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REVIEW 3 major objections 8 minor 77 references

Discovery of Odd Radio Circles and Other Peculiars in the First Year of the EMU Survey using Object Detection

T0 review · 3 major / 8 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Five new Odd Radio Circles discovered in the first-year EMU survey data.

desk verdict A useful ML search pipeline and a plausible set of new ORC candidates, but the central claim that these are five new ORCs is stronger than the evidence supports. read the letter →

arxiv 2506.08439 v1 pith:VDX5FSJ3 submitted 2025-06-10 astro-ph.GA astro-ph.CO

Nikhel Gupta , Ray P. Norris , Zeeshan Hayder , Minh Huynh , Heinz Andernach , Andrew M. Hopkins , Stanislav Shabala , Lawrence Rudnick
show 4 more authors
Miroslav D. Filipović Bärbel S. Koribalski Lars Petersson X. Rosalind Wang
This is my paper
classification astro-ph.GAastro-ph.CO
keywords OddRadioCirclesmorphologyEMUsurveyASKAPobjectdetectionmachinelearningdiffuseemissionstarburstrings
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 reports that a supervised object-detection model, applied to 4,500 square degrees of the first-year EMU survey, identified five new Odd Radio Circles (ORCs) and two candidate ORCs, growing the known population from five to at least ten confirmed or candidate systems. It also returns 55 Galaxies with Large-scale Ambient Radio Emission (GLAREs), diffuse rings or blobs around distant galaxies that may be precursors or later-stage ORCs, and 18 Starburst Radio Ring Galaxies (SRRGs). A hybrid pipeline filtered roughly three million radio sources down to 1,794 candidates for human visual inspection, making the discovery efficient at survey scale. The paper argues that ORCs remain edge-brightened rings around host galaxies with no corresponding optical or infrared ring, and that the GLARE population offers a way to test evolutionary links between these structures.

What carries the argument

The machinery is a supervised object-detection system built around Gal-DINO, a transformer-based detector trained on RadioGalaxyNET and a set of atypical radio morphologies. Extended by the RG-CAT pipeline, it scans 8-arcminute cutouts around each of roughly three million Selavy-detected radio sources, predicts a bounding box, a category, and a keypoint marking the likely infrared host, and ranks sources by confidence. Filtering for the rare-or-peculiar category at a confidence threshold of 0.7 cuts the sample to 1,794 sources for visual inspection. This is the mechanism that turns a survey-wide search into a manageable human review while keeping the ORC-like morphologies.

What would settle it

A deep, arcsecond-resolution radio image of any of the five ORCs and two candidates, combined with optical spectroscopy of every galaxy inside the ring, would settle the classification: if the ring resolves into two opposed radio lobes connected by jets, if no galaxy lies near the ring centre, or if the designated host's redshift places it far from the ring's centre, then the ORC interpretation fails.

Watch

Extended reading notes

Core claim

The central discovery is that machine-learning object detection can systematically find a rare radio morphology that was previously found by chance. Applying the Gal-DINO detector and the RG-CAT catalogue pipeline to 160 tiles of the first-year EMU main survey, the authors identify five new ORCs (J0210-5710, J0402-5321, J0452-6231, J1313-4709, and J2304-7129) and two unconfirmed candidates (J0510-5825 and J1104-6351), each an edge-brightened circular radio structure with a distant galaxy near its centre and no detectable extended optical or infrared ring. All but one host lack spectroscopic redshifts, with photometric redshifts placing the systems at roughly 0.1 to 0.6 and physical diameters of roughly 160 to 440 kiloparsecs. In the same sample the paper classifies 55 GLAREs and 18 SRRGs, and proposes that GLAREs may be precursors or later evolutionary stages of ORCs. If accepted, the known ORC population grows from the five objects in the literature to at least ten, giving the first statistical footing for formation models.

Load-bearing premise

The search's central premise is that each edge-brightened radio ring is a real ORC physically associated with the WISE galaxy at its centre, rather than a chance projection of a double-lobed radio galaxy, a cluster radio relic, an imaging artifact, or an unrelated galaxy along the line of sight.

Editorial extensions

If this is right

  • The known ORC population grows from five to at least ten confirmed or candidate systems, providing a larger sample for testing formation mechanisms.
  • The rate of two ORCs in 270 square degrees of the pilot survey implies roughly 33 ORCs in the 4,500 square degrees covered here, so the full EMU survey should yield many more.
  • The 55 GLAREs give a substantial sample for testing whether diffuse ambient radio emission evolves into edge-brightened rings through shocks from mergers or starbursts.
  • Reducing roughly three million sources to 1,794 visual inspections shows that supervised object detection can make searches for rare radio morphologies practical as next-generation surveys grow larger.
  • Multi-wavelength follow-up of the new systems can distinguish between the relic-lobe shock model and the spherical-shell shockwave model for ORC formation.

Reading between the lines

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

  • If the ORC-GLARE evolutionary sequence is real, rectangular GLAREs viewed along their long axis may be classical double-lobed or remnant radio galaxies, which would tie ORCs to the life cycle of dying radio galaxies and predict spectral-index gradients across the rings.
  • The same detector, retrained on the appropriate resolution, should transfer to northern surveys such as LoTSS and to future SKA data, potentially revealing ORC-like rings in sky areas not covered by EMU.
  • Because most host redshifts are photometric, the derived sizes, luminosities, and star formation rates carry large uncertainties; spectroscopic redshifts for the five hosts could shift which galaxy is considered the central host and change the physical interpretation.
  • A direct test of the paper's implied surface density is to run the identical pipeline on the remaining EMU tiles as they are released; finding far fewer or far more than the expected rate would indicate selection effects or a change in ORC frequency with environment.
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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 / 8 minor

Summary. The paper presents a systematic search for Odd Radio Circles (ORCs) and other unusual radio morphologies in the first year of the EMU survey, using the Gal-DINO object detection model to reduce ~3 million radio detections to 1,794 visually inspected candidates. The authors report five new ORCs, two additional ORC candidates, 55 GLAREs, and 18 SRRGs, and propose that GLAREs may be evolutionary precursors or descendants of ORCs. The ORC identification rests on visual ring morphology, absence of Galactic counterparts, and a positionally coincident WISE/DESI galaxy, with flux densities, sizes, and photometric redshifts tabulated in Table 1.

Significance. If the five new ORCs are confirmed, the known population would more than triple, making this a significant contribution to the study of a rare and poorly understood class. The paper's strengths include public availability of the model and data, a transparent candidate table, and the independent verification of photometric redshifts from multiple catalogues. The main weakness is that the central claim---that these are genuine ORCs---depends on classification criteria that the paper itself acknowledges are difficult to separate from double-lobed radio galaxies, relic lobes, or unrelated diffuse emission. The stress-test concern is valid: the evidence presented in §4 establishes round, non-Galactic radio structures but does not yet establish the strict ORC definition cited from Norris et al. (2025).

major comments (3)
  1. [§4 and §5.1] The paper's own definition of an ORC in §4 explicitly excludes rings originating from the relic lobes of double-lobed radio galaxies, yet §5.1 concedes that some GLAREs 'could be classical double-lobed or remnant radio galaxies viewed near their major radio axis' and that hostless diffuse sources might be 'fading relic radio lobes with re-energized electrons' (citing Shabala et al. 2024). Footnote j in §5.1 further notes that previously published ORC2 and ORC3 have now been removed from the ORC list (Norris et al. 2025). For the five new objects, the paper provides no spectral-index, polarization, or higher-resolution data that would rule out these mimics. The evidence in §4 (edge-brightened ring, absence of HASH/Green counterparts, and a WISE/DESI galaxy near the centre) establishes 'round and non-Galactic' but not 'ORC' in the restricted sense used by the authors. I recommend either adding discriminating observations or changing the claim to 'ORC candidates' throughout the abstract and conclusions.
  2. [Table 1 and §§4.1–4.6] Host association is the load-bearing step for each claimed ORC, but it is only position-based for all but one object. Only J2304-7129 has a spectroscopic redshift; the other four hosts rely on photometric redshifts, and J1313-4709 has no redshift at all. The paper does not quantify the chance-alignment probability between the radio ring and a random WISE galaxy. In several cases the text itself acknowledges the ambiguity: §4.2 says three galaxies within the ring of J0402-5321 'may have contributed' to the circular structure, §4.1 mentions faint galaxies near the ring that 'may have contributed to the observed radio emission', and §4.6 states for candidate J0510-5825 that 'we cannot conclusively determine that the circular emission originates solely from the central galaxy'. A positional-coincidence test, even a simple surface-density argument using WISE galaxy counts, is needed to support the claim that these rings are associated with the designated hosts.
  3. [§3.3 and §5.1] The search methodology and the associated expected-number estimate both rest on uncharacterized selection effects. The Gal-DINO model was trained on previously known ORCs and rare morphologies and then applied to search for more ORCs, which is a reasonable discovery strategy but not one that allows completeness claims. The confidence threshold of 0.7 was set after visual inspection of a subset of the same survey tiles, and no independent validation set is used to estimate false positives or completeness. Similarly, the statement in §5.1 that 'we would expect approximately 33 ORCs in the ~4,500 deg2' is based on two ORCs in a 270 deg² pilot field, which is a very small number and ignores the selection function of the ML pipeline. The paper's phrase 'systematic search' in the abstract should therefore be tempered, and the expected-number comparison should be presented with appropriate uncertainties or removed.
minor comments (8)
  1. [§4.3] The host name for ORC J0452-6231 is given as WISEA J045230.76−623123.8 in Table 1 but as WISEA J045221.40−623422.7 in the text; these are inconsistent and should be reconciled.
  2. [§5.1] The source J0318-5708 is listed in Table 5 as a diffuse source without a plausible host, but in the text it is cited as an example of a GLARE with multiple galaxies at similar redshifts; the classification should be made consistent.
  3. [§5.1] The text refers to 'The source J1407-0197, shown in Figure 6'; this appears to be a typo for J1407-0917, which is the source displayed in Figure 6 and listed in Table 5.
  4. [Figure 7 caption] The caption contains the typo 'Eaxamples' and should read 'Examples'.
  5. [§4.6] The phrase 'Greens's catalogue' should be 'Green's catalogue'.
  6. [References] In the reference list, the Parker et al. entry contains 'V ol' instead of 'Vol.', and the Introduction refers to 'MW A' instead of 'MWA'.
  7. [§3.3] The phrase 'the model's minimum estimated threshold' is not defined in this paper; the reader must consult Gupta et al. (2024b) to understand how that threshold is derived.
  8. [§5.1] The expected number of ~33 ORCs is quoted without an uncertainty; given that it is based on two detections, a Poisson error estimate would be more appropriate.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity found: the new ORC/GLARE/SRRG sample is an empirical census from independent EMU data, not a derivation forced by training inputs or self-citations.

full rationale

The paper's central claim is an empirical census of new ORCs and related morphologies in the first-year EMU data, not a derivation from a fitted model. The object detector Gal-DINO was trained on previously known radio morphologies, including a small number of ORCs, and the confidence threshold was chosen after inspecting 25 tiles; neither step makes the newly reported objects equivalent to training inputs or to the threshold. The five new ORCs are identified by edge-brightened ring morphology on 15'' EMU images, the absence of HASH/Greene counterparts, and a positionally coincident WISE/DESI host; these are independent criteria that can fail, and the text explicitly considers alternative interpretations such as relic lobes and double-lobed projections. The Section 5.1 consistency check, which folds GLAREs into an expected ORC count, is an interpretive comparison rather than a prediction forced by construction, and it does not feed back into the classification of the five ORCs. Self-citations (Norris et al. 2021b, 2025; Gupta et al. 2022, 2024a,b) supply definitions and training data, but the reported classifications are applied to new, independent EMU tiles and are falsifiable by future spectral-index, polarization, and high-resolution follow-up. No step reduces by construction to its own inputs: no fitted parameter is renamed as a prediction, no uniqueness theorem is imported from overlapping-authors work, and no known result is merely relabeled. Therefore the circularity score is 0.

Assumptions & free parameters 2 free parameters · 4 assumptions · 1 invented entities

The central existence claims require assuming the rings are extragalactic, the central WISE galaxies are the hosts, and the images are free of artifacts. The ML threshold and the assumed spectral index are choices rather than fitted physical parameters of the objects themselves.

free parameters (2)
  • Confidence score threshold = 0.7
    Chosen after visually inspecting candidates in 25 random EMU tiles; no interesting sources were found below 0.8, so the threshold was set to 0.7 to be conservative (Section 3.3).
  • Assumed radio spectral index = -0.7
    Used to convert 944 MHz flux density to radio luminosity and star formation rate for ORCs and hosts (Section 4, Table 1). This is a standard assumption but is not measured here.
assumptions (4)
  • domain assumption The detected circular radio structures are not planetary nebulae or supernova remnants
    Cross-checked against HASH and Green catalogues, but no other Galactic or instrumental origin is excluded (Section 4).
  • domain assumption The WISE-selected galaxy at the ring centre is the physical host of the radio emission
    Host association is based on positional coincidence; some ORCs have multiple galaxies within the ring, so the association is not unique (e.g., ORC J0402-5321, J1313-4709).
  • domain assumption The EMU survey images are free of artifacts that mimic ring-like diffuse emission
    Implicit throughout the analysis; no explicit artifact rejection is described beyond visual inspection.
  • ad hoc to paper The object detection model's rare/peculiar class and confidence threshold capture the relevant ORC population
    The model is trained on known ORCs and a small sample of peculiar morphologies; completeness of the search is not quantified (Sections 3.1, 3.3).
invented entities (1)
  • GLARE (Galaxy with Large-scale Ambient Radio Emission)
    purpose: A proposed new observational class of diffuse radio emission around galaxies, suggested to be related to ORCs
    The class is introduced to group 55 newly identified sources, but the definition is broad and lacks quantitative selection criteria. No falsifiable prediction is made beyond the morphological description, and the ORC connection is speculative (Section 5.1).

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Cite this review

Pith. "Pith review of Discovery of Odd Radio Circles and Other Peculiars in the First Year of the EMU Survey using Object Detection." pith.science (2026). https://pith.science/paper/VDX5FSJ3

@misc{pith2026250608439,
  author       = {Pith},
  title        = {Pith review of: Discovery of Odd Radio Circles and Other Peculiars in the First Year of the EMU Survey using Object Detection},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/VDX5FSJ3}},
  note         = {Machine review of arXiv:2506.08439}
}
read the original abstract

We present a systematic search for Odd Radio Circles (ORCs) and other unusual radio morphologies using data from the first year of the EMU (Evolutionary Map of the Universe) survey. ORCs are rare, enigmatic objects characterized by edge-brightened rings of radio emission, often found in association with distant galaxies. To identify these objects, we employ a hybrid methodology combining supervised object detection techniques and visual inspection of radio source candidates. This approach leads to the discovery of five new ORCs and two additional candidate ORCs, expanding the known population of these objects. In addition to ORCs, we also identify 55 Galaxies with Large-scale Ambient Radio Emission (GLAREs), which feature irregular, rectangular, or circular shapes of diffuse radio emission mostly surrounding central host galaxies. These GLAREs may represent different evolutionary stages of ORCs, and studying them could offer valuable insights into their evolutionary processes. We also highlight a subset of Starburst Radio Ring Galaxies (SRRGs), which are star-forming galaxies exhibiting edge-brightened radio rings surrounding their central star-forming regions. We emphasize the importance of multi-wavelength follow-up observations to better understand the physical properties, host galaxy characteristics, and evolutionary pathways of these radio sources.

Figures

Figures reproduced from arXiv: 2506.08439 by the authors.

Figure 1
Figure 1. The footprint of the first year of the EMU main survey, conducted between February 2023 and March 2024 (tiles SBID 45638 to 59612 in [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. ORCs in the first year of the EMU survey. The panels display radio images (left), corresponding infrared images (middle), and optical [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. The top panel shows the WISE colours of the two ORC host [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: ORC candidates with unconfirmed host galaxies are presented. Details about the panels are provided in Figure 2. The corresponding optical [PITH_FULL_IMAGE:figures/full_fig_p010_4.png]
Figure 5
Figure 5. Figure 5: Examples of Galaxies with Large-scale Ambient Radio Emission (GLAREs). The left panels of each column display radio images from [PITH_FULL_IMAGE:figures/full_fig_p012_5.png]
Figure 6
Figure 6. Figure 6: An example of a diffuse radio source without a plausible host galaxy (left panel), as seen in the infrared W1 band from the AllWISE [PITH_FULL_IMAGE:figures/full_fig_p016_6.png]
Figure 7
Figure 7. Figure 7: Eaxamples of Starburst Radio Ring Galaxies (SRRGs) identified in the first year of the EMU survey. A notable characteristic of these [PITH_FULL_IMAGE:figures/full_fig_p016_7.png]

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Works this paper leans on

77 extracted references · 59 canonical work pages

  1. [1]

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

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution 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 :=...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.doi doi empty "" "doi:" doi * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix ":" * if eprint field.or.null * if FUNCTION format.pid eprint empty format.doi format.eprint if FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "-...

  3. [3]

    2020, , 249, 3

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

    2020

  4. [4]

    2021, , 500, 1633

    Beck , R., Szapudi , I., Flewelling , H., et al. 2021, , 500, 1633

    work page 2021

  5. [5]

    H., Peacock , J

    Bilicki , M., Jarrett , T. H., Peacock , J. A., Cluver , M. E., & Steward , L. 2014, , 210, 9

    work page 2014

  6. [6]

    A., Jarrett , T

    Bilicki , M., Peacock , J. A., Jarrett , T. H., et al. 2016, , 225, 5

    work page 2016

  7. [7]

    1986, , 61, 609

    Buta , R. 1986, , 61, 609

    work page 1986

  8. [8]

    L., Perrotta , S., Rupke , D

    Coil , A. L., Perrotta , S., Rupke , D. S. N., et al. 2024, , 625, 459

    work page 2024

Show all 77 references
  1. [9]

    M., Wright , E

    Cutri , R. M., Wright , E. L., Conrow , T., et al. 2021, VizieR Online Data Catalog, II/328

    2021

  2. [10]

    R., Gough , R

    DeBoer , D. R., Gough , R. G., Bunton , J. D., et al. 2009, IEEE Proceedings, 97, 1507

    2009

  3. [11]

    M., Koribalski , B

    Dolag , K., B \"o ss , L. M., Koribalski , B. S., Steinwandel , U. P., & Valentini , M. 2023, , 945, 74

    2023

  4. [12]

    Duncan , K. J. 2022, , 512, 3662

    2022

  5. [13]

    Ekers , R. D. 2009, in Proceedings of the special session ``Accelerating the Rate of Astronomical Discovery'' of the 27th IAU General Assembly. August 11-14 2009. Rio de Janeiro, 7

    2009

  6. [14]

    Elmegreen , B. G. 1994, , 425, L73

    1994

  7. [15]

    L., & Riley , J

    Fanaroff , B. L., & Riley , J. M. 1974, MNRAS, 167, 31P

    1974

  8. [16]

    A., Norris , R

    Forbes , D. A., Norris , R. P., Williger , G. M., & Smith , R. C. 1994, , 107, 984

    1994

  9. [17]

    Green , D. A. 2025, Journal of Astrophysics and Astronomy, 46, 14

    2025

  10. [18]

    P., Huynh , M., & Petersson , L

    Gupta , N., Hayder , Z., Norris , R. P., Huynh , M., & Petersson , L. 2024 a , , 41, e001

    2024

  11. [19]

    P., Hyunh , M., & Petersson , L

    Gupta , N., Hayder , Z., Norris , R. P., Hyunh , M., & Petersson , L. 2023, NeurIPS ML4PS 2023, arXiv:2312.06728

    2023 arXiv

  12. [20]

    P., et al

    Gupta , N., Huynh , M., Norris , R. P., et al. 2022, , 39, e051

    2022

  13. [21]

    P., et al

    Gupta, N., Hayder, Z., Norris, R. P., et al. 2023, Publications of the Astronomical Society of Australia, 40, e044

    2023

  14. [22]

    P., Hayder , Z., et al

    Gupta , N., Norris , R. P., Hayder , Z., et al. 2024 b , , 41, e027

    2024

  15. [23]

    in preparation

    Gupta et al. in preparation

  16. [24]

    M., Kapinska, A., Marvil, J., et al

    Hopkins, A. M., Kapinska, A., Marvil, J., et al. 2025, Publications of the Astronomical Society of Australia, 1–32

    2025

  17. [25]

    W., Bunton , J

    Hotan , A. W., Bunton , J. D., Chippendale , A. P., et al. 2021, PASA, 38, e009

    2021

  18. [26]

    2007, , 24, 174

    Johnston , S., Bailes , M., Bartel , N., et al. 2007, , 24, 174

    2007

  19. [27]

    2016, in MeerKAT Science: On the Pathway to the SKA, 1

    Jonas , J., & MeerKAT Team . 2016, in MeerKAT Science: On the Pathway to the SKA, 1

    2016

  20. [28]

    H., Read , M

    Jones , D. H., Read , M. A., Saunders , W., et al. 2009, , 399, 683

    2009

  21. [29]

    S., Norris , R

    Koribalski , B. S., Norris , R. P., Andernach , H., et al. 2021, , 505, L11

    2021

  22. [30]

    S., Veronica , A., Dolag , K., et al

    Koribalski , B. S., Veronica , A., Dolag , K., et al. 2024 a , , 531, 3357

    2024

  23. [31]

    S., Khabibullin , I., Dolag , K., et al

    Koribalski , B. S., Khabibullin , I., Dolag , K., et al. 2024 b , , 532, 3682

    2024

  24. [32]

    2024 a , , 683, A175

    Kumari , S., & Pal , S. 2024 a , , 683, A175

    2024

  25. [33]

    2024 b , , 527, 11233

    ---. 2024 b , , 527, 11233

    2024

  26. [34]

    W., & Mykytyn, D

    Lang, D., Hogg, D. W., & Mykytyn, D. 2016, Astrophysics Source Code Library, ascl

    2016

  27. [35]

    M., Sturch , C

    Lasker , B. M., Sturch , C. R., McLean , B. J., et al. 1990, , 99, 2019

    1990

  28. [36]

    2024, , 690, A310

    Lastufka , E., Bait , O., Taran , O., et al. 2024, , 690, A310

    2024

  29. [37]

    2024, arXiv e-prints, arXiv:2411.04188

    Lochner , M., & Rudnick , L. 2024, arXiv e-prints, arXiv:2411.04188

    2024 arXiv

  30. [38]

    Lochner , M., Rudnick , L., Heywood , I., Knowles , K., & Shabala , S. S. 2023, , 520, 1439

    2023

  31. [39]

    L., Maraston , C., Nichol , R

    Masters , K. L., Maraston , C., Nichol , R. C., et al. 2011, , 418, 1055

    2011

  32. [40]

    2024, , 530, 1274

    Mohale , K., & Lochner , M. 2024, , 530, 1274

    2024

  33. [41]

    Mostert , R. I. J., Duncan , K. J., R \"o ttgering , H. J. A., et al. 2021, , 645, A89

    2021

  34. [42]

    J., Condon , J

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

    2011

  35. [43]

    2015, Monthly Notices of the Royal Astronomical Society, 447, 3612

    Nims, J., Quataert, E., & Faucher-Giguère, C.-A. 2015, Monthly Notices of the Royal Astronomical Society, 447, 3612

    2015

  36. [44]

    2015, in Advancing Astrophysics with the Square Kilometre Array (AASKA14), 86

    Norris , R., Basu , K., Brown , M., et al. 2015, in Advancing Astrophysics with the Square Kilometre Array (AASKA14), 86

    2015

  37. [45]

    Norris , R. P. 2011, Journal of Astrophysics and Astronomy, 32, 599

    2011

  38. [46]

    P., Koribalski , B

    Norris , R. P., Koribalski , B. S., Hale , C. L., et al. 2025, , 537, L42

    2025

  39. [47]

    P., Marvil , J., Collier , J

    Norris , R. P., Marvil , J., Collier , J. D., et al. 2021 a , , 38, e046

    2021

  40. [48]

    P., Intema , H

    Norris , R. P., Intema , H. T., Kapi \'n ska , A. D., et al. 2021 b , , 38, e003

    2021

  41. [49]

    P., Collier , J

    Norris , R. P., Collier , J. D., Crocker , R. M., et al. 2022, , 513, 1300

    2022

  42. [50]

    2022, Research Notes of the American Astronomical Society, 6, 100

    Omar , A. 2022, Research Notes of the American Astronomical Society, 6, 100

    2022

  43. [51]

    A., Boji c i \'c , I., & Frew , D

    Parker , Q. A., Boji c i \'c , I., & Frew , D. J. 2017, in Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution, ed. X. Liu , L. Stanghellini , & A. Karakas , Vol. 323, 36--39

    2017

  44. [52]

    A., Chandler , C

    Perley , R. A., Chandler , C. J., Butler , B. J., & Wrobel , J. M. 2011, APJ, 739, L1

    2011

  45. [53]

    2020, , 641, A6

    Planck Collaboration , Aghanim , N., Akrami , Y., et al. 2020, , 641, A6

    2020

  46. [54]

    2024, , 41, e085

    Riggi , S., Cecconello , T., Palazzo , S., et al. 2024, , 41, e085

    2024

  47. [55]

    Rupke , D. S. N., Coil , A. L., Whalen , K. E., et al. 2024, , 967, 51

    2024

  48. [56]

    K., Schlafly , E

    Saydjari , A. K., Schlafly , E. F., Lang , D., et al. 2023, , 264, 28

    2023

  49. [57]

    F., & Finkbeiner , D

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

    2011

  50. [58]

    2021, in American Astronomical Society Meeting Abstracts, Vol

    Schlegel , D., Dey , A., Herrera , D., et al. 2021, in American Astronomical Society Meeting Abstracts, Vol. 53, American Astronomical Society Meeting Abstracts, 235.03

    2021

  51. [59]

    J., Finkbeiner , D

    Schlegel , D. J., Finkbeiner , D. P., & Davis , M. 1998, , 500, 525

    1998

  52. [60]

    2022, arXiv e-prints, arXiv:2206.14677

    Segal , G., Parkinson , D., Norris , R., et al. 2022, arXiv e-prints, arXiv:2206.14677

    2022 arXiv

  53. [61]

    S., Yates-Jones , P

    Shabala , S. S., Yates-Jones , P. M., Jerrim , L. A., et al. 2024, , 41, e024

    2024

  54. [62]

    W., Hardcastle , M

    Shimwell , T. W., Hardcastle , M. J., Tasse , C., et al. 2022, , 659, A1

    2022

  55. [63]

    V., Scaife , A

    Slijepcevic , I. V., Scaife , A. M. M., Walmsley , M., et al. 2024, RAS Techniques and Instruments, 3, 19

    2024

  56. [64]

    C., Sobacchi, E., & Sanders, J

    Sormani, M. C., Sobacchi, E., & Sanders, J. L. 2024, Monthly Notices of the Royal Astronomical Society, 528, 5742

    2024

  57. [65]

    L., Denneau , L., Flewelling , H., et al

    Tonry , J. L., Denneau , L., Flewelling , H., et al. 2018, , 867, 105

    2018

  58. [66]

    P., Wise , M

    van Haarlem , M. P., Wise , M. W., Gunst , A. W., et al. 2013, , 556, A2

    2013

  59. [67]

    Walmsley , M., Scaife , A. M. M., Lintott , C., et al. 2022, , 513, 1581

    2022

  60. [68]

    B., Tingay , S

    Wayth , R. B., Tingay , S. J., Trott , C. M., et al. 2018, , 35, e033

    2018

  61. [69]

    L., & Han , J

    Wen , Z. L., & Han , J. L. 2024, , 272, 39

    2024

  62. [70]

    2012, , 29, 371

    Whiting , M., & Humphreys , B. 2012, , 29, 371

    2012

  63. [71]

    2017, in Astronomical Society of the Pacific Conference Series, Vol

    Whiting , M., Voronkov , M., Mitchell , D., & Askap Team . 2017, in Astronomical Society of the Pacific Conference Series, Vol. 512, Astronomical Data Analysis Software and Systems XXV, ed. N. P. F. Lorente , K. Shortridge , & R. Wayth , 431

    2017

  64. [72]

    L., Eisenhardt , P

    Wright , E. L., Eisenhardt , P. R. M., Mainzer , A. K., et al. 2010, , 140, 1868

    2010

  65. [73]

    Zaw , I., Chen , Y.-P., & Farrar , G. R. 2019, , 872, 134

    2019

  66. [74]

    A., Mao , Y.-Y., et al

    Zhou , R., Newman , J. A., Mao , Y.-Y., et al. 2021, , 501, 3309

    2021

  67. [75]

    2025, , 536, 2260

    Zhou , X., Li , N., Zou , H., et al. 2025, , 536, 2260

    2025

  68. [76]

    2019, The Astrophysical Journal Supplement Series, 242, 8

    Zou, H., Gao, J., Zhou, X., & Kong, X. 2019, The Astrophysical Journal Supplement Series, 242, 8

    2019

  69. [77]

    2022, Research in Astronomy and Astrophysics, 22, 065001

    Zou , H., Sui , J., Xue , S., et al. 2022, Research in Astronomy and Astrophysics, 22, 065001

    2022

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.