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REVIEW 3 major objections 6 minor 49 references

Discovery of a kinematically distinct component in the central region of the collisional ring galaxy AM0644-741

T0 review · 3 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read The center of ring galaxy AM0644-741 holds a rotating stellar component that survived the collision that made its ring.

desk verdict Plausible but not yet proven: the two-component photometric decomposition is solid, but the kinematic distinctness of the inner component needs a PSF/AGN contamination test. read the letter →

arxiv 2505.21352 v1 pith:KOFL4ULZ submitted 2025-05-27 astro-ph.GA

Chayan Mondal , Sudhanshu Barway This is my paper
classification astro-ph.GA
keywords collisionalringgalaxyAM0644-741stellarkinematicsintegralfieldspectroscopySersicdecompositiongalacticstructureAGNLINER
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

Using HST imaging and MUSE integral-field spectroscopy, the authors find that the center of the collisional ring galaxy AM0644-741 hosts two distinct stellar components: a compact rotating inner structure and an outer exponential disk whose position angle differs by about 60 degrees. The inner component, with an effective radius of about 1 kpc, shows the kinematic signature of rotation (a strong anticorrelation between V_LOS/sigma_LOS and h3), disky isophotes, elevated velocity dispersion up to roughly 240 km/s, and a strong Mg b line index. The authors argue that this is a pre-collisional rotating structure that survived the encounter 133 Myr ago, while the outer disk was disrupted to form the star-forming ring. If correct, this means the recent collision had a smaller dynamical effect on the central stellar orbits than on the outer disk, and it makes AM0644-741 a test case for how fly-by encounters reshape galaxies from the outside in.

What carries the argument

The analysis combines two tools: (1) two-component Sersic photometric decomposition with an unresolved point source for the AGN via Galfit, which establishes the photometric distinctness and the ~60 degree position-angle twist; (2) stellar line-of-sight velocity distribution fitting with the pPXF/GIST pipeline on Voronoi-binned MUSE spectra, which produces V_LOS, sigma_LOS, h3, h4 maps and stellar population ages. The load-bearing diagnostic is the V_LOS/sigma_LOS versus h3 anticorrelation within the inner component, a standard kinematic signature of a rotation-supported disk; the authors combine it with b4 isophote shapes and Mg b line strength to argue for a dynamically hot but still rotationally supported pre-collisional structure.

What would settle it

Re-extract the MUSE kinematics after subtracting a PSF-scaled image of the nuclear source (or obtain adaptive-optics IFU data with ~0.2 arcsec resolution) and check whether the V_LOS/sigma_LOS–h3 anticorrelation and the velocity dispersion peak inside 2 arcsec persist; if they vanish, the central rotating component is an artifact of the AGN point-spread function.

Watch

Extended reading notes

Core claim

The paper's central discovery is a kinematically distinct stellar component in the central ~1 kpc of AM0644-741, identified through two-component Sersic decomposition of the HST F814W image and stellar line-of-sight kinematics from MUSE. The inner component (Sersic index 1.72, effective radius 2.19 arcsec = 0.97 kpc) is misaligned with the outer disk (index 1.11, re = 4.44 kpc) by about 60 degrees in position angle. Within the inner component, the authors measure a Spearman anticorrelation of -0.75 between V_LOS/sigma_LOS and h3, a signature of near-circular stellar orbits, along with central velocity dispersion peaks reaching ~240 km/s and positive b4 isophotes indicating disky shapes. They interpret this combination as a pre-collisional compact stellar disk that has retained its rotation and been dynamically heated, while the outer disk's orbits were more strongly disturbed in the ring-forming collision. The nuclear spectrum shows LINER-type ionization, consistent with an AGN whose activity may have been triggered or enhanced by the encounter.

Load-bearing premise

The load-bearing premise is that the inner component's photometric and kinematic signature survives the subtraction of the unresolved nuclear source and the seeing-limited resolution of the MUSE data; if the point-spread-function model is imperfect, the measured rotation and high dispersion could come from the AGN point source or beam smearing rather than from a separate stellar structure.

Editorial extensions

If this is right

  • If the central component is truly pre-collisional, then the collision did not destroy the innermost disk of the progenitor; only the outer disk was strongly perturbed, constraining the impact parameter and the coupling of the intruder's tidal field to stellar orbits.
  • The ~60 degree position-angle twist between photometric and kinematic axes inside and outside the inner component provides a direct measure of how a ring-forming encounter misaligns an outer disk relative to the inner disk.
  • The elevated central velocity dispersion (up to ~240 km/s) along with rotation implies that dynamical heating and a possible pseudo-bulge or compact bulge can form in the center of a collisional ring galaxy without merging.
  • The LINER-type nuclear ionization suggests that AGN activity can be present in ring galaxies and may be triggered by the encounter, making AM0644-741 a candidate for studying AGN fueling in collisional systems.
  • The mass-weighted age of ~11 Gyr for the inner component indicates that the surviving disk formed long before the encounter, making it an old, quiescent stellar structure within an actively star-forming ring.

Reading between the lines

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

  • If the decomposition is correct, the inner component's high velocity dispersion and rotation could make it an example of a 'hot disk' that may be an evolutionary precursor to a classical bulge, a connection worth testing with detailed simulations of impulsive tidal heating.
  • The finding that the inner disk survives while the outer disk is disrupted suggests that in off-center collisions, the angular momentum and orbital structure of the inner disk are shielded; this may generalize to other collisional ring galaxies and could be tested by comparing the central kinematics of the Cartwheel, AM0644-741, and Bullseye.
  • The strong dependence on PSF modeling suggests that a targeted high-spatial-resolution IFU observation (e.g., with adaptive optics) could verify the rotation signature inside 1 kpc and separate it cleanly from AGN contamination.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. This Letter reports a two-component photometric decomposition and MUSE stellar kinematics for the central region of the collisional ring galaxy AM0644-741. Using Galfit on the HST F814W image, the authors identify an inner Sérsic component (re ~ 0.97 kpc, n = 1.72) and an outer disk-like component (re ~ 4.4 kpc, n = 1.11) with a ~60 degree difference in position angle, plus an unresolved nuclear point source. MUSE/GIST kinematic maps show coherent rotation in V_LOS/sigma_LOS, a central velocity-dispersion peak reaching ~200-260 km/s, an h3 versus V_LOS/sigma_LOS anticorrelation (Spearman coefficient -0.75) within the inner component, disky isophotes, and a strong Mg b line index. The authors interpret the inner component as a pre-collisional rotating stellar structure that survived a ~133 Myr old encounter, while the outer disk was more strongly affected; they also report LINER-type ionization and hint at an AGN in the nucleus.

Significance. If the central kinematic claim holds, this is a valuable observational constraint on the survival of inner stellar disks in collisional ring galaxies and a useful complement to the Cartwheel bar studies. The paper is methodologically transparent: it uses public HST and MUSE data, standard tools (Galfit, GIST, pPXF, Voronoi binning), and provides appendices on isophotal shape, inclination effects, stellar-population ages, and BPT diagnostics. The main weakness is that the kinematic evidence for the inner component is derived at angular scales only about two times the MUSE seeing, in a region that also contains an unresolved LINER/AGN source. Because the paper does not yet quantify the AGN continuum contribution or test PSF/beam-smearing effects, the unique identification of a distinct rotating stellar component is not yet fully established.

major comments (3)
  1. [§3.2, Figures 3 and 4; Table 1] The inner-component kinematics are measured at scales comparable to the MUSE seeing: the inner component has re = 2.19 arcsec while the seeing is reported as 1.16 arcsec. The same region contains an unresolved nuclear source classified as LINER in Appendix D and detected as an X-ray point source by Wolter et al. (2019). The paper does not quantify the AGN continuum fraction in the 4800-5800 Å fitting window, does not mask or explicitly model the nucleus in the pPXF fits, and does not test the effect of PSF smoothing on the Voronoi-binned maps. Beam smearing across a steep central velocity gradient can broaden the measured LOSVD and can in principle produce an h3-V/sigma correlation that mimics a rotating disk. Because the V/sigma-h3 anticorrelation (-0.75) and the high central dispersion are the main kinematic evidence for a distinct rotating component, control tests are needed: masked-nucleus fits, PSF-convolved signal-injection simulations based on the Galfit model, and an estimate of the AGN continuum fraction in the fitting window.
  2. [§3.2 and Figure 4] The strength of the rotation signature is quantified by a Spearman correlation computed from all spaxels inside the photometric inner-component ellipse, but the effective number of independent resolution elements across that component is small (re ~ 2.19 arcsec against a seeing of 1.16 arcsec), and Voronoi binning to S/N = 30 introduces strong spatial correlations between adjacent bins. The paper does not report an effective sample size, a bootstrap estimate, or a spatially conservative significance test. The reported coefficient -0.75 therefore overstates the statistical robustness of the anticorrelation as presented. A bootstrap over Voronoi bins or an analysis on a coarser independent grid would give a more defensible significance.
  3. [§4.1 and Appendix C] The conclusion that the inner structure is pre-collisional relies on mass-weighted stellar ages of ~11 Gyr, but no formal uncertainties are given for the age estimates, and the adopted regularization parameter (REGUL_ERR = 0.15) is presented without a clear quantitative justification. This point is not fatal because the collision age is only ~133 Myr, so even large age errors would not change the qualitative conclusion; however, the age map should be shown for all tested regularization values with error bars, and the text should not present the ages as tightly constrained without a stated uncertainty.
minor comments (6)
  1. [Abstract and text] There are typographical artifacts throughout the manuscript (e.g., 'G alfit', 'di fference', 'V oronoi'); a careful proofread is needed.
  2. [Table 1] Table 1 lists the Galfit parameters without uncertainties; please add formal fit errors or a sensitivity test (for example, varying the nuclear PSF magnitude) to demonstrate that the two-Sérsic + PSF decomposition is not degenerate.
  3. [§3.2 and Figure 4] The pseudo-slit used for the radial V/sigma and sigma profiles is not fully described; please specify the slit width and how the profiles were extracted and binned.
  4. [Appendix D and Figure D.1] The LINER classification in the BPT diagram relies on an upper limit for the [O III]/H-beta ratio because H-beta is not detected; the text and figure caption should state clearly that the classification is based on a limit rather than a measured line ratio, and the method used to derive the upper limit should be described.
  5. [§4.2 and Figure D.1] The Mg b line index is reported as 4.9 Å without an uncertainty or the adopted Lick-style bandpass definitions; please provide the bandpasses and an error estimate.
  6. [Appendix C] The dependence of the stellar age map on the regularization parameter is shown only as a shaded envelope in one profile panel; please provide the age maps for the tested REGUL_ERR values (0.10, 0.15, 0.30, 0.45) or otherwise quantify the pixel-to-pixel scatter and justify the adopted value.

Circularity Check

0 steps flagged · score 2.0 of 10

No material circularity: the central result is an observational characterization, and the few self-citations serve only as external benchmarks.

full rationale

The paper's derivation chain is photometric decomposition with Galfit on HST F814W imaging followed by independent MUSE stellar kinematics extracted with pPXF via the GIST pipeline. The central claim, that AM0644-741 hosts a kinematically distinct inner stellar component, rests on directly measured quantities: the VLOS/sigmaLOS versus h3 anticorrelation (Spearman coefficient -0.75), the sigmaLOS central peak near 240 km/s, the positive b4 isophotes, the ~60 degree position-angle shift, and the mass-weighted age of about 11 Gyr. None of these quantities is defined in terms of the conclusion; they are measurements on the data, and the region labelled 'inner component' comes from the HST fit while the kinematic maps come from the separate MUSE data cube. The comparison with the Cartwheel galaxy uses the authors' earlier work (Mondal & Barway 2024) only as a benchmark value, and Barway et al. (2020) is cited only for context; neither citation is load-bearing for the discovery claim. The seeing-limited effective radius and the unresolved AGN are potential systematic errors in the measurement, but they concern correctness rather than circularity. The minor, non-load-bearing self-citations justify a low score of 2 rather than 0.

Assumptions & free parameters 12 free parameters · 5 assumptions · 0 invented entities

The central claim depends on a set of Galfit-fitted structural parameters, the assumption that archival data are calibrated, and the reliability of pPXF kinematics and stellar population ages. No new physical entities are introduced; the inner component is a decomposition of observed light. The main unvalidated inputs are the PSF model, the template set, and the H-beta upper-limit BPT classification.

free parameters (12)
  • Inner Sérsic magnitude = 14.15 mag
    Fitted by Galfit to the HST F814W image; defines the brightness of the inner component and enters the decomposition.
  • Inner Sérsic effective radius = 2.19 arcsec (0.97 kpc)
    Fitted; sets the spatial scale over which the inner component kinematics are measured.
  • Inner Sérsic index = 1.72
    Fitted; used to describe the inner component as bulge-like.
  • Inner Sérsic axis ratio = 0.71
    Fitted; used in the projected shape and inclination discussion.
  • Inner Sérsic PA = 33.4 deg
    Fitted; the 60-degree offset from the outer component PA is a central piece of evidence for two distinct components.
  • Outer Sérsic magnitude = 12.97 mag
    Fitted; defines the outer disk component.
  • Outer Sérsic effective radius = 9.98 arcsec (4.44 kpc)
    Fitted; extent of the outer disk.
  • Outer Sérsic index = 1.11
    Fitted; close to exponential disk.
  • Outer Sérsic axis ratio = 0.65
    Fitted.
  • Outer Sérsic PA = -26.5 deg
    Fitted; used for the 60-degree offset and inclination estimates.
  • PSF magnitude = 19.29 mag
    Fitted; represents the unresolved nuclear source; uncertainties here could affect the inner component parameters.
  • Regularization error for age fitting = REGUL_ERR = 0.15
    Chosen by hand for the stellar population age fitting; the paper checks four values (0.10, 0.15, 0.30, 0.45).
assumptions (5)
  • domain assumption The archival HST and MUSE data are correctly reduced and aligned.
    The analysis uses public data without independent calibration or astrometric verification.
  • domain assumption A two-Sersic plus point-source model adequately represents the central light distribution of AM0644-741.
    Galfit residuals show dust lanes and a filamentary structure; the model is assumed to separate real components rather than overfit the dust.
  • domain assumption pPXF stellar kinematics with MILES templates are unbiased despite AGN emission and dust.
    The nuclear source is photometrically modeled as a PSF, but the MUSE spectra in the inner region are not corrected for AGN continuum or emission lines before fitting the stellar absorption features.
  • domain assumption The stellar population ages derived with regularized pPXF are reliable and not strongly affected by age-metallicity degeneracy.
    Ages of about 11 Gyr are used to argue for a pre-collisional origin; the paper tests regularization strength but not other systematic effects such as template mismatch or AGN contamination.
  • domain assumption The BPT classification based on an upper limit for H-beta robustly identifies a LINER.
    Since H-beta is not detected, the [OIII]/H-beta ratio is an upper limit, so the position in the BPT diagram is not fully constrained; the paper treats this as a hint rather than a definitive measurement.

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Pith. "Pith review of Discovery of a kinematically distinct component in the central region of the collisional ring galaxy AM0644-741." pith.science (2026). https://pith.science/paper/KOFL4ULZ

@misc{pith2026250521352,
  author       = {Pith},
  title        = {Pith review of: Discovery of a kinematically distinct component in the central region of the collisional ring galaxy AM0644-741},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/KOFL4ULZ}},
  note         = {Machine review of arXiv:2505.21352}
}
abstract

We present the discovery of a peculiar central stellar structure in the collisional ring galaxy AM0644-741 using HST imaging and MUSE integral field unit (IFU) data. We identified two S\'ersic components with a S\'ersic index of 1.72 (inner part) and 1.11 (outer part) in the HST F814W band optical image using \textsc{Galfit}. We utilized the MUSE data cube to construct stellar line of sight velocity (V$_{\rm LOS}$), velocity dispersion ($\sigma_{\rm LOS}$), h$_3$ \& h$_4$ velocity moments, and stellar population age maps using the \textsc{GIST} pipeline for further investigating both S\'ersic components, which have a difference of $\sim$ 60 degrees in their position angle. The inner component, with an effective radius $\sim$1 kpc, shows a strong anticorrelation between V$_{\rm LOS}$/$\sigma_{\rm LOS}$ and h$_3$, indicating the presence of a rotating stellar structure. In addition, the inner component also shows a relatively higher velocity dispersion (average values reaching up to $\sim$240 km sec$^{-1}$) along with disky isophotes and stronger Mg~$b$ line strength, which all together highlight a peculiar dynamical state of AM0644-741's central region. Our analysis suggests that the recent encounter has had a smaller impact on the stellar orbits within the inner component. In contrast, it has specifically affected the stellar orbits of the progenitor's outer disk when forming the star-forming ring. The BPT analysis of the unresolved nuclear source shows a LINER-type ionization, hinting at AGN activity in the galaxy. Our study projects the dynamical evolution of collisional systems and provides scope for simulations to explore the central region in greater detail.

Figures

Figures reproduced from arXiv: 2505.21352 by the authors.

Figure 2
Figure 2. Surface brightness profiles derived using the IRAF ELLIPSE task from the HST F814W band observed and Galfit model images. The black points denote the values derived from the observed image, whereas the profiles for the inner Sérsic, outer Sérsic, and the combined model are shown in red dashed, blue dashed, and black solid lines, re￾spectively. In the inset, we show the HST image and the extent of both components in … view at source ↗
Figure 3
Figure 3. Stellar kinematic maps of AM0644-741 derived from the MUSE IFU data using the GIST pipeline. The figure shows stellar VLOS/σLOS (left), velocity dispersion (σLOS) (middle), and h3 velocity moment (right) maps of the inner part (i.e., region within the blue rectangle shown in [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. VLOS/σLOS (left) and LOS velocity dispersion (middle) profiles, measured along the pseudo slit shown in [PITH_FULL_IMAGE:figures/full_fig_p004_4.png] view at source ↗

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Works this paper leans on

49 extracted references · 34 canonical work pages

  1. [1]

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

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

  2. [2]

    write newline

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

  3. [3]

    & Wallin , J

    Antunes , A. & Wallin , J. 2007, , 670, 261

    work page 2007

  4. [4]

    Appleton , P. N. & Marston , A. P. 1997, , 113, 201

    work page 1997

  5. [5]

    Appleton , P. N. & Struck-Marcell , C. 1996, , 16, 111

    work page 1996

  6. [6]

    Arp , H. C. & Madore , B. 1987, A catalogue of southern peculiar galaxies and associations

    work page 1987

  7. [7]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, , 156, 123

    2018

  8. [8]

    P., Tollerud , E

    Astropy Collaboration , Robitaille , T. P., Tollerud , E. J., et al. 2013, , 558, A33

    2013

Show all 49 references
  1. [9]

    1997, , 286, 284

    Athanassoula , E., Puerari , I., & Bosma , A. 1997, , 286, 284

    1997

  2. [10]

    2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Bacon , R., Accardo , M., Adjali , L., et al. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 7735, Ground-based and Airborne Instrumentation for Astronomy III, ed. I. S. McLean , S. K. Ramsay , & H. Takami , 773508

    2010

  3. [11]

    D., & Robleto-Or \'u s , A

    Barway , S., Mayya , Y. D., & Robleto-Or \'u s , A. 2020, , 497, 44

    2020

  4. [12]

    P., & Gerhard , O

    Bender , R., Saglia , R. P., & Gerhard , O. E. 1994, , 269, 785

    1994

  5. [13]

    A., et al

    Bittner , A., de Lorenzo-C \'a ceres , A., Gadotti , D. A., et al. 2021, , 646, A42

    2021

  6. [14]

    2019, , 628, A117

    Bittner , A., Falc \'o n-Barroso , J., Nedelchev , B., et al. 2019, , 628, A117

    2019

  7. [15]

    V., Moiseev , A

    Bizyaev , D. V., Moiseev , A. V., & Vorobyov , E. I. 2007, , 662, 304

    2007

  8. [16]

    2017, , 466, 798

    Cappellari , M. 2017, , 466, 798

    2017

  9. [17]

    & Copin , Y

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

    2003

  10. [18]

    & Emsellem , E

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

    2004

  11. [19]

    1987, , 313, 42

    Dressler , A., Lynden-Bell , D., Burstein , D., et al. 1987, , 313, 42

    1987

  12. [20]

    Elagali , A., Lagos , C. D. P., Wong , O. I., et al. 2018 a , , 481, 2951

    2018

  13. [21]

    Elagali , A., Lagos , C. D. P., Wong , O. I., et al. 2018 b , , 481, 2951

    2018

  14. [22]

    Few , J. M. A., Madore , B. F., & Arp , H. C. 1982, , 199, 633

    1982

  15. [23]

    Fisher , D. B. & Drory , N. 2016, in Astrophysics and Space Science Library, Vol. 418, Galactic Bulges, ed. E. Laurikainen , R. Peletier , & D. Gadotti , 41

    2016

  16. [24]

    A., Bittner , A., Falc \'o n-Barroso , J., et al

    Gadotti , D. A., Bittner , A., Falc \'o n-Barroso , J., et al. 2020, , 643, A14

    2020

  17. [25]

    L., Higdon , S

    Higdon , J. L., Higdon , S. J. U., & Rand , R. J. 2011, , 739, 97

    2011

  18. [26]

    Higdon , J. L. & Wallin , J. F. 1997, , 474, 686

    1997

  19. [27]

    1995, , 298, 743

    Horellou , C., Casoli , F., Combes , F., & Dupraz , C. 1995, , 298, 743

    1995

  20. [28]

    Hunter, J. D. 2007, Computing In Science & Engineering, 9, 90

    2007

  21. [29]

    Jedrzejewski , R. I. 1987, , 226, 747

    1987

  22. [30]

    Joye , W. A. & Mandel , E. 2003, in Astronomical Society of the Pacific Conference Series, Vol. 295, Astronomical Data Analysis Software and Systems XII, ed. H. E. Payne , R. I. Jedrzejewski , & R. N. Hook , 489

    2003

  23. [31]

    M., Tremonti , C., et al

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

    2003

  24. [32]

    J., Dopita , M

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

    2001

  25. [33]

    D., & Vorobyov , E

    Korchagin , V., Mayya , Y. D., & Vorobyov , E. 2001, , 554, 281

    2001

  26. [34]

    2006, , 369, 497

    Kuntschner , H., Emsellem , E., Bacon , R., et al. 2006, , 369, 497

    2006

  27. [35]

    & Toomre , A

    Lynds , R. & Toomre , A. 1976, , 209, 382

    1976

  28. [36]

    M., Appleton , P

    Marcum , P. M., Appleton , P. N., & Higdon , J. L. 1992, , 399, 57

    1992

  29. [37]

    Marston , A. P. & Appleton , P. N. 1995, , 109, 1002

    1995

  30. [38]

    Mogotsi , K. M. & Romeo , A. B. 2019, , 489, 3797

    2019

  31. [39]

    & Barway , S

    Mondal , C. & Barway , S. 2024, , 681, A53

    2024

  32. [40]

    2020, , 495, 4638

    Oh , S., Colless , M., Barsanti , S., et al. 2020, , 495, 4638

    2020

  33. [41]

    G., Liu , Q., et al

    Pasha , I., van Dokkum , P. G., Liu , Q., et al. 2025, , 980, L3

    2025

  34. [42]

    Y., Ho , L

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

    2002

  35. [43]

    2018, , 473, 585

    Renaud , F., Athanassoula , E., Amram , P., et al. 2018, , 473, 585

    2018

  36. [44]

    D., & Vorobyov , E

    Romano , R., Mayya , Y. D., & Vorobyov , E. I. 2008, , 136, 1259

    2008

  37. [45]

    2007, , 382, 1415

    Schawinski , K., Thomas , D., Sarzi , M., et al. 2007, , 382, 1415

    2007

  38. [46]

    Theys , J. C. & Spiegel , E. A. 1976, , 208, 650

    1976

  39. [47]

    2010, , 404, 1639

    Vazdekis , A., S \'a nchez-Bl \'a zquez , P., Falc \'o n-Barroso , J., et al. 2010, , 404, 1639

    2010

  40. [48]

    2019, IAU Symposium, 346, 297

    Wolter , A., Consolandi , G., Longhetti , M., Landoni , M., & Bianco , A. 2019, IAU Symposium, 346, 297

    2019

  41. [49]

    Ziegler , B. L. & Bender , R. 1997, , 291, 527

    1997

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