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Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra-I cluster. VI. A star-forming UDG in Hydra I: a rare UDG or a transition phase?

T0 review · 1 major / 0 minor · reviewed 2026-06-29 · grok-4.3

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

Pith's one-line read UDG 6 in Hydra I likely formed as a puffed-up dwarf stretched by cluster tides that also triggered its star formation.

desk verdict Solid new MUSE kinematics and morphology for one gas-rich UDG, but the puffed-up dwarf interpretation stays qualitative. read the letter →

arxiv 2605.27109 v1 pith:ZZXVJT4J submitted 2026-05-26 astro-ph.GA

Luca Rossi , Chiara Buttitta , Goran Doll , Enrichetta Iodice , Marco Gullieuszik , Marc Sarzi , Marco Mirabile , Johanna Hartke
show 16 more authors
Magda Arnaboldi Rosa Calvi Michele Cantiello Enrico Maria Corsini Giuseppe D'Ago Jesús Falcón-Barroso Francesca Fonzo Duncan A. Forbes Michael Hilker Antonio La Marca Alessandro Loni Steffen Mieske Maurizio Paolillo Marina Rejkuba Marilena Spavone Chiara Spiniello
This is my paper
classification astro-ph.GA
keywords ultra-diffusegalaxiesHydraIclusterstar-formingUDGMUSEspectroscopytidalfeaturespuffed-updwarfgalaxyformation
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

The paper analyzes UDG 6, the only gas-rich star-forming ultra-diffuse galaxy in the LEWIS MUSE sample of the Hydra I cluster. Integral-field spectroscopy reveals its regular elongated shape, coherent gas rotation, clumpy recent star formation, dust content, metal-poor ionised gas, old-to-intermediate stars, and an arc-like tidal feature. These traits are interpreted as evidence that the galaxy began as a more compact dwarf whose stellar body was stretched outward, with cluster environmental effects and a possible tidal encounter driving the current activity while leaving rotation intact. A reader would care because the case supplies an observed pathway by which ordinary dwarfs can become ultra-diffuse objects inside clusters.

What carries the argument

MUSE-derived combination of regular elongated shape, coherent gas rotation, clumpy star formation, and arc-like tidal feature matched to the puffed-up dwarf formation channel.

What would settle it

A quantitative comparison or simulation showing that UDG 6’s properties match a failed-galaxy or high-spin-halo model better than the puffed-up dwarf channel would disprove the paper’s interpretation.

Watch

Extended reading notes

Core claim

UDG 6 is confirmed as a Hydra I member whose MUSE data show a regular elongated morphology, significant dust, metal-poor ionised gas, and an underlying old-to-intermediate stellar population. Emission-line analysis indicates local clumpy star-forming activity, while unsharp masking uncovers an arc-like tidal feature. The authors conclude that UDG 6 originated from a puffed-up dwarf whose stellar content was stretched to larger radii and is passively evolving into a more diffuse galaxy; its location in a dynamically active cluster region and possible tidal interaction with a neighbour are suggested to have shaped its properties and triggered the recent star formation without destroying the co

Load-bearing premise

The observed shape, rotation, star-formation clumps, and tidal arc uniquely identify the puffed-up dwarf channel and exclude other formation routes such as failed-galaxy or high-spin-halo origins.

Editorial extensions

If this is right

  • Tidal interactions inside dynamically active cluster regions can stretch dwarf galaxies into ultra-diffuse objects while preserving coherent gas rotation.
  • Recent star formation in UDGs can be triggered by gentle tidal encounters rather than requiring exotic initial conditions.
  • An arc-like tidal feature together with clumpy star formation marks a possible transition phase between compact dwarfs and fully passive UDGs.
  • Multi-band globular-cluster analysis combined with gas kinematics can further test the stellar-mass assembly history of such objects.

Reading between the lines

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

  • If similar tidal features and preserved rotation appear in other star-forming UDGs, the puffed-up dwarf channel may be more common than the failed-galaxy route inside clusters.
  • Targeted simulations of UDG 6 could quantify how unique the observed feature combination is to the puffed-up dwarf scenario.
  • Extending the same MUSE analysis to the rest of the LEWIS sample could reveal whether UDG 6 is an outlier or part of a continuous environmental sequence.
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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

1 major / 0 minor

Summary. The paper presents MUSE integral-field spectroscopy of UDG 6, a gas-rich star-forming ultra-diffuse galaxy in the Hydra I cluster. It derives the galaxy's elongated morphology, coherent gas rotation, clumpy star formation, metal-poor ionized gas, underlying old-to-intermediate stellar population, dust content, and an arc-like tidal feature via spectral fitting, Voronoi binning, and unsharp masking. Based on qualitative comparison to formation scenarios, it concludes that UDG 6 likely originated as a 'puffed-up dwarf' stretched by environmental processes, with a possible tidal interaction triggering recent star formation while preserving gas rotation.

Significance. If the formation interpretation holds, the work supplies a detailed observational case of a star-forming UDG in a dynamically active cluster environment, illustrating how tidal features and stripping may contribute to UDG properties. The application of standard MUSE reduction, Voronoi tessellation, and multi-band GC analysis provides concrete data on kinematics and stellar populations that can be compared to other UDGs.

major comments (1)
  1. [Abstract / Discussion] Abstract and Discussion (formation scenario paragraph): The central claim that the regular elongated shape, coherent gas rotation, clumpy star formation, and arc-like tidal feature uniquely identify the puffed-up dwarf channel (and rule out failed-galaxy or high-spin-halo alternatives) rests on qualitative feature matching without quantitative model comparison, mock observations, or simulation matching. This assumption is load-bearing for the formation-history conclusion.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their detailed and constructive report. We address the single major comment below and have revised the manuscript to strengthen the presentation of our formation-scenario discussion while preserving the observational results.

read point-by-point responses

  1. Referee: [Abstract / Discussion] Abstract and Discussion (formation scenario paragraph): The central claim that the regular elongated shape, coherent gas rotation, clumpy star formation, and arc-like tidal feature uniquely identify the puffed-up dwarf channel (and rule out failed-galaxy or high-spin-halo alternatives) rests on qualitative feature matching without quantitative model comparison, mock observations, or simulation matching. This assumption is load-bearing for the formation-history conclusion.

    Authors: We agree that the formation interpretation rests on qualitative comparison of observed morphological, kinematic, and star-formation features to the expectations of the main UDG formation channels. The manuscript does not claim that these features 'uniquely identify' the puffed-up dwarf scenario or definitively rule out the alternatives; the language in both the abstract and discussion uses 'might originate' and 'we suggest'. Nevertheless, we acknowledge that a more explicit statement of the qualitative nature of the comparison, together with a brief note on the current absence of tailored simulations or mock MUSE observations for this specific object, would improve clarity. We have therefore revised the relevant paragraphs in the abstract and Section 5 to (i) emphasize that the features are consistent with the puffed-up dwarf channel under cluster tidal influence, (ii) state that other channels cannot be excluded on the basis of the present data alone, and (iii) identify quantitative model comparison as desirable future work. These changes do not alter the observational results or the overall narrative but make the evidential basis of the interpretation more transparent. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: observational description and qualitative hypothesis

full rationale

The paper reports MUSE-derived morphology, kinematics, emission-line properties, and an arc-like feature for UDG 6, then offers a qualitative suggestion that these match a puffed-up dwarf scenario influenced by the cluster environment. No equations, fitted parameters, or predictions are defined in terms of one another; the formation-channel interpretation is presented as a hypothesis without any reduction to self-referential inputs or load-bearing self-citations. The derivation chain is therefore self-contained against external benchmarks.

Assumptions & free parameters 0 free parameters · 2 assumptions · 0 invented entities

The work rests on standard assumptions of cluster membership via redshift, standard stellar population synthesis models for age and metallicity, and the applicability of existing UDG formation scenarios to interpret one object; no new free parameters or invented entities are introduced.

assumptions (2)
  • domain assumption Hydra I cluster distance and velocity dispersion are taken from prior literature to confirm membership.
    Membership confirmation is stated without re-derivation in the abstract.
  • standard math Emission-line ratios and equivalent widths reliably indicate recent star formation and metal-poor gas.
    Standard nebular diagnostics assumed without new calibration.

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Cite this review

Pith. "Pith review of Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra-I cluster. VI. A star-forming UDG in Hydra I: a rare UDG or a transition phase?." pith.science (2026). https://pith.science/paper/ZZXVJT4J

@misc{pith2026260527109,
  author       = {Pith},
  title        = {Pith review of: Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra-I cluster. VI. A star-forming UDG in Hydra I: a rare UDG or a transition phase?},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZZXVJT4J}},
  note         = {Machine review of arXiv:2605.27109}
}
read the original abstract

This paper presents a detailed analysis of a gas-rich star-forming ultra-diffuse galaxy (UDG) as part of the ESO Large Programme 'Looking into the faintEst WIth MUSE (LEWIS)'. Among the UDGs in the LEWIS sample, UDG 6 is the only galaxy that hosts a significant amount of ionised gas with evidence of emission lines, suggesting recent star-forming activity. The main goal of this work is to constrain the formation history of this UDG by comparing its properties with the main formation scenarios proposed for this extreme class of galaxies. We adopted integral field spectroscopy from MUSE to derive the morphology and the structural properties of the stellar and gas components of UDG 6. We applied spectral fitting and Voronoi tessellation algorithms to the MUSE data-cube to derive the kinematics and properties of the gas and stellar component. Moreover, we derived the GCs populations' properties by applying a multi-band spectrophotometric analysis. We confirmed that UDG 6 is a member of Hydra I cluster. It is characterised by a regular and elongated shape and contains a significant dust content, a metal-poor ionised gas fraction and an underlying old-to-intermediate stellar component. Evidence of local and clumpy star-forming activity has been revealed through the analysis of emission line, and an arc-like tidal feature was discovered from unsharp masking analysis. UDG 6 might originate from a 'puffed-up dwarf' whose stellar content has been stretched out to larger radii, passively evolving into a more diffuse galaxy. Being located in a dynamically active region of the cluster, characterised by tidal features and stripping phenomena, we suggest that the environmental processes have played a role in shaping the properties of UDG 6. A tidal interaction with a nearby galaxy might have triggered recent star-formation activity, without dramatically altering the coherent gas rotation in UDG 6.

Figures

Figures reproduced from arXiv: 2605.27109 by the authors.

Figure 1
Figure 1. OmegaCAM@VST r-band image of the North group of the Hydra I cluster, adapted from ESO/INAF/M. Spavone, E. Iodice. Left panel: The field-of-view is 10 × 5 arcmin2 . Right panel: Zoom-in g − r colour-composite image of UDG 6. The field-of-view is 1.6 × 1.6 arcmin2 Data of UDG 6 were acquired on three different observation blocks (OB): 23 − 24 April 2023, 18 − 19 December 2023, and 12 − 13 January 2024. Within each OB,… view at source ↗
Figure 2
Figure 2. Isophotal analysis of UDG 6. Top panels: MUSE reconstructed white image of UDG 6 with contours (left), bi-dimensional [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Unsharp mask of UDG 6. Total white image (4800 [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: Stacked spectrum of UDG 6 with its best-fit. Top row: the stacked spectrum is shown as a black line, and the best-fit obtained [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: Stellar population analysis of 1D stacked spectrum of UDG 6. Each panel shows the distributions of the stellar population [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]
Figure 6
Figure 6. Figure 6: Emission lines analysis of UDG 6. Left panel: the MUSE reconstructed image (grey) superimposed with contours of H [PITH_FULL_IMAGE:figures/full_fig_p008_6.png]
Figure 7
Figure 7. Figure 7: BPT diagram (Baldwin et al. 1981). The red circle is the value for UDG 6 obtained from 1Reff stacked spectrum, while the black circles mark the values obtained from the four apertures. The green and red lines separate the regions of the AGN galaxy, the LINER objects, a…
Figure 8
Figure 8. Figure 8: Spatially-resolved gas kinematics of UDG 6. Left panel: Voronoi-binned map of the S [PITH_FULL_IMAGE:figures/full_fig_p009_8.png]
Figure 9
Figure 9. Figure 9: Projected phase-space diagram for galaxies in Hydra I. [PITH_FULL_IMAGE:figures/full_fig_p010_9.png]
Figure 10
Figure 10. Figure 10: Mass-Metallicity relation. The black solid line and [PITH_FULL_IMAGE:figures/full_fig_p011_10.png]

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Works this paper leans on

90 extracted references

  1. [1]

    Adams, E. A. K., Šiljeg, B., Ponomareva, A. A., et al. 2026, A&A, 708, A122

    2026

  2. [2]

    Amorisco, N. C. & Loeb, A. 2016, MNRAS, 459, L51

    2016

  3. [3]

    2012, A&A, 545, A37

    Arnaboldi, M., Ventimiglia, G., Iodice, E., Gerhard, O., & Coccato, L. 2012, A&A, 545, A37

    2012

  4. [4]

    2010, in Proc

    Bacon, R., Accardo, M., Adjali, L., et al. 2010, in Proc. SPIE, V ol. 7735, Ground- based and Airborne Instrumentation for Astronomy III, 773508

    2010

  5. [5]

    2017, A&A, 608, A1

    Bacon, R., Conseil, S., Mary, D., et al. 2017, A&A, 608, A1

    2017

  6. [6]

    A., Phillips, M

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

    1981

  7. [7]

    J., Zaritsky, D., et al

    Bennet, P., Sand, D. J., Zaritsky, D., et al. 2018, ApJ, 866, L11

    2018

  8. [8]

    P., Vazdekis, A., & Ajhar, E

    Blakeslee, J. P., Vazdekis, A., & Ajhar, E. A. 2001, MNRAS, 320, 193

    2001

Show all 90 references
  1. [9]

    2023, A&A, 675, A123

    Boselli, A., Fossati, M., Côté, P., et al. 2023, A&A, 675, A123

    2023

  2. [10]

    2023, astropy/photutils: 1.8.0

    Bradley, L., Sip˝ocz, B., Robitaille, T., et al. 2023, astropy/photutils: 1.8.0

    2023

  3. [11]

    2025, A&A, 694, A276

    Buttitta, C., Iodice, E., Doll, G., et al. 2025, A&A, 694, A276

    2025

  4. [12]

    L., Forbes, D

    Buzzo, M. L., Forbes, D. A., Jarrett, T. H., et al. 2024, MNRAS, 529, 3210

    2024

  5. [13]

    L., Zanella, A., Hilker, M., et al

    Buzzo, M. L., Zanella, A., Hilker, M., et al. 2025, A&A, 700, A165 Calabrò, A., Amorín, R., Fontana, A., et al. 2017, A&A, 601, A95

    2025

  6. [14]

    C., et al

    Calzetti, D., Armus, L., Bohlin, R. C., et al. 2000, ApJ, 533, 682

    2000

  7. [15]

    2020, A&A, 639, A136

    Cantiello, M., Venhola, A., Grado, A., et al. 2020, A&A, 639, A136

    2020

  8. [16]

    2015, A&A, 581, A10

    Capaccioli, M., Spavone, M., Grado, A., et al. 2015, A&A, 581, A10

    2015

  9. [17]

    2017, MNRAS, 466, 798

    Cappellari, M. 2017, MNRAS, 466, 798

    2017

  10. [18]

    2023, MNRAS, 526, 3273

    Cappellari, M. 2023, MNRAS, 526, 3273

    2023

  11. [19]

    & Copin, Y

    Cappellari, M. & Copin, Y . 2003, MNRAS, 342, 345

    2003

  12. [20]

    & Emsellem, E

    Cappellari, M. & Emsellem, E. 2004, PASP, 116, 138

    2004

  13. [21]

    & Zabludoff, A

    Christlein, D. & Zabludoff, A. I. 2003, ApJ, 591, 764 D’Abrusco, R., Cantiello, M., Paolillo, M., et al. 2016, ApJ, 819, L31 Di Cintio, A., Brook, C. B., Dutton, A. A., et al. 2017, MNRAS, 466, L1

    2003

  14. [22]

    2026, A&A, 707, A88 Domínguez, A., Siana, B., Henry, A

    Doll, G., Buttitta, C., Iodice, E., et al. 2026, A&A, 707, A88 Domínguez, A., Siana, B., Henry, A. L., et al. 2013, ApJ, 763, 145

    2026

  15. [23]

    A., Kewley, L

    Dopita, M. A., Kewley, L. J., Sutherland, R. S., & Nicholls, D. C. 2016, Ap&SS, 361, 61

    2016

  16. [24]

    M., et al

    Duc, P.-A., Paudel, S., McDermid, R. M., et al. 2014, MNRAS, 440, 1458 Ferré-Mateu, A., Gannon, J. S., Forbes, D. A., et al. 2023, MNRAS

    2014

  17. [25]

    Fitzpatrick, E. L. & Massa, D. 2007, ApJ, 663, 320

    2007

  18. [26]

    A., Gannon, J., Iodice, E., et al

    Forbes, D. A., Gannon, J., Iodice, E., et al. 2023, MNRAS, 525, L93

    2023

  19. [27]

    2022, MNRAS, 510, 320 Article number, page 12 of 13 L

    Fraser-McKelvie, A., Cortese, L., Groves, B., et al. 2022, MNRAS, 510, 320 Article number, page 12 of 13 L. Rossi et al.: VI. The case study of UDG 6

    2022

  20. [28]

    Freeman, K. C. 1970, ApJ, 160, 811

    1970

  21. [29]

    M., et al

    Freudling, W., Romaniello, M., Bramich, D. M., et al. 2013, A&A, 559, A96

    2013

  22. [30]

    S., Ferré-Mateu, A., & Forbes, D

    Gannon, J. S., Ferré-Mateu, A., & Forbes, D. A. 2026, PASA, 43, e031

    2026

  23. [31]

    S., Forbes, D

    Gannon, J. S., Forbes, D. A., Romanowsky, A. J., et al. 2022, MNRAS, 510, 946

    2022

  24. [32]

    Gault, L., Leisman, L., Adams, E. A. K., et al. 2021, ApJ, 909, 19

    2021

  25. [33]

    Gerhard, O. E. 1993, MNRAS, 265, 213

    1993

  26. [34]

    2000, Astron

    Girardi, L., Bressan, A., Bertelli, G., & Chiosi, C. 2000, Astron. Astrophys. Suppl. Ser., 141, 371

    2000

  27. [35]

    P., Greene, J

    Greco, J. P., Greene, J. E., Strauss, M. A., et al. 2018, ApJ, 857, 104

    2018

  28. [36]

    A., Chilingarian, I

    Grishin, K. A., Chilingarian, I. V ., Afanasiev, A. V ., et al. 2021, Nature Astron- omy, 5, 1308

    2021

  29. [37]

    2025, A&A, 695, A91

    Hartke, J., Iodice, E., Gullieuszik, M., et al. 2025, A&A, 695, A91

    2025

  30. [38]

    M., Kotulla, R., Chen, H., et al

    Hess, K. M., Kotulla, R., Chen, H., et al. 2022, A&A, 668, A184

    2022

  31. [39]

    2013, ApJS, 208, 19

    Hinshaw, G., Larson, D., Komatsu, E., et al. 2013, ApJS, 208, 19

    2013

  32. [40]

    & Portinari, L

    Into, T. & Portinari, L. 2013, MNRAS, 430, 2715

    2013

  33. [41]

    2020, A&A, 642, A48

    Iodice, E., Cantiello, M., Hilker, M., et al. 2020, A&A, 642, A48

    2020

  34. [42]

    2023, A&A, 679, A69

    Iodice, E., Hilker, M., Doll, G., et al. 2023, A&A, 679, A69

    2023

  35. [43]

    2021, The Messenger, 183, 25

    Iodice, E., Spavone, M., Capaccioli, M., et al. 2021, The Messenger, 183, 25

    2021

  36. [44]

    M., & Dolag, K

    Ivleva, A., Remus, R.-S., Valenzuela, L. M., & Dolag, K. 2024, A&A, 687, A105

    2024

  37. [45]

    G., Leisman, L., & Webb, A

    Janowiecki, S., Jones, M. G., Leisman, L., & Webb, A. 2019, MNRAS, 490, 566

    2019

  38. [46]

    2015, ApJ, 812, 98

    Jimmy, Tran, K.-V ., Saintonge, A., et al. 2015, ApJ, 812, 98

    2015

  39. [47]

    2021, A&A, 650, A99

    Junais, Boissier, S., Boselli, A., et al. 2021, A&A, 650, A99

    2021

  40. [48]

    E., Huang, S., & Goulding, A

    Kado-Fong, E., Greene, J. E., Huang, S., & Goulding, A. 2022, ApJ, 941, 11

    2022

  41. [49]

    Kadowaki, J., Zaritsky, D., & Donnerstein, R. L. 2017, ApJ, 838, L21

    2017

  42. [50]

    2020, ApJ, 902, 39

    Karunakaran, A., Spekkens, K., Zaritsky, D., et al. 2020, ApJ, 902, 39

    2020

  43. [51]

    Kennicutt, Jr., R. C. 1998, ARA&A, 36, 189

    1998

  44. [52]

    J., Zaritsky, D., Sandoval Ascencio, L., Cooper, M

    Khim, D. J., Zaritsky, D., Sandoval Ascencio, L., Cooper, M. C., & Donnerstein, R. 2025, ApJ, 989, 154

    2025

  45. [53]

    N., Cohen, J

    Kirby, E. N., Cohen, J. G., Guhathakurta, P., et al. 2013, ApJ, 779, 102

    2013

  46. [54]

    M., et al

    Koch, A., Burkert, A., Rich, R. M., et al. 2012, ApJ, 755, L13

    2012

  47. [55]

    2001, MNRAS, 322, 231 La Marca, A., Iodice, E., Cantiello, M., et al

    Kroupa, P. 2001, MNRAS, 322, 231 La Marca, A., Iodice, E., Cantiello, M., et al. 2022a, A&A, 665, A105 La Marca, A., Peletier, R., Iodice, E., et al. 2022b, A&A, 659, A92 Lara-López, M. A., Galán-de Anta, P. M., Sarzi, M., et al. 2022, A&A, 660, A105

    2001

  48. [56]

    G., Yuk, I.-S., Park, H

    Lee, M. G., Yuk, I.-S., Park, H. S., Harris, J., & Zaritsky, D. 2009, ApJ, 703, 692

    2009

  49. [57]

    P., Janowiecki, S., et al

    Leisman, L., Haynes, M. P., Janowiecki, S., et al. 2017, ApJ, 842, 133

    2017

  50. [58]

    2015, A&A, 584, A113

    Lelli, F., Duc, P.-A., Brinks, E., et al. 2015, A&A, 584, A113

    2015

  51. [59]

    W., et al

    Lim, S., Côté, P., Peng, E. W., et al. 2020, ApJ, 899, 69

    2020

  52. [60]

    2021, MNRAS, 500, 1323

    Lima-Dias, C., Monachesi, A., Torres-Flores, S., et al. 2021, MNRAS, 500, 1323

    2021

  53. [61]

    A., Blyth, S

    Makda, N. A., Blyth, S. L., & Skelton, R. E. 2025, MNRAS, 544, 3824 Mancera Piña, P. E., Aguerri, J. A. L., Peletier, R. F., et al. 2019, MNRAS, 485, 1036 Mancera Piña, P. E., Fraternali, F., Oman, K. A., et al. 2020, MNRAS, 495, 3636 Mancera Piña, P. E., Golini, G., Trujillo,...

    2025

  54. [62]

    R., Cuillandre, J.-C., Cantiello, M., et al

    Marleau, F. R., Cuillandre, J.-C., Cantiello, M., et al. 2025, A&A, 697, A12

    2025

  55. [63]

    2024, A&A, 691, A104

    Mirabile, M., Cantiello, M., Lonare, P., et al. 2024, A&A, 691, A104

    2024

  56. [64]

    2026, A&A, 705, A117

    Mirabile, M., Cantiello, M., Rejkuba, M., et al. 2026, A&A, 705, A117

    2026

  57. [65]

    2008, A&A, 486, 697 Müller, O., Rich, R

    Misgeld, I., Mieske, S., & Hilker, M. 2008, A&A, 486, 697 Müller, O., Rich, R. M., Román, J., et al. 2019, A&A, 624, L6

    2008

  58. [66]

    Osterbrock, D. E. & Ferland, G. J. 2006, Astrophysics of gaseous nebulae and active galactic nuclei (University Science Books)

    2006

  59. [67]

    Papastergis, E., Adams, E. A. K., & Romanowsky, A. J. 2017, A&A, 601, L10

    2017

  60. [68]

    2018, MNRAS, 474, 580

    Ploeckinger, S., Sharma, K., Schaye, J., et al. 2018, MNRAS, 474, 580

    2018

  61. [69]

    M., Moretti, A., Gullieuszik, M., et al

    Poggianti, B. M., Moretti, A., Gullieuszik, M., et al. 2017, ApJ, 844, 48

    2017

  62. [70]

    J., van der Burg, R

    Prole, D. J., van der Burg, R. F. J., Hilker, M., & Davies, J. I. 2019, MNRAS, 488, 2143

    2019

  63. [71]

    2014, A&A, 561, A10

    Proxauf, B., Öttl, S., & Kimeswenger, S. 2014, A&A, 561, A10

    2014

  64. [72]

    2017, ApJ, 843, 128 Román, J

    Rhee, J., Smith, R., Choi, H., et al. 2017, ApJ, 843, 128 Román, J. & Trujillo, I. 2017, MNRAS, 468, 4039 Romero-Gómez, J., Peletier, R. F., Aguerri, J. A. L., et al. 2023, MNRAS, 522, 130

    2017

  65. [73]

    2017, MNRAS, 470, 4231

    Rong, Y ., Guo, Q., Gao, L., et al. 2017, MNRAS, 470, 4231

    2017

  66. [74]

    & Scannapieco, E

    Safarzadeh, M. & Scannapieco, E. 2017, ApJ, 850, 99

    2017

  67. [75]

    V ., Navarro, J

    Sales, L. V ., Navarro, J. F., Peñafiel, L., et al. 2020, MNRAS, 494, 1848

    2020

  68. [76]

    Salpeter, E. E. 1955, ApJ, 121, 161

    1955

  69. [77]

    T., Lilly, S

    Soto, K. T., Lilly, S. J., Bacon, R., Richard, J., & Conseil, S. 2016, MNRAS, 458, 3210

    2016

  70. [78]

    S., et al

    Spavone, M., Iodice, E., Lohmann, F. S., et al. 2024, A&A, 689, A306

    2024

  71. [79]

    & Karunakaran, A

    Spekkens, K. & Karunakaran, A. 2018, ApJ, 855, 28

    2018

  72. [80]

    2026, A&A, 707, A107

    Taylor, R., Partík, V ., & Minchin, R. 2026, A&A, 707, A107

    2026

  73. [81]

    2017, ApJ, 836, 191 van der Burg, R

    Trujillo, I., Roman, J., Filho, M., & Sánchez Almeida, J. 2017, ApJ, 836, 191 van der Burg, R. F. J., Muzzin, A., & Hoekstra, H. 2016, A&A, 590, A20 van der Marel, R. P. & Franx, M. 1993, ApJ, 407, 525 van Dokkum, P. G., Romanowsky, A. J., Abraham, R., et al. 2015, ApJ, 804, L26

    2017

  74. [82]

    F., & Beckman, J

    Vazdekis, A., Casuso, E., Peletier, R. F., & Beckman, J. E. 1996, ApJS, 106, 307

    1996

  75. [83]

    2016, MNRAS, 463, 3409

    Vazdekis, A., Koleva, M., Ricciardelli, E., Röck, B., & Falcón-Barroso, J. 2016, MNRAS, 463, 3409

    2016

  76. [84]

    J., et al

    Vazdekis, A., Ricciardelli, E., Cenarro, A. J., et al. 2012, MNRAS, 424, 157

    2012

  77. [85]

    2017, A&A, 608, A142

    Venhola, A., Peletier, R., Laurikainen, E., et al. 2017, A&A, 608, A142

    2017

  78. [86]

    M., Palsa, R., Streicher, O., et al

    Weilbacher, P. M., Palsa, R., Streicher, O., et al. 2020, A&A, 641, A28

    2020

  79. [87]

    2022, PASA, 39, e058

    Westmeier, T., Deg, N., Spekkens, K., et al. 2022, PASA, 39, e058

    2022

  80. [88]

    2017, MNRAS, 470, 1512

    Wittmann, C., Lisker, T., Ambachew Tilahun, L., et al. 2017, MNRAS, 470, 1512

    2017

  81. [89]

    & Behroozi, P

    Zaritsky, D. & Behroozi, P. 2023, MNRAS, 519, 871

    2023

  82. [90]

    Federico II

    Zaritsky, D., Donnerstein, R., Dey, A., et al. 2023, ApJS, 267, 27 1 INAF−Astronomical Observatory of Capodimonte, Salita Moiariello 16, I-80131, Naples, Italy 2 University of Naples “Federico II”, C.U. Monte Sant’Angelo, Via Cinthia, 80126, Naples, Italy 3 INAF−Osservatorio A...

    2023

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