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A Deep Study of the Spiral Galaxy W2246f

T0 review · 2 major / 2 minor · reviewed 2026-06-29 · grok-4.3

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Pith's one-line read W2246f is a cLIER galaxy whose central kiloparsec is dominated by old metal-poor stars with little star formation.

desk verdict A straightforward case study of inside-out quenching in one low-z spiral using deep MUSE data, with the central retired classification resting on standard but un-cross-checked diagnostics. read the letter →

arxiv 2605.29014 v1 pith:D23OYWLH submitted 2026-05-27 astro-ph.GA

Evelyn J. Johnston , Sorya Lambert , Aparna Nair , Alejandra Z. Lugo-Aranda , Manuel Aravena , Roberto J. Assef , Tanio Diaz Santos , Román Fernández Aranda
show 5 more authors
Hyunsung D. Jun Guodong Li Mai Liao Devika Shobhana Chao-Wei Tsai
This is my paper
classification astro-ph.GA
keywords spiralgalaxycLIERinside-outquenchingstellarpopulationsionizedgasmetallicitygradientMUSEspectroscopy
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 uses unusually deep MUSE integral-field observations of the spiral galaxy W2246f at redshift 0.09 to map its stellar populations, gas properties, and ionization sources at high spatial resolution. It finds that the central region shows older luminosity-weighted stellar ages, lower gas metallicity, and retired emission classified as LIER, while the surrounding disc shows ongoing star formation. The mass-weighted ages remain flat across the galaxy, and the overall pattern matches inside-out quenching in which star formation ceases first in the center. This detailed single-galaxy study illustrates how quenching can proceed spatially even when large surveys lose such resolution.

What carries the argument

The WHAN and WHaD diagrams together with the O3N2 calibrator, which classify the dominant ionization source and measure gas metallicity in each spatial bin.

What would settle it

New observations that detect strong AGN-like line ratios or shock signatures in the central kiloparsec would falsify the retired, hot-evolved-star interpretation.

Watch

Extended reading notes

Core claim

W2246f is a cLIER galaxy. The central kiloparsec is dominated by old, metal-poor stars with little star formation, and the central LIER emission is powered primarily by hot evolved stars. The rest of the disc shows ongoing star formation, a negative metallicity gradient, and a drop in star-formation-rate density toward the center. These properties are consistent with inside-out quenching.

Load-bearing premise

The WHAN and WHaD diagrams plus the O3N2 calibrator correctly identify the ionization source and metallicity in the central region without significant bias from dust, shocks, or non-stellar contributions.

Editorial extensions

If this is right

  • The central kiloparsec has retired with emission powered by hot evolved stars rather than star formation.
  • Star-formation-rate density and gas metallicity both decline toward the center.
  • Luminosity-weighted ages show a negative gradient while mass-weighted ages stay flat across the disc.
  • The galaxy as a whole follows an inside-out quenching pattern.

Reading between the lines

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

  • If the retired classification holds, it shows that hot evolved stars alone can sustain LIER emission across an entire central kiloparsec without requiring an active nucleus.
  • The contrast between flat mass-weighted ages and younger outer luminosity-weighted ages implies that recent star formation has been suppressed only in the center.
  • Deep IFU maps of similar low-redshift spirals could test whether cLIER signatures appear mainly in galaxies of this mass and morphology.
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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

2 major / 2 minor

Summary. The manuscript presents a MUSE integral-field spectroscopic study of the spiral galaxy W2246f at z≈0.09. It derives spatially resolved stellar kinematics, luminosity- and mass-weighted ages and metallicities, gas extinction, oxygen abundances via the O3N2 calibrator, and star-formation rates. Using the WHAN and WHaD diagrams, the central kiloparsec is classified as retired (cLIER) with ionization powered by hot evolved stars, while the disc is star-forming; the radial profiles are interpreted as evidence for inside-out quenching.

Significance. If the ionization classification holds, the work supplies a high-spatial-resolution case study of a cLIER galaxy at moderate redshift, with detailed radial gradients in stellar populations and gas properties that directly support inside-out quenching scenarios. The depth of the MUSE data enables resolution finer than typical IFU surveys at this redshift.

major comments (2)
  1. [Abstract and gas properties analysis] Abstract (gas properties and ionization analysis): the central claim that the inner kpc is retired and powered by hot evolved stars rests on direct application of the WHAN and WHaD diagrams plus O3N2 metallicities. No cross-checks against the BPT diagram, alternative line-ratio diagnostics, or post-AGB photoionization models are reported to exclude possible contamination by shocks or differential dust in the central spaxels; if such contamination is present the retired-versus-star-forming distinction collapses.
  2. [Stellar populations and radial profiles] Stellar population results (radial profiles): the reported flat mass-weighted ages and negative luminosity-weighted age gradient are used to support the quenching scenario, yet the spatial masking of the central region is informed by the same gas diagnostics whose robustness is unverified; this coupling makes the stellar-population interpretation dependent on the untested ionization classification.
minor comments (2)
  1. [Abstract] The phrase 'nice example' in the abstract is informal; replace with 'clear example' or equivalent.
  2. [Gas metallicity] The O3N2 calibrator is listed among the derived quantities; state explicitly which published calibration relation is adopted and any assumed solar abundance scale.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments on our manuscript. We address each major comment below and commit to revisions that will strengthen the presentation of the ionization classification and its relation to the stellar population results.

read point-by-point responses

  1. Referee: [Abstract and gas properties analysis] Abstract (gas properties and ionization analysis): the central claim that the inner kpc is retired and powered by hot evolved stars rests on direct application of the WHAN and WHaD diagrams plus O3N2 metallicities. No cross-checks against the BPT diagram, alternative line-ratio diagnostics, or post-AGB photoionization models are reported to exclude possible contamination by shocks or differential dust in the central spaxels; if such contamination is present the retired-versus-star-forming distinction collapses.

    Authors: We agree that additional cross-checks would strengthen the robustness of the retired classification. The WHAN and WHaD diagrams were selected because they are specifically calibrated for low-ionization emission in retired galaxies and have been validated against other methods in the literature. In the revised manuscript we will add the BPT diagram for the central spaxels, compare the resulting classifications, and discuss consistency with post-AGB photoionization models. We will also use the existing velocity dispersion and extinction maps to argue against significant shock or differential-dust contamination. These additions will be incorporated without changing the main conclusions. revision: yes

  2. Referee: [Stellar populations and radial profiles] Stellar population results (radial profiles): the reported flat mass-weighted ages and negative luminosity-weighted age gradient are used to support the quenching scenario, yet the spatial masking of the central region is informed by the same gas diagnostics whose robustness is unverified; this coupling makes the stellar-population interpretation dependent on the untested ionization classification.

    Authors: The stellar population fitting was performed independently on all spaxels above a uniform S/N threshold using full-spectrum fitting; the radial profiles were constructed in fixed radial annuli. The central retired classification is used only for interpretive discussion, not for defining the masks applied to the stellar maps. In the revision we will explicitly document the S/N-based masking criteria, add a supplementary figure showing the stellar population gradients under purely S/N masking, and clarify that the inside-out quenching interpretation rests on the combination of age gradients, SFR density decline, and metallicity profile rather than on the gas classification alone. revision: partial

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: purely observational application of external diagnostics

full rationale

The paper performs a standard IFU analysis of MUSE data on W2246f, extracting stellar population parameters (ages, metallicities), gas kinematics, extinction, SFR, and metallicities via the published O3N2 calibrator, then classifying ionization sources with the published WHAN and WHaD diagrams. None of these steps involve equations that define outputs in terms of the same fitted quantities, self-citations that bear the central claim, or predictions that reduce to inputs by construction. The cLIER classification and inside-out quenching interpretation are direct consequences of applying these independent, externally validated tools to the observed spectra; the derivation chain is self-contained against external benchmarks.

Assumptions & free parameters 1 free parameters · 2 assumptions · 0 invented entities

The central claim rests on standard domain assumptions about spectral diagnostics and stellar population models rather than new free parameters or postulated entities.

free parameters (1)
  • O3N2 calibrator
    Choice of strong-line calibrator for oxygen abundance; different calibrators can shift the reported metallicity gradient.
assumptions (2)
  • domain assumption WHAN and WHaD diagrams reliably separate star-forming from retired (LIER) ionization without significant contamination
    Invoked to classify the central region as retired and the disk as star-forming.
  • domain assumption Stellar population synthesis models recover unbiased luminosity- and mass-weighted ages and metallicities from the observed spectra
    Required for the reported radial profiles and the claim of older central populations.

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Cite this review

Pith. "Pith review of A Deep Study of the Spiral Galaxy W2246f." pith.science (2026). https://pith.science/paper/D23OYWLH

@misc{pith2026260529014,
  author       = {Pith},
  title        = {Pith review of: A Deep Study of the Spiral Galaxy W2246f},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/D23OYWLH}},
  note         = {Machine review of arXiv:2605.29014}
}
abstract

In this era of large surveys and statistical studies of galaxies, the beauty in the details of individual galaxies is often lost. We present a deep study of the spiral galaxy W2246f with MUSE, exploring the spatially-resolved stellar and ionized gas properties to understand how it formed and evolved over time. The unusually deep observations of this galaxy give us a rare opportunity to study this phenomenon with better spatial resolution than can normally be achieved with the current IFU surveys of galaxies at a similar redshift ($z\sim0.09$). We analyse the stellar and gas kinematics, as well as the spatially resolved stellar populations and gas properties, including gas metallicity and the dominant ionization sources. The derived properties include the stellar mass, radial profiles of luminosity- and mass-weighted mean ages and metallicities, and ionized gas characteristics such as E(B-V), H$\alpha$ extinction, dust-corrected H$\alpha$ flux, oxygen abundance using the O3N2 calibrator, and H$\alpha$-based star formation rate. Analysis of the stellar populations revealed a negative metallicity gradient, and the mass-weighted ages showed uniformly flat ages across the disc while the luminosity-weighted ages show a negative gradient. We find that the gas metallicity and star formation rate density also drop in the central region of the galaxy where the older luminosity-weighted stellar populations are found. Analysis of the WHAN and WHaD diagrams reveal that in fact the central region is retired while the rest of the disc is star forming. We conclude that W2246f is a nice example of a cLIER galaxy, where the central kpc is dominated by old, metal-poor stars with little star formation. The central LIER emission is primarily powered by hot evolved stars, while the rest of the disc displays ongoing star formation. These findings are consistent with a scenario of inside-out quenching.

Figures

Figures reproduced from arXiv: 2605.29014 by the authors.

Figure 1
Figure 1. Images of W2246f and its companion galaxy to the North-West, extracted from the MUSE datacube. On the left is the white [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Maps of the stellar (top) and gas (bottom) kinematics, showing from left to right the line of sight velocities, velocity [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Maps showing the stellar line of sight velocities (left) [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: Example fits with pPXF to two spectra from the galaxy. On the left is a spectrum taken from close to the center of the galaxy [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: Overview of the mass- and luminosity-weighted ages (top) and metallicities (bottom). On the left are radial plots for these [PITH_FULL_IMAGE:figures/full_fig_p007_5.png]
Figure 6
Figure 6. Figure 6: The BPT diagram for W2246f at the top along with the [S ii] (middle) and [O i] diagnostic diagrams on the left. The brown curves represent the maximum starburst line of Kewley et al. (2001), the dashed brown lines represent the separation between Seyferts and LINERs fr…
Figure 7
Figure 7. Figure 7: Reddening (left) and extinction (right) maps of W2246f. [PITH_FULL_IMAGE:figures/full_fig_p009_7.png]
Figure 8
Figure 8. Figure 8: The WHAN (top) and WHaD (bottom) diagrams for W2246f on the left and the cor￾responding maps on the right. The gray lines demonstrate the regions of each diagram that are dominated by different ionization sources, such as star formation (SF), Seyferts (sAGN), LINERS (w…
Figure 9
Figure 9. Figure 9: The gas metallicity (top) and the SFR density (bottom), plotted as a function of distance from the centre of the galaxy on [PITH_FULL_IMAGE:figures/full_fig_p012_9.png]

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Works this paper leans on

120 extracted references · 2 canonical work pages

  1. [1]

    Agostino, C. J. & Salim, S. 2019, ApJ, 876, 12 Aragon Calvo, M. A., Neyrinck, M. C., & Silk, J. 2019, The Open Journal of Astrophysics, 2, 7

    2019

  2. [2]

    Aragon-Calvo, M. A. & Szalay, A. S. 2013, MNRAS, 428, 3409

    2013

  3. [3]

    2010, in Society of Photo-Optical In- strumentation Engineers (SPIE) Conference Series, V ol

    Bacon, R., Accardo, M., Adjali, L., et al. 2010, in Society of Photo-Optical In- strumentation Engineers (SPIE) Conference Series, V ol. 7735, Ground-based and Airborne Instrumentation for Astronomy III, 773508

    2010

  4. [4]

    A., Phillips, M

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

    1981

  5. [5]

    2022, ApJ, 926, L13

    Bao, M., Chen, Y ., Zhu, P., et al. 2022, ApJ, 926, L13

    2022

  6. [6]

    2015, MNRAS, 449, 867

    Belfiore, F., Maiolino, R., Bundy, K., et al. 2015, MNRAS, 449, 867

    2015

  7. [7]

    2016, MNRAS, 461, 3111

    Belfiore, F., Maiolino, R., Maraston, C., et al. 2016, MNRAS, 461, 3111

    2016

  8. [8]

    2017, MNRAS, 469, 151

    Belfiore, F., Maiolino, R., Tremonti, C., et al. 2017, MNRAS, 469, 151

    2017

Show all 120 references
  1. [9]

    G., Stasi´nska, G., & Bruzual, A

    Binette, L., Magris, C. G., Stasi´nska, G., & Bruzual, A. G. 1994, A&A, 292, 13

    1994

  2. [10]

    C., Rodríguez-Pérez, C., et al

    Borlaff, A., Eliche-Moral, M. C., Rodríguez-Pérez, C., et al. 2014, A&A, 570, A103

    2014

  3. [11]

    D., Tojeiro, R., Aubourg, É., et al

    Brandt, T. D., Tojeiro, R., Aubourg, É., et al. 2010, AJ, 140, 804

    2010

  4. [12]

    M., et al

    Breda, I., Papaderos, P., Gomes, J. M., et al. 2020, A&A, 635, A177

    2020

  5. [13]

    J., Owers, M

    Bryant, J. J., Owers, M. S., Robotham, A. S. G., et al. 2015, MNRAS, 447, 2857

    2015

  6. [14]

    A., Law, D

    Bundy, K., Bershady, M. A., Law, D. R., et al. 2015, ApJ, 798, 7

    2015

  7. [15]

    R., Ellison, S

    Byrne-Mamahit, S., Patton, D. R., Ellison, S. L., et al. 2024, MNRAS, 528, 5864

    2024

  8. [16]

    2013, in Secular Evolution of Galaxies, ed

    Calzetti, D. 2013, in Secular Evolution of Galaxies, ed. J. Falcón-Barroso & J. H. Knapen, 419

    2013

  9. [17]

    C., et al

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

    2000

  10. [18]

    C., Engelbracht, C

    Calzetti, D., Kennicutt, R. C., Engelbracht, C. W., et al. 2007, ApJ, 666, 870 Cano-Díaz, M., Sánchez, S. F., Zibetti, S., et al. 2016, ApJ, 821, L26

    2007

  11. [19]

    2017, MNRAS, 466, 798

    Cappellari, M. 2017, MNRAS, 466, 798

    2017

  12. [20]

    2023, MNRAS, 526, 3273

    Cappellari, M. 2023, MNRAS, 526, 3273

    2023

  13. [21]

    2025, MNRAS, 544, 1432

    Cappellari, M. 2025, MNRAS, 544, 1432

    2025

  14. [22]

    A., Clayton, G

    Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245

    1989

  15. [23]

    Casteels, K. R. V ., Bamford, S. P., Skibba, R. A., et al. 2013, MNRAS, 429, 1051 Catalán-Torrecilla, C., Gil de Paz, A., Castillo-Morales, A., et al. 2015, A&A, 584, A87 Catalán-Torrecilla, C., Gil de Paz, A., Castillo-Morales, A., et al. 2017, ApJ, 848, 87

    2013

  16. [24]

    2016, MNRAS, 457, 2605

    Ceverino, D., Sánchez Almeida, J., Muñoz Tuñón, C., et al. 2016, MNRAS, 457, 2605

    2016

  17. [25]

    D., Dolgachev, V

    Chernin, A. D., Dolgachev, V . P., & Domozhilova, L. M. 2000, MNRAS, 319, 851 Cid Fernandes, R., Carvalho, M. S., Sánchez, S. F., de Amorim, A., & Ruschel-

    2000

  18. [26]

    2021, MNRAS, 502, 1386 Cid Fernandes, R., Stasi ´nska, G., Mateus, A., & Vale Asari, N

    Dutra, D. 2021, MNRAS, 502, 1386 Cid Fernandes, R., Stasi ´nska, G., Mateus, A., & Vale Asari, N. 2011, MNRAS, 413, 1687

    2021

  19. [27]

    M., Lawrence, J

    Croom, S. M., Lawrence, J. S., Bland-Hawthorn, J., et al. 2012, MNRAS, 421, 872

    2012

  20. [28]

    2022, MNRAS, 512, 4136

    Curti, M., Hayden-Pawson, C., Maiolino, R., et al. 2022, MNRAS, 512, 4136

    2022

  21. [29]

    Davies, L. J. M., Driver, S. P., Robotham, A. S. G., et al. 2016, MNRAS, 461, 458

    2016

  22. [30]

    Davis, T. A. & Bureau, M. 2016, MNRAS, 457, 272 Di Matteo, P., Haywood, M., Combes, F., Semelin, B., & Snaith, O. N. 2013, A&A, 553, A102 Díaz-Santos, T., Assef, R. J., Blain, A. W., et al. 2018, Science, 362, 1034 Díaz-Santos, T., Assef, R. J., Blain, A. W., et al. 2016, ApJ,...

    2016

  23. [31]

    Dopita, M. A. & Sutherland, R. S. 1996, ApJS, 102, 161

    1996

  24. [32]

    A., Kreckel, K., et al

    Drory, N., Blanc, G. A., Kreckel, K., et al. 2024, AJ, 168, 198

    2024

  25. [33]

    Easeman, B., Schady, P., Wuyts, S., & Yates, R. M. 2022, MNRAS, 511, 371 Ebrová, I., Bílek, M., & Eliášek, J. 2025, arXiv e-prints, arXiv:2510.02257

    2022

  26. [34]

    2025, arXiv e-prints, arXiv:2511.00235

    Egorova, E., Kreckel, K., Egorov, O., et al. 2025, arXiv e-prints, arXiv:2511.00235

    2025

  27. [35]

    C., Rodríguez-Pérez, C., Borlaff, A., Querejeta, M., & Tapia, T

    Eliche-Moral, M. C., Rodríguez-Pérez, C., Borlaff, A., Querejeta, M., & Tapia, T. 2018, A&A, 617, A113

    2018

  28. [36]

    L., Patton, D

    Ellison, S. L., Patton, D. R., Simard, L., & McConnachie, A. W. 2008, AJ, 135, 1877

    2008

  29. [37]

    2022, A&A, 659, A191

    Emsellem, E., Schinnerer, E., Santoro, F., et al. 2022, A&A, 659, A191

    2022

  30. [38]

    M., den Brok, M., et al

    Erroz-Ferrer, S., Carollo, C. M., den Brok, M., et al. 2019, MNRAS, 484, 5009 ESO CPL Development Team. 2015, EsoRex: ESO Recipe Execution Tool, As- trophysics Source Code Library

    2019

  31. [39]

    K., & Shu, X

    Fan, L., Gao, Y ., Knudsen, K. K., & Shu, X. 2018, ApJ, 854, 157

    2018

  32. [40]

    M., Boquien, M., & Zackrisson, E

    Fensch, J., Duc, P.-A., Weilbacher, P. M., Boquien, M., & Zackrisson, E. 2016, A&A, 585, A79

    2016

  33. [41]

    Fitzpatrick, E. L. 1999, PASP, 111, 63

    1999

  34. [42]

    2011, MNRAS, 415, 2182 Flores Velázquez, J

    Flores-Fajardo, N., Morisset, C., Stasi ´nska, G., & Binette, L. 2011, MNRAS, 415, 2182 Flores Velázquez, J. A., Gurvich, A. B., Faucher-Giguère, C.-A., et al. 2021, MNRAS, 501, 4812

    2011

  35. [43]

    M., et al

    Franchetto, A., Mingozzi, M., Poggianti, B. M., et al. 2021, ApJ, 923, 28

    2021

  36. [44]

    A., Bittner, A., Falcón-Barroso, J., et al

    Gadotti, D. A., Bittner, A., Falcón-Barroso, J., et al. 2020, A&A, 643, A14

    2020

  37. [45]

    A., Sánchez-Blázquez, P., Falcón-Barroso, J., et al

    Gadotti, D. A., Sánchez-Blázquez, P., Falcón-Barroso, J., et al. 2019, MNRAS, 482, 506

    2019

  38. [46]

    Gibson, B. K. 1997, MNRAS, 290, 471

    1997

  39. [47]

    2017, MNRAS, 466, 4731 González Delgado, R

    Goddard, D., Thomas, D., Maraston, C., et al. 2017, MNRAS, 466, 4731 González Delgado, R. M., Pérez, E., Cid Fernandes, R., et al. 2017, A&A, 607, A128

    2017

  40. [48]

    W., Glazebrook, K., McGregor, P

    Green, A. W., Glazebrook, K., McGregor, P. J., et al. 2010, Nature, 467, 684 Article number, page 13 A&A proofs:manuscript no. Leda_galaxy_v3_CLEAN

    2010

  41. [49]

    W., Glazebrook, K., McGregor, P

    Green, A. W., Glazebrook, K., McGregor, P. J., et al. 2014, MNRAS, 437, 1070

    2014

  42. [50]

    Groves, B., Brinchmann, J., & Walcher, C. J. 2012, MNRAS, 419, 1402

    2012

  43. [51]

    2023, ApJ, 959, 39 Häußler, B., Bamford, S

    Harikane, Y ., Zhang, Y ., Nakajima, K., et al. 2023, ApJ, 959, 39 Häußler, B., Bamford, S. P., Vika, M., et al. 2013, MNRAS, 430, 330 Häußler, B., McIntosh, D. H., Barden, M., et al. 2007, ApJS, 172, 615

    2023

  44. [52]

    J., Lee, H., MacQueen, P

    Hill, G. J., Lee, H., MacQueen, P. J., et al. 2021, AJ, 162, 298

    2021

  45. [53]

    Hummer, D. G. & Storey, P. J. 1987, MNRAS, 224, 801

    1987

  46. [54]

    C., Smith, H

    Hung, C.-L., Hayward, C. C., Smith, H. A., et al. 2016, ApJ, 816, 99

    2016

  47. [55]

    J., Häußler, B., & Nedkova, K

    Jegatheesan, K., Johnston, E. J., Häußler, B., & Nedkova, K. V . 2024, A&A, 684, A32

    2024

  48. [56]

    2024, A&A, 681, A95

    Jin, Y ., Zhu, L., Zibetti, S., et al. 2024, A&A, 681, A95

    2024

  49. [57]

    J., Hau, G

    Johnston, E. J., Hau, G. K. T., Coccato, L., & Herrera, C. 2018, MNRAS, 480, 3215

    2018

  50. [58]

    M., Tremonti, C., et al

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

    2003

  51. [59]

    1998, ApJ, 498, 541

    Kennicutt, Robert C., J. 1998, ApJ, 498, 541

    1998

  52. [60]

    Kennicutt, R. C. & Evans, N. J. 2012, ARA&A, 50, 531

    2012

  53. [61]

    J., Dopita, M

    Kewley, L. J., Dopita, M. A., Sutherland, R. S., Heisler, C. A., & Trevena, J. 2001, ApJ, 556, 121

    2001

  54. [62]

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

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

    2006

  55. [63]

    D., Onoue, M., Inayoshi, K., et al

    Kocevski, D. D., Onoue, M., Inayoshi, K., et al. 2023, ApJ, 954, L4

    2023

  56. [64]

    2015, MNRAS, 453, 879 Krajnovi´c, D., Weilbacher, P

    Koyama, Y ., Kodama, T., Hayashi, M., et al. 2015, MNRAS, 453, 879 Krajnovi´c, D., Weilbacher, P. M., Urrutia, T., et al. 2015, MNRAS, 452, 2

    2015

  57. [65]

    Lacerda, E. A. D., Cid Fernandes, R., Couto, G. S., et al. 2018, MNRAS, 474, 3727

    2018

  58. [66]

    M., et al

    Lah, P., Scott, N., Barone, T. M., et al. 2023, PASA, 40, e002 Lara-López, M. A., Galán-de Anta, P. M., Sarzi, M., et al. 2022, A&A, 660, A105

    2023

  59. [67]

    2010, A&A, 516, A11

    Lelli, F., Fraternali, F., & Sancisi, R. 2010, A&A, 516, A11

    2010

  60. [68]

    K., Bigiel, F., de Blok, W

    Leroy, A. K., Bigiel, F., de Blok, W. J. G., et al. 2012, AJ, 144, 3

    2012

  61. [69]

    M., Jing, Y

    Li, C., Kauffmann, G., Heckman, T. M., Jing, Y . P., & White, S. D. M. 2008, MNRAS, 385, 1903

    2008

  62. [70]

    2018, MNRAS, 476, 3883 López-Cobá, C., Sánchez, S

    Lian, J., Thomas, D., Maraston, C., et al. 2018, MNRAS, 476, 3883 López-Cobá, C., Sánchez, S. F., Anderson, J. P., et al. 2020, AJ, 159, 167

    2018

  63. [71]

    P., Fabbiano, G., et al

    Ma, J., Maksym, W. P., Fabbiano, G., et al. 2021, ApJ, 908, 155

    2021

  64. [72]

    2024, A&A, 691, A145

    Maiolino, R., Scholtz, J., Curtis-Lake, E., et al. 2024, A&A, 691, A145

    2024

  65. [73]

    2005, A&A, 433, 807

    Mannucci, F., Della Valle, M., Panagia, N., et al. 2005, A&A, 433, 807

    2005

  66. [74]

    & Mannucci, F

    Maoz, D. & Mannucci, F. 2012, PASA, 29, 447

    2012

  67. [75]

    2011, MNRAS, 412, 1508

    Maoz, D., Mannucci, F., Li, W., et al. 2011, MNRAS, 412, 1508

    2011

  68. [76]

    2025, A&A, 701, A113

    Marconcini, C., Feltre, A., Lamperti, I., et al. 2025, A&A, 701, A113

    2025

  69. [77]

    A., Rosales-Ortega, F

    Marino, R. A., Rosales-Ortega, F. F., Sánchez, S. F., et al. 2013, A&A, 559, A114 Martínez-Delgado, D., Stein, M., Sakowska, J. D., et al. 2025, A&A, 701, A182

    2013

  70. [78]

    & Francois, P

    Matteucci, F. & Francois, P. 1989, MNRAS, 239, 885

    1989

  71. [79]

    2009, A&A, 501, 531

    Matteucci, F., Spitoni, E., Recchi, S., & Valiante, R. 2009, A&A, 501, 531

    2009

  72. [80]

    M., U, V ., Guedes, J., et al

    Medling, A. M., U, V ., Guedes, J., et al. 2014, ApJ, 784, 70

    2014

  73. [81]

    G., Alonso, M

    Michel-Dansac, L., Lambas, D. G., Alonso, M. S., & Tissera, P. 2008, MNRAS, 386, L82

    2008

  74. [82]

    C., Tremonti, C

    Moustakas, J., Kennicutt, Jr., R. C., Tremonti, C. A., et al. 2010, ApJS, 190, 233

    2010

  75. [83]

    2014, MNRAS, 444, 3357

    Naab, T., Oser, L., Emsellem, E., et al. 2014, MNRAS, 444, 3357

    2014

  76. [84]

    & Maiolino, R

    Nakajima, K. & Maiolino, R. 2022, MNRAS, 513, 5134

    2022

  77. [85]

    M., et al

    Nedelchev, B., Coccato, L., Corsini, E. M., et al. 2019, A&A, 623, A87

    2019

  78. [86]

    V ., Häußler, B., Marchesini, D., et al

    Nedkova, K. V ., Häußler, B., Marchesini, D., et al. 2021, MNRAS, 506, 928

    2021

  79. [87]

    2004, MNRAS, 355, 874

    Nikolic, B., Cullen, H., & Alexander, P. 2004, MNRAS, 355, 874

    2004

  80. [88]

    Osterbrock, D. E. 1989, Astrophysics of gaseous nebulae and active galactic nu- clei (University Science Books)

    1989

  81. [89]

    2021, MNRAS, 502, 5508

    Parikh, T., Thomas, D., Maraston, C., et al. 2021, MNRAS, 502, 5508

    2021

  82. [90]

    R., Ellison, S

    Patton, D. R., Ellison, S. L., Simard, L., McConnachie, A. W., & Mendel, J. T. 2011, MNRAS, 412, 591

    2011

  83. [91]

    R., Faria, L., Hani, M

    Patton, D. R., Faria, L., Hani, M. H., et al. 2024, MNRAS, 529, 1493

    2024

  84. [92]

    Y ., Ho, L

    Peng, C. Y ., Ho, L. C., Impey, C. D., & Rix, H.-W. 2002, AJ, 124, 266

    2002

  85. [93]

    Y ., Ho, L

    Peng, C. Y ., Ho, L. C., Impey, C. D., & Rix, H.-W. 2010, AJ, 139, 2097 Pérez-Montero, E. & Contini, T. 2009, MNRAS, 398, 949

    2010

  86. [94]

    2023, A&A, 673, A147

    Pessa, I., Schinnerer, E., Sanchez-Blazquez, P., et al. 2023, A&A, 673, A147

    2023

  87. [95]

    2020, MNRAS, 495, 3387

    Peterken, T., Merrifield, M., Aragón-Salamanca, A., et al. 2020, MNRAS, 495, 3387

    2020

  88. [96]

    & Pagel, B

    Pettini, M. & Pagel, B. E. J. 2004, MNRAS, 348, L59

    2004

  89. [97]

    S., Zinchenko, I

    Pilyugin, L. S., Zinchenko, I. A., Lara-López, M. A., Nefedyev, Y . A., & Vílchez, J. M. 2021, A&A, 646, A54

    2021

  90. [98]

    R., Bell, E

    Robaina, A. R., Bell, E. F., Skelton, R. E., et al. 2009, ApJ, 704, 324

    2009

  91. [99]

    F., Díaz, A

    Rosales-Ortega, F. F., Díaz, A. I., Kennicutt, R. C., & Sánchez, S. F. 2011, MN- RAS, 415, 2439

    2011

  92. [100]

    2017, A&A, 604, A4

    Ruiz-Lara, T., Pérez, I., Florido, E., et al. 2017, A&A, 604, A4

    2017

  93. [101]

    Rupke, D. S. N., Kewley, L. J., & Chien, L.-H. 2010, ApJ, 723, 1255 Sánchez, S. F. 2020, ARA&A, 58, 99 Sánchez, S. F., García-Benito, R., Zibetti, S., et al. 2016, A&A, 594, A36 Sánchez, S. F., Lugo-Aranda, A. Z., Sánchez Almeida, J., et al. 2024, A&A, 682, A71 Sánchez, S. F.,...

    2010

  94. [102]

    2022, A&A, 658, A188

    Santoro, F., Kreckel, K., Belfiore, F., et al. 2022, A&A, 658, A188

    2022

  95. [103]

    & Bildsten, L

    Scannapieco, E. & Bildsten, L. 2005, ApJ, 629, L85

    2005

  96. [104]

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

    2011

  97. [105]

    A., Kartaltepe, J

    Shah, E. A., Kartaltepe, J. S., Magagnoli, C. T., et al. 2022, ApJ, 940, 4

    2022

  98. [106]

    2013, A&A, 558, A43

    Singh, R., van de Ven, G., Jahnke, K., et al. 2013, A&A, 558, A43

    2013

  99. [107]

    T., Lilly, S

    Soto, K. T., Lilly, S. J., Bacon, R., Richard, J., & Conseil, S. 2016, MNRAS, 458, 3210 Stasi´nska, G., Vale Asari, N., Cid Fernandes, R., et al. 2008, MNRAS, 391, L29

    2016

  100. [108]

    J., et al

    Sullivan, M., Le Borgne, D., Pritchet, C. J., et al. 2006, ApJ, 648, 868

    2006

  101. [109]

    B., Sillero, E., et al

    Tapia-Contreras, B., Tissera, P. B., Sillero, E., et al. 2025, A&A, 700, A69

    2025

  102. [110]

    B., Machado, R

    Tissera, P. B., Machado, R. E. G., Sanchez-Blazquez, P., et al. 2016, A&A, 592, A93

    2016

  103. [111]

    Tsai, C.-W., Eisenhardt, P. R. M., Jun, H. D., et al. 2018, ApJ, 868, 15

    2018

  104. [112]

    Tsai, C.-W., Eisenhardt, P. R. M., Wu, J., et al. 2015, ApJ, 805, 90 Übler, H., Maiolino, R., Curtis-Lake, E., et al. 2023, A&A, 677, A145 Valé, G., Lara-López, M. A., Valerdi, M., et al. 2025, A&A, 701, A226 van de Sande, J., Bland-Hawthorn, J., Fogarty, L. M. R., et al. 2017...

    2015

  105. [113]

    2016, MNRAS, 463, 3409

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

    2016

  106. [114]

    & Osterbrock, D

    Veilleux, S. & Osterbrock, D. E. 1987, ApJS, 63, 295

    1987

  107. [115]

    2017, Frontiers in Astronomy and Space Sciences, 4, 46

    Venturi, G., Marconi, A., Mingozzi, M., et al. 2017, Frontiers in Astronomy and Space Sciences, 4, 46

    2017

  108. [116]

    & Lilly, S

    Wang, E. & Lilly, S. J. 2022, ApJ, 929, 95

    2022

  109. [117]

    M., Streicher, O., Urrutia, T., et al

    Weilbacher, P. M., Streicher, O., Urrutia, T., et al. 2012, in Proc. SPIE, V ol. 8451, Software and Cyberinfrastructure for Astronomy II, 84510B

    2012

  110. [118]

    2012, ApJ, 756, 96

    Wu, J., Tsai, C.-W., Sayers, J., et al. 2012, ApJ, 756, 96

    2012

  111. [119]

    2019, MNRAS, 486, 4463

    Yu, X., Shi, Y ., Chen, Y ., et al. 2019, MNRAS, 486, 4463

    2019

  112. [120]

    C., & Huchra, J

    Zaritsky, D., Kennicutt, Jr., R. C., & Huchra, J. P. 1994, ApJ, 420, 87 Article number, page 14

    1994

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