Pith. sign in

REVIEW 2 major objections 5 minor 93 references

JWST/MIRI finds 928 red mid-IR sources in Cen A that track the warped disc and recent star formation, not the radio jet.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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

T0 review · grok-4.5

2026-07-11 11:08 UTC pith:JWN6WEC4

load-bearing objection Clean first JWST/MIRI census of Cen A’s disc that delivers a solid geometric test of merger-driven vs jet-driven star formation; YSO classification is the only soft spot and is already caveated. the 2 major comments →

arxiv 2607.04942 v1 pith:JWN6WEC4 submitted 2026-07-06 astro-ph.GA astro-ph.SR

MICONIC: The spatial relationship between star formation and the AGN in Centaurus A revealed by JWST/MIRI

O. C. Jones , M. L. Jones , D. Dicken , G. S. Wright , M. Garc\'ia Mar\'in , A. Alonso Herrero , P. Guillard , K. Justtanont
show 16 more authors
M. Meixner A. Labiano D. Rouan P. van der Werf L. Pantoni V. A. Buiten T. B\"oker G. \"Ostlin L. Evangelista M. Baes L. Colina L. Hermosa Mu\~noz Th. Henning M. G\"udel T. P. Ray P.-O. Lagage
This is my paper
classification astro-ph.GA astro-ph.SR
keywords Centaurus AJWST/MIRIstar formationyoung stellar objectswarped dust discAGN jet-ISM interactionmid-infrared photometry
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Centaurus A is the nearest active radio galaxy and hosts a warped dust disc left over from a gas-rich merger. This paper uses JWST/MIRI imaging in three mid-infrared filters over a roughly 4 by 2 kpc central region to resolve the point sources inside that disc. Colour diagnostics isolate 928 red sources with strong infrared excess, about 36 percent of the high-quality three-band sample; they show rising spectral slopes from warm dust and sit tightly along the disc and its filaments. The authors argue these sources are dominated by embedded young stellar objects that mark star formation only a few hundred thousand to a million years old. Because the sources align with the merger-built disc and show no spatial correlation with the radio jet, the paper concludes that central star formation is regulated by the accreted gas reservoir rather than by jet–ISM interactions.

Core claim

A population of 928 red mid-infrared point sources with strong infrared excess is spatially confined to Cen A’s warped dust disc, exhibits rising mid-IR spectral slopes from warm dust, and is consistent with embedded young stellar objects tracing recent (~10^5–10^6 yr) star formation. Their geometric alignment with the disc and lack of correlation with the radio jet imply that star formation in the central regions is primarily regulated by merger-accreted gas, with no strong evidence for AGN jet–ISM interactions.

What carries the argument

Mid-infrared colour cuts (F560W–F770W > 1.4 and F560W–F1130W > 1.8) applied to high-quality three-band photometry, combined with the sources’ measured spatial confinement to the warped disc and rising spectral slopes, that separate the red dust-enshrouded population from ordinary photospheric sources.

Load-bearing premise

That the mid-infrared colours plus spatial confinement to the disc are enough to show the red sources are mostly embedded young stars rather than extreme dust-producing evolved stars or other contaminants.

What would settle it

Near-infrared imaging or mid-infrared spectroscopy of a substantial fraction of the 928 red sources that reclassifies most of them as extreme AGB or other evolved stars, or that reveals a clear overdensity of the red sources along the radio-jet axis rather than the disc.

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

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. The paper presents JWST/MIRI F560W, F770W and F1130W imaging of the central ~4 imes2 kpc of Centaurus A, producing a band-matched PSF catalogue of 58 445 sources (2 558 with σ≤0.1 mag in all three bands). Colour–magnitude and colour–colour diagrams show a clear bimodality; 928 sources selected by F560W–F770W>1.4 and F560W–F1130W>1.8 exhibit rising mid-IR slopes (median α=3.55) and are spatially confined to the warped dust disc (PCA first-component variance 94 %, perpendicular dispersion 0.38 kpc versus 0.63 kpc for the photospheric population). The authors interpret these sources as dominated by embedded Stage-I YSOs tracing recent (~10^5–10^6 yr) star formation regulated by merger-accreted gas, with no geometric correlation to the radio jet. The previously known Spitzer “oval dusty shell” is resolved into multiple F1130W-bright loops associated with the disc.

Significance. If the geometric result holds, the work cleanly separates merger-driven star formation in the central disc of the nearest radio galaxy from jet-triggered modes previously reported only in the outer halo. The public MIRI catalogue, the quantitative PCA/dispersion statistics, the multi-wavelength overlays with CO, radio and X-ray, and the resolution of the dusty shell into multiple loops are lasting observational contributions. The mid-IR colour selection and SED-slope analysis are carefully executed and provide a useful benchmark for future spectroscopic follow-up.

major comments (2)
  1. Section 4.1 (and colour cuts in §3.1.1): the claim that the 928 red sources are “dominated by embedded YSO candidates” rests on mid-IR colour analogy to Local Group regions, source counts exceeding the expected extreme-AGB fraction, and spatial confinement to the disc. The paper itself notes the colour overlap between Stage-I YSOs and extreme AGB stars and the absence of spectroscopic confirmation. While the geometric argument against a pure AGB population is persuasive, the language should be softened to “consistent with a population dominated by…” and residual AGB/RSG contamination should be quantified more explicitly (e.g., an upper limit scaled from LMC statistics or a simple luminosity-function comparison).
  2. Section 4.3: the conclusion of “no strong evidence for AGN jet–ISM interactions” on the scales probed is well supported by the lack of alignment with the radio/X-ray jet and by the thin-disc geometry. However, the paper also cites Espada et al. (2019) that star-formation efficiency is lower in the circumnuclear disc, possibly due to AGN-related shear/turbulence. A short quantitative statement of the surface-density contrast (or lack thereof) between jet-proximate and jet-distant regions of the disc would make the “no strong evidence” claim more falsifiable.
minor comments (5)
  1. Table 1 / §2.1: the two programmes have very different on-source times (1199 s vs 233 s). A brief note on how the depth variation is handled in the completeness limits (Fig. 4) and in the final high-quality sample would help the reader.
  2. Figure 9: the weak positive slope of the “main population” is attributed to residual diffuse/PAH background. A short test (e.g., aperture-size dependence or local-background residual map) would strengthen that interpretation.
  3. §3.3: the elevated 11.3/7.7 µm PAH ratio in the shells is cited from Quillen et al. (2008). Given that MIRI imaging alone cannot separate the two features, the statement should be clearly labelled as a literature result rather than a new measurement.
  4. Catalogue description (Table 4): magnitudes are stated to be uncorrected for extinction; a one-sentence reminder in the abstract or §3.1 would avoid misinterpretation by catalogue users.
  5. Typographical: “Observ ations” in the section heading; occasional missing spaces after commas in the abstract and introduction.

Circularity Check

0 steps flagged

No significant circularity: observational colour selection and geometric comparison to external disc/jet maps are independent of any fitted prediction or self-definitional loop.

full rationale

The paper is a straightforward JWST/MIRI imaging study. Source detection and PSF photometry (Section 2.3, starbugii parameters in Table 2) produce a catalogue; colour cuts F560W–F770W > 1.4 and F560W–F1130W > 1.8 are chosen at the observed density minimum separating bimodal populations in the CMD/CCD (Section 3.1.1, Figs 5–6), not derived from a model that already encodes the YSO claim. Spatial confinement is measured via PCA and perpendicular dispersions (Section 3.1.2) and compared to independently mapped CO, radio, and X-ray structures (Figs 10–11, citations to Espada et al. 2019, Hardcastle et al. 2003/2007). The interpretation that the 928 red sources are dominated by embedded YSOs rests on colour analogy to Local Group studies, source counts exceeding expected extreme-AGB fractions, and disc morphology; the paper itself flags the colour overlap and lack of spectroscopy (Section 4.1, 4.4). No parameter is fitted to a subset and then re-labelled a prediction, no uniqueness theorem is imported from the authors, and self-citations (Alonso Herrero et al. 2025, Pantoni et al. 2026, Evangelista et al. 2026) supply only ancillary MRS context for the nucleus, not the load-bearing disc-versus-jet geometry. The derivation chain is therefore self-contained against external multi-wavelength benchmarks.

Axiom & Free-Parameter Ledger

3 free parameters · 4 axioms · 0 invented entities

The central geometric claim rests on standard photometric practice, literature distance and extinction values, and an empirical colour cut. No new physical entities are introduced; the main free choices are the colour thresholds and the morphological sharpness/roundness filters used to reject extended sources.

free parameters (3)
  • F560W-F770W colour cut = >1.4 mag
    Threshold >1.4 mag chosen at the observed density minimum separating the two CMD populations (Section 3.1.1); directly controls the size of the red sample.
  • F560W-F1130W colour cut = >1.8 mag
    Threshold >1.8 mag likewise set by the colour-colour density minimum; jointly defines the 928-source sample.
  • Photometric uncertainty threshold = ≤0.1 mag
    ≤0.1 mag in all three bands for the high-quality sample of 2558 sources used in population analysis.
axioms (4)
  • domain assumption Distance to Cen A is 3.8 Mpc
    Adopted from Neumayer et al. (2007) and Harris (2010); converts angular scales to physical kpc used throughout.
  • domain assumption Mid-IR extinction is relatively flat (A_5.6 ~0.05 A_V, A_11.3 ~0.02 A_V)
    Used in Section 3.2 to argue that extinction alone cannot produce the observed steep spectral slopes of the red sources.
  • domain assumption Extreme AGB stars are rare (~4 percent of evolved stars in the LMC) and follow the smooth stellar mass distribution
    Invoked in Section 4.1 to argue that the large number and disc-confined geometry of red sources cannot be explained by evolved stars.
  • ad hoc to paper Colour loci of Stage-I YSOs and extreme AGB stars can be distinguished statistically by spatial distribution even if they overlap in colour space
    Core interpretive step of Section 4.1; not independently verified for Cen A.

pith-pipeline@v1.1.0-grok45 · 24252 in / 2647 out tokens · 19116 ms · 2026-07-11T11:08:07.282822+00:00 · methodology

0 comments
read the original abstract

Centaurus A (Cen A), the nearest active radio galaxy, hosts a warped dust disc formed in a gas-rich merger. We present JWST/MIRI imaging in three filters, F560W, F770W, and F1130W, of this central disc over a ~4 x 2 kpc region to characterise its resolved mid-infrared stellar populations. The images reveal a system of extended dusty structures, previously identified with Spitzer as an "oval dusty shell", now resolved into multiple loop-like features that are brightest in F1130W and closely associated with the warped disc. Colour-magnitude and colour-colour diagnostics reveal a distinct population of 928 red point sources with strong infrared excess, accounting for ~36 per cent of sources with high-quality photometry in all three bands, spatially confined to the disc. These sources exhibit rising mid-infrared spectral slopes indicative of emission from warm dust. Their colours and spatial distribution are consistent with a population dominated by embedded young stellar objects, tracing recent (~10^5-10^6 yr) star formation within the disc. The strong geometric alignment of these sources with the disc, together with the lack of correlation with the radio jet, suggests that star formation in the central regions of Cen A is primarily regulated by merger-accreted gas, with no strong evidence for AGN jet-ISM interactions.

Figures

Figures reproduced from arXiv: 2607.04942 by A. Alonso Herrero, A. Labiano, D. Dicken, D. Rouan, G. \"Ostlin, G. S. Wright, K. Justtanont, L. Colina, L. Evangelista, L. Hermosa Mu\~noz, L. Pantoni, M. Baes, M. Garc\'ia Mar\'in, M. G\"udel, M. L. Jones, M. Meixner, O. C. Jones, P. Guillard, P.-O. Lagage, P. van der Werf, T. B\"oker, Th. Henning, T. P. Ray, V. A. Buiten.

Figure 1
Figure 1. Figure 1: Colour composite image of Centaurus A: red corresponds to 5.8 𝜇m emission from Spitzer/IRAC (Quillen et al. 2006), green to X-ray emission from Chandra/ACIS (Hardcastle et al. 2007), and blue to the VLA radio jet (Hardcastle et al. 2003). The MIRI imaging mosaic (this work) is outlined in solid white, while the MICONIC MIRI/MRS footprint of the central 7 ′′ × 12′′ (see Alonso Herrero et al. 2025; Pantoni e… view at source ↗
Figure 2
Figure 2. Figure 2: Three-colour JWST/MIRI mosaic of the central region and inner disc of Centaurus A. The image combines F560W (blue), F770W (green), and F1130W (red), highlighting the prominent warped dust disc, filamentary structures, and the active nucleus. The nucleus appears as a bright compact source located between the prominent dust lanes of the warped disc. The mosaic covers approximately 6.9 arcmin2 . MNRAS 000, 1–… view at source ↗
Figure 3
Figure 3. Figure 3: Photometric uncertainty as a function of AB magnitude for sources detected in the MIRI F560W, F770W, and F1130W filters. The Cen A band￾matched catalogue includes sources with uncertainties up to 0.4 mag. The red horizontal line indicates the more stringent 0.1 mag uncertainty threshold used in this work. 10 1 10 2 10 3 (a) F560W 10 1 10 2 10 3 (b) F770W 26 24 22 20 18 16 14 Apparent magnitude 10 1 10 2 10… view at source ↗
Figure 4
Figure 4. Figure 4: Luminosity functions for sources detected in the MIRI F560W, F770W, and F1130W filters. The turnover at faint magnitudes, marked by the red vertical dashed lines, indicates the estimated photometric completeness limit. MNRAS 000, 1–14 (2026) [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: F560W versus F560W–F770W colour–magnitude diagram for Cen A point sources. Grey points show all 2,558 sources; red points indicate the 928 objects with an infrared excess. Representative uncertainties as a function of magnitude are indicated on the right. The separation is also apparent in the colour–colour plane (e.g., [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Colour–colour diagram of 𝐹560𝑊 − 𝐹770𝑊 versus 𝐹560𝑊 − 𝐹1130𝑊 for the Cen A point-source sample. The dashed lines mark the adopted colour cuts used to select the red dust-enshrouded population. Sym￾bols are colour-coded as in [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Spatial distribution of resolved sources in the central region of Cen A. Grey points show all sources detected in all three MIRI bands with photometric uncertainties < 0.1 mag, while red circles indicate the dust-enshrouded sources selected using the mid-infrared colour criteria. A 1 kpc scale bar is shown. disc both morphologically and spectrally. In particular, previous work (Quillen et al. 2008) has sho… view at source ↗
Figure 8
Figure 8. Figure 8: Positions of the red, dust-enshrouded sources from [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Median normalised mid-infrared SEDs of the colour-selected red sources (red) and the main point-source population (grey) in Cen A. Fluxes are normalised at F560W (5.6 𝜇m); shaded regions show the 16–84 per cent ranges. The red population exhibits a systematically steeper mid-infrared continuum consistent with emission dominated by warm dust. 4 DISCUSSION 4.1 Nature of the dust-enshrouded population The JWS… view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of the JWST/MIRI F1130W emission with tracers of cold molecular gas and radio continuum in Cen A. The JWST/MIRI F1130W image is overlaid with contours of CO(1–0) emission (cyan contours, from Espada et al. 2019, with a beam of 1"×1.5"), tracing the cold molecular gas, and VLA 21 cm radio continuum (blue contours) tracing large-scale radio emission (Hardcastle et al. 2003). The mid-infrared loop… view at source ↗
Figure 11
Figure 11. Figure 11: Comparison of the JWST/MIRI F1130W emission with radio and X-ray tracers of the AGN jet in Cen A. The F1130W image is overlaid with VLA 21 cm radio continuum (blue contours; Hardcastle et al. 2003) and Chandra X-ray emission (green contours; Hardcastle et al. 2007). The radio and X-ray emission trace the collimated AGN jet, which is oriented approximately perpendicular to the warped dust disc. The mid-inf… view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

93 extracted references · 40 canonical work pages · 3 internal anchors

  1. [1]

    T., et al., 2024, @doi [ ] 10.3847/1538-4357/ad57c0 , https://ui.adsabs.harvard.edu/abs/2024ApJ...972...47A 972, 47

    Aghdam S. T., et al., 2024, @doi [ ] 10.3847/1538-4357/ad57c0 , https://ui.adsabs.harvard.edu/abs/2024ApJ...972...47A 972, 47

    work page doi:10.3847/1538-4357/ad57c0 2024

  2. [2]

    Alonso Herrero A., et al., 2025, @doi [ ] 10.1051/0004-6361/202554823 , https://ui.adsabs.harvard.edu/abs/2025A&A...699A.334A 699, A334

    doi:10.1051/0004-6361/202554823 2025

  3. [3]

    Andr \'e P., Mattern M., Arzoumanian D., Shimajiri Y., Zavagno A., Abe D., Russeil D., 2025, @doi [ ] 10.3847/2041-8213/adc73d , https://ui.adsabs.harvard.edu/abs/2025ApJ...984L..59A 984, L59

    doi:10.3847/2041-8213/adc73d 2025

  4. [4]

    L., et al., 2012, @doi [ ] 10.1088/0004-637X/748/1/40 , https://ui.adsabs.harvard.edu/abs/2012ApJ...748...40B 748, 40

    Boyer M. L., et al., 2012, @doi [ ] 10.1088/0004-637X/748/1/40 , https://ui.adsabs.harvard.edu/abs/2012ApJ...748...40B 748, 40

    doi:10.1088/0004-637x/748/1/40 2012

  5. [5]

    Bradley L., et al., 2024, astropy/photutils: 2.0.2, @doi 10.5281/zenodo.13989456 , https://doi.org/10.5281/zenodo.13989456

    doi:10.5281/zenodo.13989456 2024

  6. [6]

    Bushouse H., et al., 2025, JWST Calibration Pipeline , @doi 10.5281/zenodo.6984365

    doi:10.5281/zenodo.6984365 2025

  7. [7]

    A., Burns J

    Clarke D. A., Burns J. O., Norman M. L., 1992, @doi [ ] 10.1086/171663 , https://ui.adsabs.harvard.edu/abs/1992ApJ...395..444C 395, 444

    work page doi:10.1086/171663 1992

  8. [8]

    Cresci G., et al., 2015, @doi [ ] 10.1088/0004-637X/799/1/82 , https://ui.adsabs.harvard.edu/abs/2015ApJ...799...82C 799, 82

    doi:10.1088/0004-637x/799/1/82 2015

  9. [9]

    M., et al., 2012, @doi [ ] 10.1111/j.1365-2966.2012.20418.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.421.1603C 421, 1603

    Crockett R. M., et al., 2012, @doi [ ] 10.1111/j.1365-2966.2012.20418.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.421.1603C 421, 1603

    doi:10.1111/j.1365-2966.2012.20418.x 2012

  10. [10]

    A., et al., 2026, @doi [ ] 10.3847/1538-4357/ae5f66 , https://ui.adsabs.harvard.edu/abs/2026ApJ..1002..217C 1002, 217

    Cronin S. A., et al., 2026, @doi [ ] 10.3847/1538-4357/ae5f66 , https://ui.adsabs.harvard.edu/abs/2026ApJ..1002..217C 1002, 217

    work page doi:10.3847/1538-4357/ae5f66 2026

  11. [11]

    H., et al., 2009, @doi [ ] 10.1111/j.1365-2966.2009.14715.x , https://ui.adsabs.harvard.edu/abs/2009MNRAS.395.1999C 395, 1999

    Croston J. H., et al., 2009, @doi [ ] 10.1111/j.1365-2966.2009.14715.x , https://ui.adsabs.harvard.edu/abs/2009MNRAS.395.1999C 395, 1999

    doi:10.1111/j.1365-2966.2009.14715.x 2009

  12. [12]

    Uniqueness in Harper's vertex-isoperimetric theorem

    Crowther P. A., 2007, @doi [ ] 10.1146/annurev.astro.45.051806.110615 , https://ui.adsabs.harvard.edu/abs/2007ARA&A..45..177C 45, 177

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev.astro.45.051806.110615 2007

  13. [13]

    Dicken D., et al., 2024, @doi [ ] 10.1051/0004-6361/202449451 , https://ui.adsabs.harvard.edu/abs/2024A&A...689A...5D 689, A5

    doi:10.1051/0004-6361/202449451 2024

  14. [14]

    J., van den Bergh S., Harvel C

    Dufour R. J., van den Bergh S., Harvel C. A., Martins D. H., Schiffer III F. H., Talbot Jr. R. J., Talent D. L., Wells D. C., 1979, @doi [ ] 10.1086/112421 , https://ui.adsabs.harvard.edu/abs/1979AJ.....84..284D 84, 284

    work page doi:10.1086/112421 1979

  15. [15]

    Espada D., et al., 2009, @doi [ ] 10.1088/0004-637X/695/1/116 , https://ui.adsabs.harvard.edu/abs/2009ApJ...695..116E 695, 116

    doi:10.1088/0004-637x/695/1/116 2009

  16. [16]

    Espada D., et al., 2017, @doi [ ] 10.3847/1538-4357/aa78a9 , https://ui.adsabs.harvard.edu/abs/2017ApJ...843..136E 843, 136

    doi:10.3847/1538-4357/aa78a9 2017

  17. [17]

    Espada D., et al., 2019, @doi [ ] 10.3847/1538-4357/ab262d , https://ui.adsabs.harvard.edu/abs/2019ApJ...887...88E 887, 88

    doi:10.3847/1538-4357/ab262d 2019

  18. [18]

    MICONIC: The multiphase circumnuclear region of Centaurus A as seen with JWST/MIRI MRS observations. I. Spectral inventory and properties of the warm molecular disk

    Evangelista L., et al., 2026, @doi [arXiv e-prints] 10.48550/arXiv.2605.22497 , https://ui.adsabs.harvard.edu/abs/2026arXiv260522497E p. arXiv:2605.22497

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2605.22497 2026

  19. [19]

    Garc \' a-Bernete I., et al., 2024, @doi [ ] 10.1051/0004-6361/202450086 , https://ui.adsabs.harvard.edu/abs/2024A&A...691A.162G 691, A162

    doi:10.1051/0004-6361/202450086 2024

  20. [20]

    P., et al., 2023, @doi [ ] 10.1088/1538-3873/acd1b5 , https://ui.adsabs.harvard.edu/abs/2023PASP..135f8001G 135, 068001

    Gardner J. P., et al., 2023, @doi [ ] 10.1088/1538-3873/acd1b5 , https://ui.adsabs.harvard.edu/abs/2023PASP..135f8001G 135, 068001

    doi:10.1088/1538-3873/acd1b5 2023

  21. [21]

    A., 1979, @doi [ ] 10.1086/157265 , https://ui.adsabs.harvard.edu/abs/1979ApJ...232...60G 232, 60

    Graham J. A., 1979, @doi [ ] 10.1086/157265 , https://ui.adsabs.harvard.edu/abs/1979ApJ...232...60G 232, 60

    work page doi:10.1086/157265 1979

  22. [22]

    Habel N., et al., 2024, @doi [ ] 10.3847/1538-4357/ad5343 , https://ui.adsabs.harvard.edu/abs/2024ApJ...971..108H 971, 108

    doi:10.3847/1538-4357/ad5343 2024

  23. [23]

    J., Olofsson H., eds, 2003, Asymptotic giant branch stars

    Habing H. J., Olofsson H., eds, 2003, Asymptotic giant branch stars

    2003

  24. [24]

    J., Worrall D

    Hardcastle M. J., Worrall D. M., Kraft R. P., Forman W. R., Jones C., Murray S. S., 2003, @doi [ ] 10.1086/376519 , https://ui.adsabs.harvard.edu/abs/2003ApJ...593..169H 593, 169

    doi:10.1086/376519 2003

  25. [25]

    J., et al., 2007, @doi [ ] 10.1086/524197 , https://ui.adsabs.harvard.edu/abs/2007ApJ...670L..81H 670, L81

    Hardcastle M. J., et al., 2007, @doi [ ] 10.1086/524197 , https://ui.adsabs.harvard.edu/abs/2007ApJ...670L..81H 670, L81

    doi:10.1086/524197 2007

  26. [26]

    Harris G. L. H., 2010, @doi [ ] 10.1071/AS09063 , https://ui.adsabs.harvard.edu/abs/2010PASA...27..475H 27, 475

    work page doi:10.1071/as09063 2010

  27. [27]

    E., Harris G

    Harris W. E., Harris G. L. H., 2002, @doi [ ] 10.1086/340466 , https://ui.adsabs.harvard.edu/abs/2002AJ....123.3108H 123, 3108

    work page doi:10.1086/340466 2002

  28. [28]

    Hermosa Mu \ n oz L., et al., 2024, @doi [ ] 10.1051/0004-6361/202450262 , https://ui.adsabs.harvard.edu/abs/2024A&A...690A.350H 690, A350

    doi:10.1051/0004-6361/202450262 2024

  29. [29]

    W., Kennicutt Jr

    Hodge P. W., Kennicutt Jr. R. C., 1983, @doi [ ] 10.1086/113318 , https://ui.adsabs.harvard.edu/abs/1983AJ.....88..296H 88, 296

    work page doi:10.1086/113318 1983

  30. [30]

    P., 1998, @doi [ ] 10.1007/s001590050011 , https://ui.adsabs.harvard.edu/abs/1998A&ARv...8..237I 8, 237

    Israel F. P., 1998, @doi [ ] 10.1007/s001590050011 , https://ui.adsabs.harvard.edu/abs/1998A&ARv...8..237I 8, 237

    doi:10.1007/s001590050011 1998

  31. [31]

    C., Meixner M., Sargent B

    Jones O. C., Meixner M., Sargent B. A., Boyer M. L., Sewi o M., Hony S., Roman-Duval J., 2015, @doi [ ] 10.1088/0004-637X/811/2/145 , https://ui.adsabs.harvard.edu/abs/2015ApJ...811..145J 811, 145

    work page doi:10.1088/0004-637x/811/2/145 2015

  32. [32]

    C., et al., 2017a, @doi [ ] 10.1093/mnras/stx1101 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.3250J 470, 3250

    Jones O. C., et al., 2017a, @doi [ ] 10.1093/mnras/stx1101 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.3250J 470, 3250

    work page doi:10.1093/mnras/stx1101

  33. [33]

    C., Meixner M., Justtanont K., Glasse A., 2017b, @doi [ ] 10.3847/1538-4357/aa6bf6 , https://ui.adsabs.harvard.edu/abs/2017ApJ...841...15J 841, 15

    Jones O. C., Meixner M., Justtanont K., Glasse A., 2017b, @doi [ ] 10.3847/1538-4357/aa6bf6 , https://ui.adsabs.harvard.edu/abs/2017ApJ...841...15J 841, 15

    doi:10.3847/1538-4357/aa6bf6

  34. [34]

    C., et al., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-01945-7 , https://ui.adsabs.harvard.edu/abs/2023NatAs...7..694J 7, 694

    Jones O. C., et al., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-01945-7 , https://ui.adsabs.harvard.edu/abs/2023NatAs...7..694J 7, 694

    work page doi:10.1038/s41550-023-01945-7 2023

  35. [35]

    S., Paul K

    Joseph P., Sreekumar P., Stalin C. S., Paul K. T., Mondal C., George K., Mathew B., 2022, @doi [ ] 10.1093/mnras/stac2388 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.2300J 516, 2300

    doi:10.1093/mnras/stac2388 2022

  36. [36]

    T., et al., 2009, @doi [ ] 10.1051/0004-6361/200912624 , https://ui.adsabs.harvard.edu/abs/2009A&A...502L...5K 502, L5

    Kainulainen J. T., et al., 2009, @doi [ ] 10.1051/0004-6361/200912624 , https://ui.adsabs.harvard.edu/abs/2009A&A...502L...5K 502, L5

    work page doi:10.1051/0004-6361/200912624 2009

  37. [37]

    C., Banfield J

    Keel W. C., Banfield J. K., Medling A. M., Neff S. G., 2019, @doi [ ] 10.3847/1538-3881/aaf809 , https://ui.adsabs.harvard.edu/abs/2019AJ....157...66K 157, 66

    work page doi:10.3847/1538-3881/aaf809 2019

  38. [38]

    L., Hawarden T

    Leeuw L. L., Hawarden T. G., Matthews H. E., Robson E. I., Eckart A., 2002, @doi [ ] 10.1086/324494 , https://ui.adsabs.harvard.edu/abs/2002ApJ...565..131L 565, 131

    work page doi:10.1086/324494 2002

  39. [39]

    Lenki \'c L., et al., 2024, @doi [ ] 10.3847/1538-4357/ad3f90 , https://ui.adsabs.harvard.edu/abs/2024ApJ...967..110L 967, 110

    doi:10.3847/1538-4357/ad3f90 2024

  40. [40]

    K., et al., 2023, @doi [ ] 10.3847/2041-8213/acaf85 , https://ui.adsabs.harvard.edu/abs/2023ApJ...944L...9L 944, L9

    Leroy A. K., et al., 2023, @doi [ ] 10.3847/2041-8213/acaf85 , https://ui.adsabs.harvard.edu/abs/2023ApJ...944L...9L 944, L9

    doi:10.3847/2041-8213/acaf85 2023

  41. [41]

    J., Koekemoer A., Capetti A., Axon D., Macchetto D., Caon N., 2000, @doi [ ] 10.1086/308168 , https://ui.adsabs.harvard.edu/abs/2000ApJ...528..276M 528, 276

    Marconi A., Schreier E. J., Koekemoer A., Capetti A., Axon D., Macchetto D., Caon N., 2000, @doi [ ] 10.1086/308168 , https://ui.adsabs.harvard.edu/abs/2000ApJ...528..276M 528, 276

    work page doi:10.1086/308168 2000

  42. [42]

    G., Kennicutt Jr

    Minniti D., Rejkuba M., Funes J. G., Kennicutt Jr. R. C., 2004, @doi [ ] 10.1086/422546 , https://ui.adsabs.harvard.edu/abs/2004ApJ...612..215M 612, 215

    work page doi:10.1086/422546 2004

  43. [43]

    A barred spiral at the centre of the giant elliptical radio galaxy Centaurus A

    Mirabel I. F., et al., 1999, @doi [ ] 10.48550/arXiv.astro-ph/9810419 , https://ui.adsabs.harvard.edu/abs/1999A&A...341..667M 341, 667

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9810419 1999

  44. [44]

    R., et al., 2000, @doi [ ] 10.1086/308927 , https://ui.adsabs.harvard.edu/abs/2000ApJ...536..266M 536, 266

    Mould J. R., et al., 2000, @doi [ ] 10.1086/308927 , https://ui.adsabs.harvard.edu/abs/2000ApJ...536..266M 536, 266

    work page doi:10.1086/308927 2000

  45. [45]

    V., Sutherland R., Wagner A., 2016, @doi [ ] 10.1093/mnras/stw1368 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461..967M 461, 967

    Mukherjee D., Bicknell G. V., Sutherland R., Wagner A., 2016, @doi [ ] 10.1093/mnras/stw1368 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461..967M 461, 967

    doi:10.1093/mnras/stw1368 2016

  46. [46]

    V., Wagner A

    Mukherjee D., Bicknell G. V., Wagner A. Y., Sutherland R. S., Silk J., 2018, @doi [ ] 10.1093/mnras/sty1776 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.479.5544M 479, 5544

    doi:10.1093/mnras/sty1776 2018

  47. [47]

    Nally C., 2023, StarbugII: JWST PSF photometry for crowded fields , Astrophysics Source Code Library, record ascl:2309.012 ( @eprint ascl 2309.012 )

    2023

  48. [48]

    Nally C., et al., 2024, @doi [ ] 10.1093/mnras/stae1163 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.531..183N 531, 183

    doi:10.1093/mnras/stae1163 2024

  49. [49]

    Nayak O., et al., 2024, @doi [ ] 10.3847/1538-4357/ad7baf , https://ui.adsabs.harvard.edu/abs/2024ApJ...975..262N 975, 262

    work page doi:10.3847/1538-4357/ad7baf 2024

  50. [50]

    G., Eilek J

    Neff S. G., Eilek J. A., Owen F. N., 2015, @doi [ ] 10.1088/0004-637X/802/2/87 , https://ui.adsabs.harvard.edu/abs/2015ApJ...802...87N 802, 87

    work page doi:10.1088/0004-637x/802/2/87 2015

  51. [51]

    Nesvadba N. P. H., et al., 2010, @doi [ ] 10.1051/0004-6361/200913333 , https://ui.adsabs.harvard.edu/abs/2010A&A...521A..65N 521, A65

    doi:10.1051/0004-6361/200913333 2010

  52. [52]

    P., de Zeeuw P

    Neumayer N., Cappellari M., Reunanen J., Rix H.-W., van der Werf P. P., de Zeeuw P. T., Davies R. I., 2007, @doi [ ] 10.1086/523039 , https://ui.adsabs.harvard.edu/abs/2007ApJ...671.1329N 671, 1329

    doi:10.1086/523039 2007

  53. [53]

    A., Morganti R., 2005, @doi [ ] 10.1051/0004-6361:20041379 , https://ui.adsabs.harvard.edu/abs/2005A&A...429..469O 429, 469

    Oosterloo T. A., Morganti R., 2005, @doi [ ] 10.1051/0004-6361:20041379 , https://ui.adsabs.harvard.edu/abs/2005A&A...429..469O 429, 469

    doi:10.1051/0004-6361:20041379 2005

  54. [54]

    Pantoni L., et al., 2026, @doi [ ] 10.1051/0004-6361/202558839 , https://ui.adsabs.harvard.edu/abs/2026A&A...709A.237P 709, A237

    work page doi:10.1051/0004-6361/202558839 2026

  55. [55]

    W., Ford H

    Peng E. W., Ford H. C., Freeman K. C., White R. L., 2002, @doi [ ] 10.1086/344308 , https://ui.adsabs.harvard.edu/abs/2002AJ....124.3144P 124, 3144

    work page doi:10.1086/344308 2002

  56. [56]

    W., Ford H

    Peng E. W., Ford H. C., Freeman K. C., 2004, @doi [ ] 10.1086/381236 , https://ui.adsabs.harvard.edu/abs/2004ApJ...602..705P 602, 705

    work page doi:10.1086/381236 2004

  57. [57]

    Perna M., et al., 2020, @doi [ ] 10.1051/0004-6361/202038328 , https://ui.adsabs.harvard.edu/abs/2020A&A...643A.139P 643, A139

    doi:10.1051/0004-6361/202038328 2020

  58. [58]

    C., de Zeeuw P

    Quillen A. C., de Zeeuw P. T., Phinney E. S., Phillips T. G., 1992, @doi [ ] 10.1086/171329 , https://ui.adsabs.harvard.edu/abs/1992ApJ...391..121Q 391, 121

    work page doi:10.1086/171329 1992

  59. [59]

    C., Graham J

    Quillen A. C., Graham J. R., Frogel J. A., 1993, @doi [ ] 10.1086/172943 , https://ui.adsabs.harvard.edu/abs/1993ApJ...412..550Q 412, 550

    work page doi:10.1086/172943 1993

  60. [60]

    C., Brookes M

    Quillen A. C., Brookes M. H., Keene J., Stern D., Lawrence C. R., Werner M. W., 2006, @doi [ ] 10.1086/504418 , https://ui.adsabs.harvard.edu/abs/2006ApJ...645.1092Q 645, 1092

    doi:10.1086/504418 2006

  61. [61]

    C., et al., 2008, @doi [ ] 10.1111/j.1365-2966.2007.12768.x , https://ui.adsabs.harvard.edu/abs/2008MNRAS.384.1469Q 384, 1469

    Quillen A. C., et al., 2008, @doi [ ] 10.1111/j.1365-2966.2007.12768.x , https://ui.adsabs.harvard.edu/abs/2008MNRAS.384.1469Q 384, 1469

    doi:10.1111/j.1365-2966.2007.12768.x 2008

  62. [62]

    C., Neumayer N., Oosterloo T., Espada D., 2010, @doi [ ] 10.1071/AS09069 , https://ui.adsabs.harvard.edu/abs/2010PASA...27..396Q 27, 396

    Quillen A. C., Neumayer N., Oosterloo T., Espada D., 2010, @doi [ ] 10.1071/AS09069 , https://ui.adsabs.harvard.edu/abs/2010PASA...27..396Q 27, 396

    doi:10.1071/as09069 2010

  63. [63]

    A., Smith N., Haworth T

    Reiter M., Morse J. A., Smith N., Haworth T. J., Kuhn M. A., Klaassen P. D., 2022, @doi [ ] 10.1093/mnras/stac2820 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.5382R 517, 5382

    doi:10.1093/mnras/stac2820 2022

  64. [64]

    R., Bedding T

    Rejkuba M., Minniti D., Silva D. R., Bedding T. R., 2001, @doi [ ] 10.1051/0004-6361:20011315 , https://ui.adsabs.harvard.edu/abs/2001A&A...379..781R 379, 781

    doi:10.1051/0004-6361:20011315 2001

  65. [65]

    R., Bedding T

    Rejkuba M., Minniti D., Silva D. R., Bedding T. R., 2003, @doi [ ] 10.1051/0004-6361:20034056 , https://ui.adsabs.harvard.edu/abs/2003A&A...411..351R 411, 351

    doi:10.1051/0004-6361:20034056 2003

  66. [66]

    E., Harris G

    Rejkuba M., Greggio L., Harris W. E., Harris G. L. H., Peng E. W., 2005, @doi [ ] 10.1086/432462 , https://ui.adsabs.harvard.edu/abs/2005ApJ...631..262R 631, 262

    doi:10.1086/432462 2005

  67. [67]

    E., Greggio L., Crnojevi \'c D., Harris G

    Rejkuba M., Harris W. E., Greggio L., Crnojevi \'c D., Harris G. L. H., 2022, @doi [ ] 10.1051/0004-6361/202141347 , https://ui.adsabs.harvard.edu/abs/2022A&A...657A..41R 657, A41

    work page doi:10.1051/0004-6361/202141347 2022

  68. [68]

    Riebel D., Srinivasan S., Sargent B., Meixner M., 2012, @doi [ ] 10.1088/0004-637X/753/1/71 , https://ui.adsabs.harvard.edu/abs/2012ApJ...753...71R 753, 71

    work page doi:10.1088/0004-637x/753/1/71 2012

  69. [69]

    H., et al., 2015, @doi [ ] 10.1086/682252 , https://ui.adsabs.harvard.edu/abs/2015PASP..127..584R 127, 584

    Rieke G. H., et al., 2015, @doi [ ] 10.1086/682252 , https://ui.adsabs.harvard.edu/abs/2015PASP..127..584R 127, 584

    doi:10.1086/682252 2015

  70. [70]

    Rigby J., et al., 2023, @doi [ ] 10.1088/1538-3873/acb293 , https://ui.adsabs.harvard.edu/abs/2023PASP..135d8001R 135, 048001

    doi:10.1088/1538-3873/acb293 2023

  71. [71]

    Rigopoulou D., et al., 2024, @doi [ ] 10.1093/mnras/stae1535 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.532.1598R 532, 1598

    doi:10.1093/mnras/stae1535 2024

  72. [72]

    P., Whitney B

    Robitaille T. P., Whitney B. A., Indebetouw R., Wood K., Denzmore P., 2006, @doi [ ] 10.1086/508424 , https://ui.adsabs.harvard.edu/abs/2006ApJS..167..256R 167, 256

    doi:10.1086/508424 2006

  73. [73]

    Salom \'e Q., Salom \'e P., Miville-Desch \^e nes M.-A., Combes F., Hamer S., 2017, @doi [ ] 10.1051/0004-6361/201731429 , https://ui.adsabs.harvard.edu/abs/2017A&A...608A..98S 608, A98

    doi:10.1051/0004-6361/201731429 2017

  74. [74]

    Santoro F., Oonk J. B. R., Morganti R., Oosterloo T., 2015, @doi [ ] 10.1051/0004-6361/201425103 , https://ui.adsabs.harvard.edu/abs/2015A&A...574A..89S 574, A89

    work page doi:10.1051/0004-6361/201425103 2015

  75. [75]

    H., van der Hulst J

    Schiminovich D., van Gorkom J. H., van der Hulst J. M., Kasow S., 1994, @doi [ ] 10.1086/187246 , https://ui.adsabs.harvard.edu/abs/1994ApJ...423L.101S 423, L101

    doi:10.1086/187246 1994

  76. [76]

    J., Capetti A., Macchetto F., Sparks W

    Schreier E. J., Capetti A., Macchetto F., Sparks W. B., Ford H. J., 1996, @doi [ ] 10.1086/176917 , https://ui.adsabs.harvard.edu/abs/1996ApJ...459..535S 459, 535

    work page doi:10.1086/176917 1996

  77. [77]

    P., et al., 2014, @doi [ ] 10.1088/0004-6256/148/6/124 , https://ui.adsabs.harvard.edu/abs/2014AJ....148..124S 148, 124

    Seale J. P., et al., 2014, @doi [ ] 10.1088/0004-6256/148/6/124 , https://ui.adsabs.harvard.edu/abs/2014AJ....148..124S 148, 124

    doi:10.1088/0004-6256/148/6/124 2014

  78. [78]

    Shin J., Woo J.-H., Chung A., Baek J., Cho K., Kang D., Bae H.-J., 2019, @doi [ ] 10.3847/1538-4357/ab2e72 , https://ui.adsabs.harvard.edu/abs/2019ApJ...881..147S 881, 147

    doi:10.3847/1538-4357/ab2e72 2019

  79. [79]

    C., et al., 2007, @doi [ ] 10.1086/519236 , https://ui.adsabs.harvard.edu/abs/2007ApJ...664.1144S 664, 1144

    Sloan G. C., et al., 2007, @doi [ ] 10.1086/519236 , https://ui.adsabs.harvard.edu/abs/2007ApJ...664.1144S 664, 1144

    work page doi:10.1086/519236 2007

  80. [80]

    Soria R., et al., 1996, @doi [ ] 10.1086/177403 , https://ui.adsabs.harvard.edu/abs/1996ApJ...465...79S 465, 79

    work page doi:10.1086/177403 1996

Showing first 80 references.