 137. , year = 2009, month = jun, volume =. doi:10.1051/0004-6361/200912150 , adsurl =

    1976 doi

  66. [74]

    , keywords =

    CHIME/FRB Discovery of Eight New Repeating Fast Radio Burst Sources. , keywords =. doi:10.3847/2041-8213/ab4a80 , archivePrefix =. 1908.03507 , primaryClass =

    1908 arXiv

  67. [75]

    Maxwell Fine , year =

  68. [76]

    Bridget Andersen , year =

  69. [77]

    The Astrophysical Journal , volume =

    Statistical. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/ad0c59 , urldate =

    doi

  70. [78]

    , keywords =

    Magnetospheric origin of a fast radio burst constrained using scintillation. , keywords =. doi:10.1038/s41586-024-08297-w , archivePrefix =. 2406.11053 , primaryClass =

    arXiv

  71. [79]

    , keywords =

    CHIME/FRB Discovery and Localization of the Swift-observed FRB 20241228A. , keywords =. doi:10.3847/1538-4357/ae2ea0 , archivePrefix =. 2506.10961 , primaryClass =

    arXiv

  72. [80]

    , keywords =

    The CHIME Fast Radio Burst Project: System Overview. , keywords =. doi:10.3847/1538-4357/aad188 , archivePrefix =. 1803.11235 , primaryClass =

    arXiv

  73. [81]

    Nature Astronomy , keywords =

    A gravitationally lensed supernova with an observable two-decade time delay. Nature Astronomy , keywords =. doi:10.1038/s41550-021-01450-9 , archivePrefix =. 2106.08935 , primaryClass =

    arXiv

  74. [82]

    and Frenk, Carlos S

    Navarro, Julio F. and Frenk, Carlos S. and White, Simon D. M. , year = 1996, month = may, journal =. The. doi:10.1086/177173 , urldate =

    1996 doi

  75. [83]

    and others , year = 2017, month = feb, doi =

    Ng, C. and others , year = 2017, month = feb, doi =

    2017

  76. [84]

    Nature Communications , keywords =

    Strongly lensed repeating fast radio bursts as precision probes of the universe. Nature Communications , keywords =. doi:10.1038/s41467-018-06303-0 , archivePrefix =. 1708.06357 , primaryClass =

    arXiv

  77. [85]

    and Chatterjee, Shami and Niu, Chen-Hui and Li, Di and McKee, James W

    Ocker, Stella Koch and Cordes, James M. and Chatterjee, Shami and Niu, Chen-Hui and Li, Di and McKee, James W. and Law, Casey J. and Tsai, Chao-Wei and. The. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/ac6504 , urldate =

    doi

  78. [86]

    Ocker, S. K. and Cordes, J. M. , year = 2026, month = feb, number =. doi:10.48550/arXiv.2602.11838 , urldate =. arXiv , keywords =:2602.11838 , primaryclass =

    2026 doi arXiv

  79. [87]

    and Fonseca, Emmanuel and McGregor, Kyle and Gaensler, B

    Patil, Swarali Shivraj and Main, Robert A. and Fonseca, Emmanuel and McGregor, Kyle and Gaensler, B. M. and Bhardwaj, Mohit and Brar, Charanjot and Cook, Amanda M. and Curtin, Alice P. and Eadie, Gwendolyn and Joseph, Ronniy and Kahinga, Lordrick and Kaspi, Victoria and Khan, ...

    2026

  80. [88]

    Xavier and Simha, Sunil and

    Prochaska, J. Xavier and Simha, Sunil and. doi:10.5281/zenodo.14804392 , urldate =

    doi

  81. [89]

    Ryder, S. D. and Bannister, K. W. and Bhandari, S. and Deller, A. T. and Ekers, R. D. and Glowacki, M. and Gordon, A. C. and Gourdji, K. and James, C. W. and Kilpatrick, C. D. and Lu, W. and Marnoch, L. and Moss, V. A. and Prochaska, J. X. and Qiu, H. and Sadler, E. M. and Sim...

    2023 doi

  82. [90]

    Rykoff, E. S. and Rozo, E. and Busha, M. T. and Cunha, C. E. and Finoguenov, A. and Evrard, A. and Hao, J. and Koester, B. P. and Leauthaud, A. and Nord, B. and Pierre, M. and Reddick, R. and Sadibekova, T. and Sheldon, E. S. and Wechsler, R. H. , year = 2014, month = apr, jou...

    2014 doi

  83. [91]

    Sammons, Mawson W. and. Forecasting the. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/addc71 , urldate =

    doi

  84. [92]

    Nature , volume =

    Preferential Occurrence of Fast Radio Bursts in Massive Star-Forming Galaxies , author =. Nature , volume =. doi:10.1038/s41586-024-08074-9 , urldate =

    doi

  85. [93]

    and Bhardwaj, Mohit and Cassanelli, Tomas and Chawla, Pragya and Dobbs, Matt and Dong, Fengqiu Adam and Fonseca, Emmanuel and Gaensler, B

    Shin, Kaitlyn and Masui, Kiyoshi W. and Bhardwaj, Mohit and Cassanelli, Tomas and Chawla, Pragya and Dobbs, Matt and Dong, Fengqiu Adam and Fonseca, Emmanuel and Gaensler, B. M. and. Inferring the. The Astrophysical Journal , volume =. doi:10.3847/1538-4357/acaf06 , urldate =

    doi

  86. [94]

    Measurement of Angular Cross-Correlation between the Cosmological Dispersion Measure and the Thermal

    Takahashi, Ryuichi and Ioka, Kunihito and Shirasaki, Masato and Osato, Ken , year = 2025, month = nov, number =. Measurement of Angular Cross-Correlation between the Cosmological Dispersion Measure and the Thermal. doi:10.48550/arXiv.2511.02155 , urldate =. arXiv , keywords =:...

    2025 doi arXiv

  87. [95]

    and Stoica, Radu S

    Tempel, Elmo and Kruuse, Maarja and Kipper, Rain and Tuvikene, Taavi and Sorce, Jenny G. and Stoica, Radu S. , year = 2018, month = oct, journal =. Bayesian Group Finder Based on Marked Point Processes -. doi:10.1051/0004-6361/201833217 , urldate =

    2018 doi

  88. [96]

    Brent , year = 2015, month = apr, journal =

    Tully, R. Brent , year = 2015, month = apr, journal =. doi:10.1088/0004-6256/149/5/171 , urldate =

    2015 doi

  89. [97]

    Wen, Z. L. and Han, J. L. , year = 2024, month = jun, journal =. A. doi:10.3847/1538-4365/ad409d , urldate =

    2024 doi

  90. [98]

    Catalog of

    Xu, Weiwei and. Catalog of. Astronomy & Astrophysics , volume =. doi:10.1051/0004-6361/202140908 , urldate =

    doi

  91. [99]

    Photometric

    Zou, Hu and Sui, Jipeng and Xue, Suijian and Zhou, Xu and Ma, Jun and Zhou, Zhimin and Nie, Jundan and Zhang, Tianmeng and Feng, Lu and Shen, Zhixia and Wang, Jiali , year = 2022, month = may, journal =. Photometric. doi:10.1088/1674-4527/ac6416 , urldate =

    2022 doi

  92. [100]

    Astronomicheskii Zhurnal , author =

    The. Astronomicheskii Zhurnal , author =. 1966 , pages =

    1966

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.