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Discovery of a PRS associated with FRB 20240114A

T0 review · 3 major / 6 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read A compact 5 GHz radio source detected 50 milliarcseconds from the precise position of FRB 20240114A is the fourth persistent radio source associated with a fast radio burst.

desk verdict The VLBA detection is credible, but the PRS association and the nebular-model validation both need stronger quantitative support before this should be treated as a secure fourth PRS. read the letter →

arxiv 2412.01478 v2 pith:DRN7CZPX submitted 2024-12-02 astro-ph.HE astro-ph.GAastro-ph.SR

G. Bruni , L. Piro , Y.-P. Yang , E. Palazzi , L. Nicastro , A. Rossi , S. Savaglio , E. Maiorano
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B. Zhang
This is my paper · ORCID
classification astro-ph.HEastro-ph.GAastro-ph.SR
keywords fastradioburstspersistentsourceFRB20240114AverylongbaselineinterferometrynebularmodelFaradayrotationmeasuresynchrotronemissiondwarfstarbursthostgalaxy
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

This paper uses twelve hours of VLBA time at 5 GHz to search for a compact radio counterpart to the repeating fast radio burst FRB 20240114A, following lower-resolution MeerKAT and uGMRT hints. It detects a 46 microjansky source about 50 milliarcseconds from the FRB's nominal position and argues that this is the persistent radio source (PRS) associated with the burst, only the fourth such source known. The detection matters because PRSs are rare probes of the environment around an FRB engine; the source's luminosity and the burst's measured Faraday rotation place it on the nebular-model relation, supporting the idea that some repeating FRBs are embedded in magnetized synchrotron-emitting nebulae. The paper also characterises the host as a dwarf sub-solar-metallicity starburst galaxy and finds evidence for a possible spectral peak or steepening between 650 MHz and 5 GHz that future VLBI observations can test.

What carries the argument

The central object is a persistent radio source (PRS): a compact, non-thermal synchrotron nebula around an FRB engine, unresolved at 3.7 by 1.7 milliarcsecond resolution. The key theoretical machinery is the nebular-model scaling L_nu = (64 $pi^{3}$ / 27) zeta_e $gamma_c^{2}$ m_e $c^{2}$ $R^{2}$ |RM|, which ties the PRS specific luminosity to the rotation measure of the FRB environment; placing the measured luminosity and RM = 338.1 rad $m^{-2}$ on this relation is what turns a 5.7-$\sigma$ VLBA detection into a physically meaningful association. The VLBA phase-referenced imaging at 5 GHz with 8 microjansky rms is the observational mechanism that secures the source's compactness and its position within the plus-or-minus 200 milliarcsecond error circle.

What would settle it

Re-image the field with VLBA at 5 GHz in a later epoch: if the 46 microjansky source is absent, or if a source-count estimate shows that the expected number of sources at or above 46 microjansky inside a 200 milliarcsecond radius is comparable to 1, the PRS association would be falsified.

Watch

Extended reading notes

Core claim

At 5 GHz with the VLBA, the authors detect an unresolved radio source offset about 50 milliarcseconds north of the PRECISE position of FRB 20240114A, with peak flux density 46 +/- 9 microjansky at 5.7 $\sigma$ and an angular resolution of 3.7 by 1.7 milliarcseconds. Because the source lies within the plus-or-minus 200 milliarcsecond FRB uncertainty, is unresolved at a physical scale below about 4 parsecs for the host redshift z = 0.13056, and has a brightness temperature above 7.8 x $10^{5}$ K and a specific luminosity of 2.2 x $10^{28}$ erg $s^{-1}$ $Hz^{-1}$, the authors conclude that it is the fourth persistent radio source associated with an FRB. Its luminosity together with the previously measured rotation measure of about 338 rad $m^{-2}$ places it on the predicted luminosity--rotation-measure relation for the nebular model, and optical spectroscopy of the host galaxy excludes an AGN origin, leaving a non-thermal compact nebula as the interpretation.

Load-bearing premise

The load-bearing premise is that the PRECISE localization confines the FRB to a 200 milliarcsecond circle and that the 46 microjansky VLBA source is not an unrelated background object, a chance-coincidence probability the paper does not compute.

Editorial extensions

If this is right

  • If the association holds, FRB 20240114A becomes the fourth repeating FRB with a compact persistent radio source, establishing that such sources are a recurring feature of hyperactive repeaters.
  • The source's position on the luminosity--rotation-measure relation extends the nebular-model validation by another object, supporting the idea that the RM screen and the PRS emission originate in the same magnetized environment.
  • With a brightness temperature above 7.8 x 10^5 K and a luminosity more than an order of magnitude above the brightest star-forming regions, the emission must be non-thermal synchrotron radiation rather than free--free emission from star formation.
  • The host galaxy's BPT line ratios place it in the star-forming sequence, excluding an AGN as the origin of the persistent emission and leaving a compact nebula around the FRB engine as the explanation.
  • If follow-up VLBI at 1--2 GHz confirms a flux density consistent with MeerKAT, this would be the first PRS with a peaked synchrotron spectrum, making it an intermediate case between the steep-spectrum and inverted-spectrum PRSs known previously.

Reading between the lines

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

  • A paper-implicit test is computing the chance-coincidence probability of a source at or above 46 microjansky at 5 GHz inside the 200 milliarcsecond error circle; the paper does not report this number, and a small probability would put the association on firmer statistical footing.
  • Because the PRS lies about 1 kiloparsec from the host center in a starburst galaxy, a natural extension is to search for a young supernova remnant or compact star cluster at that position in high-resolution optical or infrared data, which the paper does not do.
  • The spectral-peak constraint of nu_peak below about 0.65 GHz implies limits on the magnetic field and electron density in the emission region; combining those constraints with the measured RM could test whether the RM screen and the synchrotron-emitting nebula are truly co-located, a self-consistency check the paper leaves implicit.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. The paper reports VLBA 5 GHz continuum observations of FRB 20240114A, detecting an unresolved source at 46 ± 9 μJy (5.7σ) located ~50 mas from the PRECISE FRB position within the ±200 mas localization. It interprets this as the fourth persistent radio source (PRS) associated with an FRB, presents a radio spectrum using earlier MeerKAT/uGMRT data, and characterizes the host galaxy with LBT imaging and spectroscopy as a dwarf sub-solar metallicity starburst at z = 0.13056. The paper also places the new source on the luminosity versus |RM| nebular relation and claims further support for that model.

Significance. If the association is secure, the discovery adds a fourth PRS to a very small sample, with a host-galaxy environment distinct from some previous PRS hosts; the VLBA detection itself appears technically sound (5.7σ, unresolved, consistent e-Merlin upper limit, no other >5σ peaks in the localization region), and the host-galaxy photometry and spectroscopy are useful contributions. The paper's immediate impact, however, depends on establishing that the positional coincidence is not a chance superposition, which the manuscript currently does not do, and on framing the L–|RM| agreement as a consistency check rather than a validation.

major comments (3)
  1. [3.1] Section 3.1: The central claim that the VLBA source is a PRS associated with FRB 20240114A is based on a positional coincidence (source ~50 mas from the phase centre, within the ±200 mas PRECISE localization), but no quantitative chance-coincidence probability is given. Please compute the probability that an unrelated compact source with S_5GHz ≥ 46 μJy appears within a 200 mas radius of the FRB position, for example using 5 GHz source counts and including the background AGN population, and discuss the implications for the association. Without this calculation, an unrelated background source or a chance projection is not excluded and the 'associated PRS' claim is not yet secure.
  2. [5 / Appendix C] Section 5 and Eq. (C.6): The claim that the new source 'further supports' the nebular L–|RM| relation is not justified as presented, because Eq. (C.6) contains the unconstrained parameter combination ζe γ_c^2 (R/0.01 pc)^2 and the new point merely fixes this combination to ~10 (Fig. 3). Because the parameter can be adjusted from source to source, agreement with the plotted curves is a consistency check with a fitted parameter, not an independent validation. The authors should either provide an independent constraint on the parameter combination or revise the wording to state explicitly that the source is consistent with the relation for a particular value of the free parameter, and soften the claim of 'further supporting the model'.
  3. [3.2] The spectral index α = −0.34 ± 0.21 between 1.3 and 5 GHz is derived from the MeerKAT 1.3 GHz flux (72 ± 14 μJy) that includes the entire host galaxy at arcsecond resolution, while the 5 GHz point is parsec-scale. The argument that star-forming emission is limited (SFR_radio ~ 1.8 M_sun/yr vs. optical SFR < 1 M_sun/yr) shows that a large part of the 1.3 GHz flux is not ordinary star formation, but it does not quantify the upper half of the allowed range; a host contribution of up to several tens of μJy at 1.3 GHz could change α significantly. Please estimate and propagate this systematic uncertainty, or obtain VLBI observations at 1–2 GHz before making the spectral shape comparison in Fig. 1 and the abstract.
minor comments (6)
  1. [3.1] Please state whether the quoted 5.7σ significance accounts for the number of independent beams searched within the ±200 mas region; if not, give the trials-corrected significance or the false-positive probability for the search.
  2. [3.1] The phase centre is presumably the PRECISE nominal position, but the text should say this explicitly and also state the astrometric uncertainty of the PRECISE localization rather than only quoting the ±200 mas uncertainty.
  3. [3.2] The e-Merlin upper limit of <50 μJy is formally consistent with the VLBA detection of 46 ± 9 μJy but adds little constraint; a sentence explaining why a detection was not expected at e-Merlin resolution would help.
  4. [Figure 3] The caption should define ζe, γc, and R directly and note that the three curves correspond to fixed values of the free parameter combination, not to predictions with independently fixed parameters.
  5. [4.2 / Conclusions] The statement that the spectral properties 'exclude an AGN origin for the PRS' is too strong: the BPT diagrams classify the host galaxy's line-emitting gas as star-forming, but the compact radio source is 0.43″ from the nucleus and could in principle be unrelated to the line-emitting gas; please rephrase to say the host galaxy shows no evidence of AGN activity.
  6. [General] There are several language slips: 'northwards the nominal position' should be 'northwards of the nominal position'; 'different' is misspelled twice in the Introduction; 'staff' is misspelled in the Acknowledgements; and the Fig. B.4 caption contains 'diagram of diagram'.

Circularity Check

1 steps flagged · score 4.0 of 10

The VLBA detection and PRS association are independent and credible, but the claimed L–|RM| 'support' for the nebular model reduces to a free-parameter identity rather than a test.

  1. fitted input called prediction [Section 5, Fig. 3 and Appendix C, Eq. C.6]
    "Lν = 64π3/27 ζeγ2c mec2R2|RM| ≃ 5.7×1028 erg s−1 Hz−1 ζeγ2c (|RM|/104 rad m−2)(R/10−2 pc)2, (C.6) ... Meanwhile, the observed specific PRS luminosity of FRB 20240114A is close to the value of ζeγc(R/10−2 pc)2 ∼ 10."

    Equation C.6 is not a fixed prediction: it contains the unconstrained product ζeγc^2(R/0.01 pc)^2 multiplying |RM|. Given the measured Lν ≈ 2.2×10^28 erg s−1 Hz−1 and RM ≈ 338.1 rad m−2, solving Eq. C.6 for that product yields ≈ 10. Saying that the source lies near the ζeγc^2(R/0.01 pc)^2 = 10 curve is therefore algebraically identical to restating the measured Lν and RM; any single point can be placed on some member of the curve family by choosing the product. The abstract and conclusions describe this placement as 'further supporting' the nebular relation, but no independent constraint or prior on ζeγc^2(R/0.01 pc)^2 is given.

full rationale

The central observational claim is not circular. The VLBA detection is an independent, internally calibrated measurement: a 5.7σ unresolved source at 5 GHz with 46 ± 9 μJy, no other >5σ peak in the PRECISE ±200 mas region, and positional uncertainty dominated by the 0.03 mas phase-calibrator accuracy. The association with FRB 20240114A rests on this detection falling within the PRECISE localization, not on the theoretical L–|RM| relation. The host-galaxy analysis and spectral-index discussion are likewise independent of the relation. The one genuinely circular element is the claimed support for the nebular model: Eq. C.6 contains a multiplicative free parameter combination, and the new data point simply fixes that combination near 10. Calling this 'expected' or 'supporting' is a restatement of the measured luminosity and RM, not an independent test. The self-citations to Yang et al. (2020, 2022) and Bruni et al. (2024) are context, but they do not make the free-parameter relation more constraining. A separate non-circularity concern is that the paper never quantifies the chance-coincidence probability for an unrelated 46 μJy 5 GHz source inside the ±200 mas error circle; that is a statistical or correctness risk, not a circularity. Overall, the discovery claim is self-contained, while the nebular-model validation claim is partially circular, giving a score of 4 rather than a higher value that would apply if the PRS association itself reduced to the model fit.

Assumptions & free parameters 1 free parameters · 5 assumptions · 0 invented entities

The central detection is observational and does not rest on free parameters. The secondary claims (nebular model support, spectral shape, host properties) rely on model assumptions from prior work, particularly the L-RM scaling with its free normalization, and on indirect arguments about host galaxy contribution.

free parameters (1)
  • ζe γc^2 (R/0.01 pc)^2 = ~10
    The L-RM relation from Yang et al. (2020, 2022) has a free normalization involving the electron fraction ζe, the characteristic Lorentz factor γc, and the nebula radius R. The observed L and |RM| of FRB 20240114A only fix this combination to about 10, so the agreement is not a sharp prediction.
assumptions (5)
  • domain assumption The nebular model relation Lν = (64π^3/27) ζe γc^2 m_e c^2 R^2 |RM| (Eq. C.6) holds for PRSs.
    The paper uses this scaling from Yang et al. (2020, 2022) to claim the new PRS 'further supports its validity'. The model has not been derived from first principles for all FRBs and contains free microphysics parameters.
  • domain assumption The RM measured from FRB bursts (RM ~ 338.1 rad/m^2) and the PRS arise from the same magneto-ionic region.
    Section 5 states this as the basis for plotting L versus |RM|. If the RM is dominated by the host galaxy along the burst path rather than the PRS environment, the comparison is invalid.
  • domain assumption The host galaxy contribution to the MeerKAT and uGMRT flux densities is limited.
    Section 3.2 argues the radio flux implies SFR ~ 1.8 solar masses per year, larger than the optical SFR (< 1 solar mass per year), so star-forming regions cannot account for all the low-frequency flux. This is an indirect argument; a direct subtraction is not possible at arcsecond resolution.
  • domain assumption The PRECISE FRB localization uncertainty is correctly characterized as ±200 mas.
    The VLBA source is ~50 mas north of the nominal position, and the association relies on the claimed 200 mas uncertainty being accurate.
  • domain assumption The Calzetti relation E(B-V)_star = 0.4 E(B-V)_gas applies to the host galaxy.
    Used in the SED fitting (Appendix B.3) to fix stellar attenuation; the derived stellar mass is robust, but the SFR is degenerate with age.

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Pith. "Pith review of Discovery of a PRS associated with FRB 20240114A." pith.science (2026). https://pith.science/paper/DRN7CZPX

@misc{pith2026241201478,
  author       = {Pith},
  title        = {Pith review of: Discovery of a PRS associated with FRB 20240114A},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/DRN7CZPX}},
  note         = {Machine review of arXiv:2412.01478}
}
abstract

We present the discovery of the fourth persistent radio source (PRS) associated with a fast radio burst (FRB). Following previous indications of a candidate PRS associated with FRB20240114A, we performed deep VLBA observations at 5 GHz to test the presence of a compact radio source within the uncertainty position of this FRB ($\pm$200 mas). We detect a component $\sim$50 mas northwards the nominal position provided by the PRECISE collaboration. The corresponding radio luminosity, together with the Faraday rotation measure provided by previous observations of the FRB, locate this PRS in the expected region of the $L$ vs |RM| relation for the nebular model, further supporting it. The comparison of the measured flux density with the values collected at lower frequency by previous studies indicates a possible steepening of the radio spectrum in the 1-5 GHz range. Optical observations performed with the LBT could reveal that the FRB and its PRS lie at $\sim$1 kpc from the centre of the host galaxy, which is a dwarf sub-solar metallicity starburst galaxy with SFR $\sim 1 M_\odot\;\mathrm{yr^{-1}}$ and stellar mass $M\sim10^8 M_\odot$.

Figures

Figures reproduced from arXiv: 2412.01478 by the authors.

Figure 1
Figure 1. Left panel: Very Long Baseline Array image of the PRS at 5 GHz. The FWHM (3.7 [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Large Binocular Cameras r′ filter image. The PRS posi￾tion is marked by a plus sign, and the galaxy centre is marked with an ’x’. The slit used for the MODS spectrum is shown. The image pixel scale is 0′′ .23, and the RMS is 0.25 cts. The galaxy extension is ≃ 3 ′′ .2×2 ′′ .8. The uGMRT (red) and MeerKAT (gold) beams are also shown. 4. Host galaxy properties 4.1. Optical observations and SED fitting Photometric obse… view at source ↗
Figure 3
Figure 3. Proposed relation between the PRS specific radio luminosity and the FRB RM adopting the general nebula model from Yang [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 9 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. A flaring radio counterpart to a fast radio burst reveals a newborn magnetized engine

    astro-ph.HE 2025-01 conditional novelty 8.0 of 10

    A compact flaring radio source detected 26 days after FRB 20240114A's first burst shows a synchrotron self-absorption peak, implying a newborn, highly magnetized FRB engine.

  2. One year of broadband radio monitoring of the enigmatic transient GRB 250702B reveals the evolution of the relativistic jet

    astro-ph.HE 2026-08 conditional novelty 6.0 of 10

    A year of 0.65-233 GHz monitoring shows GRB 250702B's radio afterglow is a synchrotron forward shock in a stratified medium, with a jet that is either narrow and fast or wide and slow.

  3. Unveiling the Local Environment of FRB 20220912A: Sub-arcsecond $4-26$ GHz Radio Continuum Mapping

    astro-ph.HE 2026-07 conditional novelty 6.0 of 10

    A 75–190 pc non-thermal radio source coincident with FRB 20220912A is identified as a compact star-forming region with Σ_SFR ≳ 13 M☉/yr/kpc², supporting a young-magnetar progenitor channel.

  4. Long-term simultaneous 2.25/8.60~GHz monitoring of the newly-discovered repeating FRB~20240114A

    astro-ph.HE 2025-08 conditional novelty 6.0 of 10

    A year of simultaneous 2.25 and 8.60 GHz monitoring of FRB 20240114A caught 155 bursts at the low frequency, none at the high frequency, revealing strong frequency-dependent activity.

  5. The CHIME/FRB Discovery of the Extremely Active Fast Radio Burst Source FRB 20240114A

    astro-ph.HE 2025-05 conditional novelty 6.0 of 10

    FRB 20240114A, discovered by CHIME/FRB, is one of the most prolific repeating fast radio burst sources known: CHIME sees a stable dispersion measure near 528 pc cm^-3, a rotation measure near +320 rad m^-2, and a burs...

  6. The Host Galaxy of the Hyperactive Repeating FRB 20240114A: Behind a Galaxy Cluster

    astro-ph.GA 2025-02 conditional novelty 6.0 of 10

    The host of FRB 20240114A is a star-forming dwarf galaxy at z=0.1306, its ionized gas plus a foreground cluster can account for most of the excess dispersion measure, and repeater hosts differ from one-off hosts in th...

  7. Propagation-induced Frequency-dependent Polarization Properties of Fast Radio Burst

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    A new analytical model shows that fast radio burst polarization spectra can precess on the Poincaré sphere when Faraday rotation and conversion are comparable, offering a physical alternative to the empirical generali...

  8. No Strong Evidence for Plasma Lensing in FRB 20240114A

    astro-ph.HE 2026-07 conditional novelty 5.5 of 10

    FAST and Parkes data show misaligned magnification peaks, no bandwidth narrowing, and chance-level carbon-copy pairs, so plasma lensing is not required for FRB 20240114A variability.

  9. Low-frequency Probes of the Persistent Radio Sources associated with Repeating FRBs

    astro-ph.HE 2024-12 accept novelty 5.0 of 10

    A 650 MHz detection toward repeating FRB 20240114A is a persistent radio source in its host galaxy, while two other repeaters show only star formation or upper limits.

Reference graph

Works this paper leans on

64 extracted references · 30 canonical work pages · cited by 9 Pith papers

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

  3. [3]

    2020, , 249, 3

    Ahumada , R., Allende Prieto , C., Almeida , A., et al. 2020, , 249, 3

    2020

  4. [4]

    1999, , 310, 540

    Arnouts , S., Cristiani , S., Moscardini , L., et al. 1999, , 310, 540

    1999

  5. [5]

    V., Cid Fernandes , R., Stasi \'n ska , G., et al

    Asari , N. V., Cid Fernandes , R., Stasi \'n ska , G., et al. 2007, , 381, 263

    work page 2007

  6. [6]

    A., Phillips , M

    Baldwin , J. A., Phillips , M. M., & Terlevich , R. 1981, , 93, 5

    1981

  7. [7]

    2024, , 532, L14

    Bassini , L., Feldmann , R., Gensior , J., et al. 2024, , 532, L14

    work page 2024

  8. [8]

    & Arnouts , S

    Bertin , E. & Arnouts , S. 1996, , 117, 393

    1996

Show all 64 references
  1. [9]

    E., Aggarwal , K., et al

    Bhandari , S., Heintz , K. E., Aggarwal , K., et al. 2022, , 163, 69

    2022

  2. [10]

    M., Prochaska , J

    Bhandari , S., Sadler , E. M., Prochaska , J. X., et al. 2020, , 895, L37

    2020

  3. [11]

    2024, The Astronomer's Telegram, 16613, 1

    Bhardwaj , M., Kirichenko , A., & Gil de Paz , A. 2024, The Astronomer's Telegram, 16613, 1

    2024

  4. [12]

    Y., Michilli , D., et al

    Bhardwaj , M., Kirichenko , A. Y., Michilli , D., et al. 2021, , 919, L24

    2021

  5. [13]

    2024 a , The Astronomer's Telegram, 16820, 1

    Bhusare , Y., Maan , Y., & Kumar , A. 2024 a , The Astronomer's Telegram, 16820, 1

    2024

  6. [14]

    2024 b , arXiv e-prints, arXiv:2412.13121

    Bhusare , Y., Maan , Y., & Kumar , A. 2024 b , arXiv e-prints, arXiv:2412.13121

    2024 arXiv

  7. [15]

    D., Ravi , V., Belov , K

    Bochenek , C. D., Ravi , V., Belov , K. V., et al. 2020, , 587, 59

    2020

  8. [16]

    2019, , 622, A103

    Boquien , M., Burgarella , D., Roehlly , Y., et al. 2019, , 622, A103

    2019

  9. [17]

    2024, , 632, 1014

    Bruni , G., Piro , L., Yang , Y.-P., et al. 2024, , 632, 1014

    2024

  10. [18]

    1997, in American Institute of Physics Conference Series, Vol

    Calzetti , D. 1997, in American Institute of Physics Conference Series, Vol. 408, The ultraviolet universe at low and High redshift, ed. W. H. Waller (AIP), 403--412

    1997

  11. [19]

    2022, , 134, 114501

    CASA Team , Bean , B., Bhatnagar , S., et al. 2022, , 134, 114501

    2022

  12. [20]

    C., Magnier , E

    Chambers , K. C., Magnier , E. A., Metcalfe , N., et al. 2016, arXiv e-prints, arXiv:1612.05560

    2016 arXiv

  13. [21]

    J., Wharton , R

    Chatterjee , S., Law , C. J., Wharton , R. S., et al. 2017, , 541, 58

    2017

  14. [22]

    2025, , 980, L24

    Chen , X.-L., Tsai , C.-W., Li , D., et al. 2025, , 980, L24

    2025

  15. [23]

    2017, , 465, 1384

    Curti , M., Cresci , G., Mannucci , F., et al. 2017, , 465, 1384

    2017

  16. [24]

    A., Magnier , E

    Flewelling , H. A., Magnier , E. A., Chambers , K. C., et al. 2020, , 251, 7

    2020

  17. [25]

    S., Paris , D., et al

    Fontana , A., Dunlop , J. S., Paris , D., et al. 2014, , 570, A11

    2014

  18. [26]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2023, , 674, A1

    2023

  19. [27]

    2022, , 514, 2902

    Gargiulo , A., Fumana , M., Bisogni , S., et al. 2022, , 514, 2902

    2022

  20. [28]

    2008, , 482, 349

    Giallongo , E., Ragazzoni , R., Grazian , A., et al. 2008, , 482, 349

    2008

  21. [29]

    L., Drout , M

    Ibik , A. L., Drout , M. R., Gaensler , B. M., et al. 2024, , 961, 99

    2024

  22. [30]

    J., et al

    Ilbert , O., Arnouts , S., McCracken , H. J., et al. 2006, , 457, 841

    2006

  23. [31]

    M., Tremonti , C., et al

    Kauffmann , G., Heckman , T. M., Tremonti , C., et al. 2003, , 346, 1055

    2003

  24. [32]

    1998, , 36, 189

    Kennicutt , Robert C., J. 1998, , 36, 189

    1998

  25. [33]

    J., Groves , B., Kauffmann , G., & Heckman , T

    Kewley , L. J., Groves , B., Kauffmann , G., & Heckman , T. 2006, , 372, 961

    2006

  26. [34]

    2022, , 602, 585

    Kirsten , F., Marcote , B., Nimmo , K., et al. 2022, , 602, 585

    2022

  27. [35]

    S., Herrmann , W., et al

    Kirsten , F., Ould-Boukattine , O. S., Herrmann , W., et al. 2024, Nature Astronomy, 8, 337

    2024

  28. [36]

    Marcote , B., Paragi , Z., Hessels , J. W. T., et al. 2017, , 834, L8

    2017

  29. [37]

    Margalit , B., Berger , E., & Metzger , B. D. 2019, , 886, 110

    2019

  30. [38]

    & Metzger , B

    Margalit , B. & Metzger , B. D. 2018, , 868, L4

    2018

  31. [39]

    D., Berger , E., & Margalit , B

    Metzger , B. D., Berger , E., & Margalit , B. 2017, , 841, 14

    2017

  32. [40]

    2021, eMCP: e-MERLIN CASA pipeline , Astrophysics Source Code Library, record ascl:2109.006

    Moldon , J. 2021, eMCP: e-MERLIN CASA pipeline , Astrophysics Source Code Library, record ascl:2109.006

    2021

  33. [41]

    2016, , 461, 1498

    Murase , K., Kashiyama , K., & M \'e sz \'a ros , P. 2016, , 461, 1498

    2016

  34. [42]

    J., Condon , J

    Murphy , E. J., Condon , J. J., Schinnerer , E., et al. 2011, , 737, 67

    2011

  35. [43]

    2021, Universe, 7, 76

    Nicastro , L., Guidorzi , C., Palazzi , E., et al. 2021, Universe, 7, 76

    2021

  36. [44]

    H., Aggarwal , K., Li , D., et al

    Niu , C. H., Aggarwal , K., Li , D., et al. 2022, , 606, 873

    2022

  37. [45]

    Osterbrock , D. E. 1989, Astrophysics of gaseous nebulae and active galactic nuclei

    1989

  38. [46]

    2021, , 656, L15

    Piro , L., Bruni , G., Troja , E., et al. 2021, , 656, L15

    2021

  39. [47]

    W., Atwood , B., Brewer , D

    Pogge , R. W., Atwood , B., Brewer , D. F., et al. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 7735, Ground-based and Airborne Instrumentation for Astronomy III, ed. I. S. McLean , S. K. Ramsay , & H. Takami , 77350A

    2010

  40. [48]

    2009, , 691, 182

    Savaglio , S., Glazebrook , K., & Le Borgne , D. 2009, , 691, 182

    2009

  41. [49]

    Schlafly , E. F. & Finkbeiner , D. P. 2011, , 737, 103

    2011

  42. [50]

    2018, , 609, A30

    Schreiber , C., Elbaz , D., Pannella , M., et al. 2018, , 609, A30

    2018

  43. [51]

    & CHIME/FRB Collaboration

    Shin , K. & CHIME/FRB Collaboration . 2024, The Astronomer's Telegram, 16420, 1

    2024

  44. [52]

    P., Bhandari , S., Kirsten , F., et al

    Snelders , M. P., Bhandari , S., Kirsten , F., et al. 2024, The Astronomer's Telegram, 16542, 1

    2024

  45. [53]

    P., Bassa , C

    Tendulkar , S. P., Bassa , C. G., Cordes , J. M., et al. 2017, , 834, L7

    2017

  46. [54]

    P., Gil de Paz , A., Kirichenko , A

    Tendulkar , S. P., Gil de Paz , A., Kirichenko , A. Y., et al. 2021, , 908, L12

    2021

  47. [55]

    M., Pastor-Marazuela , I., et al

    Tian , J., Rajwade , K. M., Pastor-Marazuela , I., et al. 2024, , 533, 3174

    2024

  48. [56]

    1993, in Astronomical Society of the Pacific Conference Series, Vol

    Tody , D. 1993, in Astronomical Society of the Pacific Conference Series, Vol. 52, Astronomical Data Analysis Software and Systems II, ed. R. J. Hanisch, R. J. V. Brissenden, & J. Barnes , 173

    1993

  49. [57]

    2020, , 895, 7

    Yang , Y.-P., Li , Q.-C., & Zhang , B. 2020, , 895, 7

    2020

  50. [58]

    2022, , 928, L16

    Yang , Y.-P., Lu , W., Feng , Y., Zhang , B., & Li , D. 2022, , 928, L16

    2022

  51. [59]

    2016, , 819, L12

    Yang , Y.-P., Zhang , B., & Dai , Z.-G. 2016, , 819, L12

    2016

  52. [60]

    2020, , 587, 45

    Zhang , B. 2020, , 587, 45

    2020

  53. [61]

    2023, Reviews of Modern Physics, 95, 035005

    Zhang , B. 2023, Reviews of Modern Physics, 95, 035005

    2023

  54. [62]

    2024, The Astronomer's Telegram, 16505, 1

    Zhang , J., Wu , Q., Cao , S., et al. 2024, The Astronomer's Telegram, 16505, 1

    2024

  55. [63]

    & Yu , W

    Zhang , X. & Yu , W. 2024, The Astronomer's Telegram, 16695, 1

    2024

  56. [64]

    2025, arXiv e-prints, arXiv:2501.14247

    Zhang , X., Yu , W., Yan , Z., Xing , Y., & Zhang , B. 2025, arXiv e-prints, arXiv:2501.14247

    2025 arXiv

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.