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Evidence for Mass-dependent Evolution of Transitional Dwarf Galaxies in the Virgo Cluster

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read The paper argues that low-mass dwarf lenticular galaxies in the Virgo cluster are rapidly transformed into dwarf ellipticals by ram-pressure stripping, while more massive dS0s keep their morphologies even in the cluster center.

desk verdict A solid, non-circular census of Virgo transitional dwarfs that makes a plausible mass-dependent transformation case, but the visual dS0/dE classification needs completeness testing before the central claim is secure. read the letter →

arxiv 2411.17086 v1 pith:3D3RXGG5 submitted 2024-11-26 astro-ph.GA

Suk Kim , Soo-Chang Rey , Youngdae Lee This is my paper · ORCID
classification astro-ph.GA
keywords dwarfgalaxiesVirgoclusterlenticularsmorphologicaltransformationrampressurestrippingprojectedphase-spacediagramstellarmassdependenceearly-type
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper argues that transitional dwarf galaxies in the Virgo cluster evolve along a mass-dependent path: faint, low-mass dwarf lenticulars (dS0s) are quickly transformed into dwarf ellipticals (dEs) by environmental effects, whereas massive dS0s retain their disk-like substructures even in the cluster center. The authors use the Extended Virgo Cluster Catalog to compare dS0s, blue-cored early-type dwarfs, dEs, and dwarf irregulars by clustercentric distance, stellar mass, and projected phase-space location. If correct, environmental quenching and morphological transformation in clusters proceed on different timescales depending on dwarf galaxy mass, with low-mass dwarfs changing morphology quickly after infall and massive dwarfs surviving as recognizable remnants. The paper also identifies blue-cored early-type dwarfs as a recently accreted population that has not yet become passive dEs.

What carries the argument

The central objects are dwarf lenticulars (dS0s), transitional dwarfs with smooth overall light plus hidden substructures such as disks, bars, and spiral arms, and early-type dwarfs with blue cores (ETdG(bc)s). The key machinery is the projected phase-space diagram, which maps clustercentric distance and line-of-sight velocity onto orbital stages (recently infalled, stripped, and virialized), combined with EVCC morphological classifications and stellar masses from SDSS colors. This diagram carries the argument by showing where each dwarf type sits relative to the ram-pressure stripping boundary: the stripped region is almost devoid of dS0s but full of dEs, whereas the virialized region contains dS0s that are predominantly bright and massive.

What would settle it

A deep, high-resolution imaging survey of the Virgo core that can resolve low-surface-brightness disks, bars, and spiral arms in galaxies fainter than about M_r = -16 would settle the claim: if many faint dS0s are found among galaxies currently classified as dEs in the stripped region, the mass-dependent transformation is an artifact of classification limits, whereas if the deficit of faint dS0s persists with such data, the claim is supported.

Watch

Extended reading notes

Core claim

The central claim is that the morphological transformation of dwarf galaxies in the Virgo cluster depends on stellar mass: low-mass dS0s are highly susceptible to environmental effects and rapidly become dEs, while higher-mass dS0s retain their morphology because their gravitational potential resists stripping, even in the cluster center. The evidence is that dS0s in the mass-clustercentric distance plane are systematically more massive than dEs at a given projected radius; dS0s are scarce in the stripped region of the projected phase-space diagram but dominate the bright and massive population in the virialized region; faint dS0s are absent where faint dEs are abundant; and ETdG(bc)s follow the distributions of late-type and dwarf irregular galaxies while being absent from the stripped and virialized regions, marking them as recently accreted objects.

Load-bearing premise

The analysis assumes that the EVCC morphological classification is complete and unbiased with clustercentric distance and stellar mass, especially the distinction between faint dS0s and dEs, so that the apparent scarcity of faint dS0s in the cluster core reflects real transformation rather than misclassification.

Editorial extensions

If this is right

  • Low-mass dS0s entering the Virgo cluster are transformed into dEs during their first passage through the dense intracluster medium, explaining the deficit of faint dS0s in the stripped region.
  • Massive dS0s can survive into the virialized region, retaining disk-like substructures for several gigayears after their star formation has been quenched.
  • ETdG(bc)s represent a recently accreted population; once they enter the stripped or virialized regions, they are expected to evolve into passive dEs.
  • Morphological transformation lags behind star-formation quenching: bright, massive dS0s are already quiescent but still show the substructures that will eventually be erased.
  • The Extended Virgo Cluster Catalog reveals morphology-clustercentric distance relations that extend beyond the virial radius and are stronger than those seen in the classical VCC.

Reading between the lines

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

  • If this mass-dependent transformation is general, then other clusters at different dynamical stages should show a similar pattern: the median stellar mass of dS0s relative to dEs in the virialized region should scale with the cluster's velocity dispersion or intracluster medium density.
  • The argument predicts that deep surface-brightness imaging of Virgo's core should uncover a population of red, massive, disky dwarfs that shallow surveys would classify as dEs; counting such objects would directly test the classification-based interpretation.
  • The two-population split between settled dS0s and recently accreted ETdG(bc)s implies that dS0s in the virialized region should have older stellar populations and lower gas content than ETdG(bc)s at the same clustercentric distance, a prediction testable with resolved spectroscopy and HI observations.
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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 / 5 minor

Summary. This paper uses the Extended Virgo Cluster Catalog (EVCC) to study the spatial distribution, stellar masses, and projected phase-space positions of transitional dwarf galaxies (dS0s and ETdG(bc)s) in the Virgo cluster, comparing them to dwarf ellipticals (dEs) and dwarf irregulars (dIrrs). The authors find that dS0s beyond 0.7 Rvir follow a decreasing fraction with clustercentric distance similar to dEs, while ETdG(bc)s show an opposite trend. They also report that dS0s are systematically more massive than dEs at a given clustercentric distance, that dS0s are scarce in the ram-pressure-stripped region of the projected phase-space diagram, and that the dS0s in the virialized region are brighter and more massive than dEs. From these observations they conclude that low-mass dS0s are rapidly transformed into dEs by environmental effects, while massive dS0s can retain their morphology even in the cluster center.

Significance. If the central claim holds, this would provide one of the clearest observational indications that morphological transformation of dwarf galaxies in clusters is mass-dependent, with low-mass dS0s evolving into dEs on short timescales after infall and massive dS0s surviving into the virialized region. The paper's strengths include the use of the larger EVCC sample extending beyond the classical VCC, the combination of spatial, mass, color, and phase-space diagnostics, and the explicit caution about small-number statistics beyond 13 degrees. The analysis is not circular: morphological classes, stellar masses, and phase-space boundaries are taken from external catalogs and published prescriptions. However, the central inference rests on an untested completeness assumption for the dS0/dE classification with respect to stellar mass, and several quantitative claims (notably the '60% of enhancement' number) are presented without uncertainties or fit parameters.

major comments (3)
  1. [Section 2; Section 5] The central claim of Section 5 is that low-mass dS0s are transformed into dEs while massive dS0s survive, and this rests on the dS0/dE morphological distinction being complete and unbiased with stellar mass at fixed clustercentric distance. Section 2 shows that dS0s are identified by low-surface-brightness substructures (bar, disk, spiral arms) in DECaLS residual images, and the paper quantifies one-way reclassification of 44 VCC dEs as dS0s, but it does not test the inverse completeness: how many faint dS0s might be misclassified as dEs because their substructures fall below the detection threshold at fainter magnitudes? Because the observed signatures (scarcity of faint dS0s in the stripped and virialized regions, Figure 6; mass skew in Figure 4) would be produced if such a bias exists, the authors should provide a completeness test as a function of stellar mass (e.g., adding synthetic substructures to dE images and checking recovery, or comparing a subsample with deeper HST/Subaru imaging). Without such a test, the central inference is not secure.
  2. [Section 3.2, Figure 3] The linear least-square fits to the dE and dS0 fractions beyond 3.5 degrees are shown as black lines in Figure 3, but no fit parameters, uncertainties, or goodness-of-fit values are reported. The statement that 'the observed numbers of dEs and dS0s in the central region are about 30 more and 17 less, respectively, than what would be expected' and the resulting 'about 60% of the enhancement' are extrapolations of these fits; with Poisson uncertainties on counts of roughly sqrt(30)~5 and sqrt(17)~4, the ratio has a large uncertainty (roughly 60% +/- 30% before including fit errors). Please show error bars on the binned fractions, report the fit parameters with uncertainties, and propagate them into the 60% claim.
  3. [Section 3.5, Figure 5] The red solid curve delimiting the stripped region is computed for a galaxy with a stellar mass of ~10^8 M_sun (following Jaffe et al. 2015), and the virialized region is defined by fixed r < Rvir and |dv| < 1.5 sigma. The paper uses these single boundaries for galaxies spanning stellar masses from roughly 10^7 to 10^9 M_sun, and the conclusion that dS0s are scarce in the stripped region while dEs are abundant is sensitive to where each galaxy falls relative to the curve. Please either compute the stripping boundary for a range of stellar masses (e.g., 10^7, 10^8, 10^9 M_sun) and show how the region classification changes, or provide a robustness test demonstrating that the main conclusions are unchanged when the boundary is varied within a plausible mass range.
minor comments (5)
  1. [Section 3.1] The two-dimensional KS test p-values are reported without the corresponding sample sizes or test statistics; adding these would make the comparisons more informative.
  2. [Figure 2] There is a minor inconsistency between the text ('dIrrs, green circles') and the Figure 2 caption ('dIrrs (green crosses)') for panel (c); please unify the symbol description.
  3. [Section 3.4] The statement that the FUV-r colors of dS0s depend on clustercentric distance is descriptive; a quantitative comparison (e.g., median FUV-r color in radial bins with uncertainties) would strengthen the CMD analysis.
  4. [Section 3.2] The paper flags the fractions beyond ~13 degrees as unreliable due to small numbers; consider moving this caveat directly into the relevant figure panels or reducing the radial range over which the running averages are shown.
  5. [Section 4] When discussing the timescale of morphological transformation versus quenching, the paper cites 'a few Gyr' without a precise comparison for Virgo; a quantitative estimate based on the cluster crossing time would help.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the mass-dependent dS0-to-dE interpretation is an observational comparison against external catalogs and prescriptions, not a reduction to its own inputs.

full rationale

The paper's derivation chain is empirical rather than definitional. Morphological classifications come from the EVCC (Kim et al. 2014, which shares authors with the present paper), but the EVCC is a pre-existing catalog based on visual inspection of SDSS and DECaLS images, not a parameter fitted to the mass-clustercentric or phase-space relations that the paper explains. Stellar masses use the external Bell et al. (2003) color-to-mass relation with a Kroupa IMF; cluster parameters (distance, Rvir, velocity dispersion) are taken from Mei et al. (2007), McLaughlin (1999), and Ferrarese et al. (2012); and the projected phase-space boundaries are adopted from Jaffe et al. (2015), Yoon et al. (2017), and Mahajan et al. (2011). None of these inputs is derived from the dS0/dE spatial, mass, or phase-space distributions that form the central claim. The conclusion that low-mass dS0s transform rapidly into dEs while massive dS0s survive is an interpretation of observed scarcity patterns (e.g., faint dS0s absent from the stripped and virialized regions, bright dS0s dominating the virialized region), not an equation that reproduces those patterns by construction. The main self-citation is the EVCC morphological classification, which is load-bearing in the sense that the dS0 sample depends on it; however, it is an external data product with documented comparison to the VCC and independent DECaLS residual-image checks, and no step in the paper reduces the conclusion to the classification itself. A possible completeness bias against faint dS0s is a legitimate observational/correctness concern, but it is not a circularity of the kind where a prediction equals its input by definition or where a fitted parameter is renamed as a prediction.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

Everything needed for the central claim sits on assumed catalog quality and assumed orbital-phase mapping, not on free parameters fit by the paper. The thresholds used to split bright/faint samples are hand-chosen but standard. No new physical entities are introduced.

free parameters (2)
  • Bright/massive sample threshold = Mr < -16 mag (log M* > 10^8.5-10^8.6 Msun)
    Chosen by hand to split dS0s and dEs into bright and faint panels in Figures 4 and 6; the mass-dependent conclusion is phrased in terms of this split.
  • FUV-r = 5.5 color cut = 5.5 mag
    Adopted from Hammer et al. (2012) to separate star-forming from quiescent galaxies; affects statements about absence of blue-cored and star-forming ETdGs in PPS regions.
assumptions (5)
  • domain assumption EVCC morphological classifications (dS0 vs dE) are sufficiently complete and unbiased across clustercentric distance and luminosity.
    Invoked throughout, especially Section 2 and Figures 2-6. The paper reclassifies 44 VCC dEs as dS0s but does not quantify completeness or misclassification for faint dwarfs in the core.
  • domain assumption The projected phase-space boundaries (stripped, virialized, recently infalled) correctly trace orbital phase and ram-pressure effects for Virgo dwarf galaxies.
    Section 3.5 adopts Jaffe et al. 2015 and Yoon et al. 2017 prescriptions; the stripped-region curve is computed for a fixed stellar mass of 10^8 Msun and a spherical NFW halo, which the paper itself calls an ideal guideline.
  • domain assumption Stellar masses from the Bell et al. 2003 g-i color relation with Kroupa IMF apply accurately to dwarf galaxies.
    Section 2, Eq. 1; mass-dependent statements rely on these masses, but no comparison to dynamical masses or SED fitting is given.
  • domain assumption dS0s and ETdG(bc)s are transitional evolutionary phases toward dEs rather than stable distinct populations.
    Set up in the Introduction and used to interpret the differential radial/PPS distributions as transformation; this is the interpretive premise behind the central claim.
  • domain assumption FUV-r color tracks recent star formation with the Hammer et al. 2012 threshold separating star-forming from quiescent galaxies.
    Section 3.4; used to connect PPS locations to quenching.

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Cite this review

Pith. "Pith review of Evidence for Mass-dependent Evolution of Transitional Dwarf Galaxies in the Virgo Cluster." pith.science (2026). https://pith.science/paper/3D3RXGG5

@misc{pith2026241117086,
  author       = {Pith},
  title        = {Pith review of: Evidence for Mass-dependent Evolution of Transitional Dwarf Galaxies in the Virgo Cluster},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3D3RXGG5}},
  note         = {Machine review of arXiv:2411.17086}
}
read the original abstract

We present a study on the evolution of transitional dwarf galaxies, specifically dwarf lenticulars (dS0s) and early-type dwarfs with blue cores (ETdG(bc)s), driven by environmental processes in the Virgo cluster utilizing the Extended Virgo Cluster Catalog. We investigated the morphological fraction and stellar mass of transitional dwarf galaxies in relation to the clustercentric distance, compared to dwarf elliptical galaxies (dEs) and dwarf irregular galaxies (dIrrs). We found that dS0s beyond 0.7R_vir exhibit a similar trend in the morphology-clustercentric distance relation to dEs, demonstrating a decreasing fraction with clustercentric distance, whereas ETdG(bc)s display an opposite trend to dS0s. The spatial distributions of transitional dwarf galaxies and dEs correlate with the mass, in which fractions of bright, massive galaxies increase towards the central region of the Virgo cluster. In the mass-clustercentric distance plane, dS0s exhibit a skewed distribution that favors more massive galaxies than dEs at a given clustercentric distance. In the projected phase-space diagram, dS0s are scarce in the stripped region, whereas ETdG(bc)s are absent in both the stripped and virialized regions. In addition, the dS0s in the virialized region are predominantly brighter and more massive than the dEs, indicating that the transformation of dS0s into dEs depends on the stellar mass. We propose that the majority of observed dS0s constitute a population that has settled into the Virgo cluster, whereas ETdG(bc)s represent a recently accreted population. We discuss the impact of ram pressure stripping effects on mass-dependent morphological evolution.

Figures

Figures reproduced from arXiv: 2411.17086 by the authors.

Figure 1
Figure 1. Examples of four VCC dEs reclassified as dS0s in the EVCC. In each galaxy, the left panel denotes g-, r-, and i-band combined color image of DECaLS data, which provides greater depth than the SDSS image. The right panel shows the residual image provided by DECaLS resulting from the ellipse fit and the subsequent modeling of the light distribution. The residual images clearly show unambiguous disk substructures, incl… view at source ↗
Figure 2
Figure 2. (a, b, and c) Projected spatial distributions of galaxies with different morphological types. Panel (a) shows the spatial distribution of dEs (red circles) and dS0s (yellow circles) in the VCC. Panels (b) and (c) show the spatial distributions of dEs (red circles)/dS0s (yellow circles)/ETdG(bc)s (blue dots) and dIrrs (green crosses) in the EVCC, respectively. (d) Cumulative radial distributions of different morpholo… view at source ↗
Figure 3
Figure 3. Fraction of morphological types as a function of the projected clustercentric distance for dEs and dIrrs (top panel), and dS0s and ETdG(bc)s (bottom panel). The fractions of the different morphological types are shown as filled circles, and the number of galaxies for each filled circle is indicated. The solid and dashed curves indicate the fractions obtained from the EVCC and VCC, respectively. The bold solid curves… view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: (Main panel) Stellar mass (and r-band luminosity) versus clustercentric distance for dwarf galaxies with different morphological types in the EVCC: dEs (red circles), dS0s (yellow circles), ETdG(bc)s (blue dots), and dIrrs (green dots). The distributions of dEs and dS0…
Figure 5
Figure 5. Figure 5: PPS diagram of dwarf galaxies with various morphological types in the EVCC: dEs (red circles), dS0s (yellow circles), ETdG(bc)s (blue dots), and dIrrs (green dots). The y-axis is the line-of-sight velocity relative to the cluster mean radial velocity (∆v), normalized b…
Figure 6
Figure 6. Figure 6: (Top and middle panels) PPS diagrams of bright (Mr < −16, top panels) and faint (Mr > −16, middle panels) dEs (left panels) and dS0s (right panels). Filled circles with various colors represent galaxies in different regions: yellow for the stripped region, red for the …

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Works this paper leans on

89 extracted references · 19 canonical work pages

  1. [1]

    Aguerri, J. A. L., Iglesias-P´ aramo, J., V ´ ılchez, J. M., Mu˜ noz-Tu˜ n´ on, C., & S´ anchez-Janssen, R. 2005, AJ, 130, 475, doi: 10.1086/431360

    work page doi:10.1086/431360 2005

  2. [2]

    B., & Seo, M

    Ann, H. B., & Seo, M. 2024, MNRAS, 530, 210, doi: 10.1093/mnras/stae913

    work page doi:10.1093/mnras/stae913 2024

  3. [3]

    B., Seo, M., & Ha, D

    Ann, H. B., Seo, M., & Ha, D. K. 2015, ApJS, 217, 27, doi: 10.1088/0067-0049/217/2/27 Bah´ e, Y. M., McCarthy, I. G., Balogh, M. L., & Font, A. S. 2013, MNRAS, 430, 3017, doi: 10.1093/mnras/stt109 15

    doi:10.1088/0067-0049/217/2/27 2015

  4. [5]

    D., Binggeli, B., & Jerjen, H

    Barazza, F. D., Binggeli, B., & Jerjen, H. 2002, A&A, 391, 823, doi: 10.1051/0004-6361:20020875

    work page doi:10.1051/0004-6361:20020875 2002

  5. [7]

    F., McIntosh, D

    Bell, E. F., McIntosh, D. H., Katz, N., & Weinberg, M. D. 2003, ApJS, 149, 289, doi: 10.1086/378847

    doi:10.1086/378847 2003

  6. [8]

    Binggeli, B., & Cameron, L. M. 1991, A&A, 252, 27 —. 1993, A&AS, 98, 297

    1991

  7. [9]

    Binggeli, B., Sandage, A., & Tammann, G. A. 1985, AJ, 90, 1681, doi: 10.1086/113874 —. 1988, ARA&A, 26, 509, doi: 10.1146/annurev.aa.26.090188.002453

    arXiv 1985

  8. [10]

    A., & Sandage, A

    Binggeli, B., Tammann, G. A., & Sandage, A. 1987, AJ, 94, 251, doi: 10.1086/114467

    doi:10.1086/114467 1987

Show all 89 references
  1. [11]

    2008, ApJ, 674, 742, doi: 10.1086/525513

    Boselli, A., Boissier, S., Cortese, L., & Gavazzi, G. 2008, ApJ, 674, 742, doi: 10.1086/525513

    2008 doi

  2. [12]

    2022, A&A Rv, 30, 3, doi: 10.1007/s00159-022-00140-3

    Boselli, A., Fossati, M., & Sun, M. 2022, A&A Rv, 30, 3, doi: 10.1007/s00159-022-00140-3

    2022 doi

  3. [13]

    2006, PASP, 118, 517, doi: 10.1086/500691

    Boselli, A., & Gavazzi, G. 2006, PASP, 118, 517, doi: 10.1086/500691

    2006 doi

  4. [14]

    2022a, A&A, 657, A9, doi: 10.1051/0004-6361/202040141

    Castignani, G., Combes, F., Jablonka, P., et al. 2022a, A&A, 657, A9, doi: 10.1051/0004-6361/202040141

    doi

  5. [15]

    A., et al

    Castignani, G., Vulcani, B., Finn, R. A., et al. 2022b, ApJS, 259, 43, doi: 10.3847/1538-4365/ac45f7

    doi

  6. [16]

    A., & Buzzoni, A

    Cellone, S. A., & Buzzoni, A. 2005, MNRAS, 356, 41, doi: 10.1111/j.1365-2966.2004.08422.x

    2005

  7. [17]

    2021, ApJ, 923, 235, doi: 10.3847/1538-4357/ac3002

    Chung, J., Kim, S., Rey, S.-C., & Lee, Y. 2021, ApJ, 923, 235, doi: 10.3847/1538-4357/ac3002

    2021 doi

  8. [18]

    H., Jeong, H., & Kim, S

    Chung, J., Lee, J. H., Jeong, H., & Kim, S. 2023, ApJ, 949, 80, doi: 10.3847/1538-4357/accae1

    2023 doi

  9. [19]

    2019, ApJ, 879, 97, doi: 10.3847/1538-4357/ab25e8

    Chung, J., Rey, S.-C., Sung, E.-C., et al. 2019, ApJ, 879, 97, doi: 10.3847/1538-4357/ab25e8

    2019 doi

  10. [20]

    J., Gallagher, John S., I., & Wyse, R

    Conselice, C. J., Gallagher, John S., I., & Wyse, R. F. G. 2001, ApJ, 559, 791, doi: 10.1086/322373 —. 2003, AJ, 125, 66, doi: 10.1086/345385

    2001 doi

  11. [21]

    P., et al

    Cortese, L., van de Sande, J., Lagos, C. P., et al. 2019, MNRAS, 485, 2656, doi: 10.1093/mnras/stz485

    2019 doi

  12. [22]

    L., & Songaila, A

    Cowie, L. L., & Songaila, A. 1977, Nature, 266, 501, doi: 10.1038/266501a0 De Rijcke, S., Buyle, P., & Koleva, M. 2013, ApJL, 770, L26, doi: 10.1088/2041-8205/770/2/L26 De Rijcke, S., Dejonghe, H., Zeilinger, W. W., & Hau, G. K. T. 2003, A&A, 400, 119, doi: 10.1051/0004-6361:2...

    1977 doi

  13. [23]

    1980, ApJS, 42, 565, doi: 10.1086/190663

    Dressler, A. 1980, ApJS, 42, 565, doi: 10.1086/190663

    1980 doi

  14. [24]

    J., Gregg, M

    Drinkwater, M. J., Gregg, M. D., Holman, B. A., & Brown, M. J. I. 2001, MNRAS, 326, 1076, doi: 10.1046/j.1365-8711.2001.04646.x

    2001

  15. [25]

    2016, ApJ, 826, 148, doi: 10.3847/0004-637X/826/2/148

    Emerick, A., Mac Low, M.-M., Grcevich, J., & Gatto, A. 2016, ApJ, 826, 148, doi: 10.3847/0004-637X/826/2/148

    2016 doi

  16. [26]

    M., Bettoni, D., et al

    Fasano, G., Poggianti, B. M., Bettoni, D., et al. 2015, MNRAS, 449, 3927, doi: 10.1093/mnras/stv500

    2015 doi

  17. [27]

    Ferguson, H. C. 1989, AJ, 98, 367, doi: 10.1086/115152

    1989 doi

  18. [28]

    C., & Binggeli, B

    Ferguson, H. C., & Binggeli, B. 1994, A&A Rv, 6, 67, doi: 10.1007/BF01208252

    1994 doi

  19. [29]

    2012, ApJS, 200, 4, doi: 10.1088/0067-0049/200/1/4

    Ferrarese, L., Cˆ ot´ e, P., Cuillandre, J.-C., et al. 2012, ApJS, 200, 4, doi: 10.1088/0067-0049/200/1/4

    2012 doi

  20. [30]

    P., Cooper, M

    Fillingham, S. P., Cooper, M. C., Pace, A. B., et al. 2016, MNRAS, 463, 1916, doi: 10.1093/mnras/stw2131

    2016 doi

  21. [31]

    P., Cooper, M

    Fillingham, S. P., Cooper, M. C., Wheeler, C., et al. 2015, MNRAS, 454, 2039, doi: 10.1093/mnras/stv2058

    2015 doi

  22. [32]

    G., Metcalfe, N., & Peach, J

    Godwin, J. G., Metcalfe, N., & Peach, J. V. 1983, MNRAS, 202, 113, doi: 10.1093/mnras/202.1.113

    1983 doi

  23. [33]

    W., & Guzm´ an, R

    Graham, A. W., & Guzm´ an, R. 2003, AJ, 125, 2936, doi: 10.1086/374992

    2003 doi

  24. [34]

    E., Danieli, S., Carlsten, S., et al

    Greene, J. E., Danieli, S., Carlsten, S., et al. 2023, ApJ, 949, 94, doi: 10.3847/1538-4357/acc58c

    2023 doi

  25. [35]

    2006, AJ, 131, 806, doi: 10.1086/498891

    Gu, Q., Zhao, Y., Shi, L., Peng, Z., & Luo, X. 2006, AJ, 131, 806, doi: 10.1086/498891

    2006 doi

  26. [36]

    E., & Gott, J

    Gunn, J. E., & Gott, J. Richard, I. 1972, ApJ, 176, 1, doi: 10.1086/151605

    1972 doi

  27. [37]

    M., Hornschemeier, A

    Hammer, D. M., Hornschemeier, A. E., Salim, S., et al. 2012, ApJ, 745, 177, doi: 10.1088/0004-637X/745/2/177

    2012 doi

  28. [38]

    F., Khosroshahi, H

    Hamraz, E., Peletier, R. F., Khosroshahi, H. G., et al. 2019, A&A, 625, A94, doi: 10.1051/0004-6361/201935076 Hern´ andez-Fern´ andez, J. D., Haines, C. P., Diaferio, A., et al. 2014, MNRAS, 438, 2186, doi: 10.1093/mnras/stt2354

    2019 doi

  29. [40]

    2012, ApJL, 745, L24, doi: 10.1088/2041-8205/745/2/L24

    Janz, J., Laurikainen, E., Lisker, T., et al. 2012, ApJL, 745, L24, doi: 10.1088/2041-8205/745/2/L24

    2012 doi

  30. [41]

    Jerjen, H., Binggeli, B., & Barazza, F. D. 2004, AJ, 127, 771, doi: 10.1086/381065

    2004 doi

  31. [42]

    2000, A&A, 358, 845, doi: 10.48550/arXiv.astro-ph/0004248 16

    Jerjen, H., Kalnajs, A., & Binggeli, B. 2000, A&A, 358, 845, doi: 10.48550/arXiv.astro-ph/0004248 16

    2000 doi arXiv

  32. [43]

    D., & Nasonova, O

    Karachentsev, I. D., & Nasonova, O. G. 2013, MNRAS, 429, 2677, doi: 10.1093/mnras/sts557

    2013 doi

  33. [44]

    C., Rich, R

    Kaviraj, S., Rey, S. C., Rich, R. M., Yoon, S. J., & Yi, S. K. 2007, MNRAS, 381, L74, doi: 10.1111/j.1745-3933.2007.00370.x

    2007

  34. [45]

    E., Arag´ on-Salamanca, A., et al

    Kelkar, K., Gray, M. E., Arag´ on-Salamanca, A., et al. 2019, MNRAS, 486, 868, doi: 10.1093/mnras/stz905

    2019 doi

  35. [46]

    1998, ARA&A, 36, 189, doi: 10.1146/annurev.astro.36.1.189

    Kennicutt, Robert C., J. 1998, ARA&A, 36, 189, doi: 10.1146/annurev.astro.36.1.189

    1998 doi

  36. [47]

    Kim, S., Rey, S.-C., Lisker, T., & Sohn, S. T. 2010, ApJL, 721, L72, doi: 10.1088/2041-8205/721/1/L72

    2010 doi

  37. [48]

    2014, ApJS, 215, 22, doi: 10.1088/0067-0049/215/2/22

    Kim, S., Rey, S.-C., Jerjen, H., et al. 2014, ApJS, 215, 22, doi: 10.1088/0067-0049/215/2/22

    2014 doi

  38. [49]

    2016, ApJ, 833, 207, doi: 10.3847/1538-4357/833/2/207

    Kim, S., Rey, S.-C., Bureau, M., et al. 2016, ApJ, 833, 207, doi: 10.3847/1538-4357/833/2/207

    2016 doi

  39. [50]

    A., & Gilmore, G

    Kroupa, P., Tout, C. A., & Gilmore, G. 1993, MNRAS, 262, 545, doi: 10.1093/mnras/262.3.545

    1993 doi

  40. [51]

    B., Tinsley, B

    Larson, R. B., Tinsley, B. M., & Caldwell, C. N. 1980, ApJ, 237, 692, doi: 10.1086/157917

    1980 doi

  41. [52]

    2021, ApJ, 906, 68, doi: 10.3847/1538-4357/abcaa0

    Lee, Y., Kim, S., Rey, S.-C., & Chung, J. 2021, ApJ, 906, 68, doi: 10.3847/1538-4357/abcaa0

    2021 doi

  42. [53]

    2009, Astronomische Nachrichten, 330, 1043, doi: 10.1002/asna.200911291

    Lisker, T. 2009, Astronomische Nachrichten, 330, 1043, doi: 10.1002/asna.200911291

    2009 doi

  43. [54]

    Lisker, T., Glatt, K., Westera, P., & Grebel, E. K. 2006a, AJ, 132, 2432, doi: 10.1086/508414

    doi

  44. [55]

    K., & Binggeli, B

    Lisker, T., Grebel, E. K., & Binggeli, B. 2006b, AJ, 132, 497, doi: 10.1086/505045

    doi

  45. [56]

    K., Binggeli, B., & Glatt, K

    Lisker, T., Grebel, E. K., Binggeli, B., & Glatt, K. 2007, ApJ, 660, 1186, doi: 10.1086/513090

    2007 doi

  46. [57]

    A., & Raychaudhury, S

    Mahajan, S., Mamon, G. A., & Raychaudhury, S. 2011, MNRAS, 416, 2882, doi: 10.1111/j.1365-2966.2011.19236.x

    2011

  47. [58]

    2003, MNRAS, 345, 1329, doi: 10.1046/j.1365-2966.2003.07054.x Mart ´ ınez, H

    Marcolini, A., Brighenti, F., & D’Ercole, A. 2003, MNRAS, 345, 1329, doi: 10.1046/j.1365-2966.2003.07054.x Mart ´ ınez, H. J., Coenda, V., Muriel, H., de los Rios, M., &

    2003

  48. [59]

    Ruiz, A. N. 2023, MNRAS, 519, 4360, doi: 10.1093/mnras/stac3746

    2023 doi

  49. [60]

    McLaughlin, D. E. 1999, ApJL, 512, L9, doi: 10.1086/311860

    1999 doi

  50. [61]

    P., Cˆ ot´ e, P., et al

    Mei, S., Blakeslee, J. P., Cˆ ot´ e, P., et al. 2007, ApJ, 655, 144, doi: 10.1086/509598

    2007 doi

  51. [62]

    2022, AJ, 164, 18, doi: 10.3847/1538-3881/ac6f5f

    Michea, J., Pasquali, A., Smith, R., et al. 2022, AJ, 164, 18, doi: 10.3847/1538-3881/ac6f5f

    2022 doi

  52. [63]

    1996, Nature, 379, 613, doi: 10.1038/379613a0

    Moore, B., Katz, N., Lake, G., Dressler, A., & Oemler, A. 1996, Nature, 379, 613, doi: 10.1038/379613a0

    1996 doi

  53. [64]

    1998, ApJ, 495, 139, doi: 10.1086/305264

    Moore, B., Lake, G., & Katz, N. 1998, ApJ, 495, 139, doi: 10.1086/305264

    1998 doi

  54. [65]

    2000, ApJ, 538, 559, doi: 10.1086/309140

    Mori, M., & Burkert, A. 2000, ApJ, 538, 559, doi: 10.1086/309140

    2000 doi

  55. [66]

    2021, ApJ, 914, 145, doi: 10.3847/1538-4357/abedb6

    Morokuma-Matsui, K., Kodama, T., Morokuma, T., et al. 2021, ApJ, 914, 145, doi: 10.3847/1538-4357/abedb6

    2021 doi

  56. [67]

    1999, MNRAS, 309, 161, doi: 10.1046/j.1365-8711.1999.02810.x

    Murakami, I., & Babul, A. 1999, MNRAS, 309, 161, doi: 10.1046/j.1365-8711.1999.02810.x

    1999

  57. [68]

    Muzzin, A., van der Burg, R. F. J., McGee, S. L., et al. 2014, ApJ, 796, 65, doi: 10.1088/0004-637X/796/1/65

    2014 doi

  58. [69]

    F., Frenk, C

    Navarro, J. F., Frenk, C. S., & White, S. D. M. 1996, ApJ, 462, 563, doi: 10.1086/177173

    1996 doi

  59. [70]

    A., & Hudson, M

    Oman, K. A., & Hudson, M. J. 2016, MNRAS, 463, 3083, doi: 10.1093/mnras/stw2195

    2016 doi

  60. [71]

    A., Hudson, M

    Oman, K. A., Hudson, M. J., & Behroozi, P. S. 2013, MNRAS, 431, 2307, doi: 10.1093/mnras/stt328

    2013 doi

  61. [72]

    2014, MNRAS, 445, 630, doi: 10.1093/mnras/stu1722

    Pak, M., Rey, S.-C., Lisker, T., et al. 2014, MNRAS, 445, 630, doi: 10.1093/mnras/stu1722

    2014 doi

  62. [74]

    J., Kovaˇ c, K., et al

    Peng, Y.-j., Lilly, S. J., Kovaˇ c, K., et al. 2010, ApJ, 721, 193, doi: 10.1088/0004-637X/721/1/193

    2010 doi

  63. [75]

    2023, ApJ, 945, 140, doi: 10.3847/1538-4357/acbc1c

    Rey, S.-C., Kim, S., Chung, J., & Lee, Y. 2023, ApJ, 945, 140, doi: 10.3847/1538-4357/acbc1c

    2023 doi

  64. [76]

    2020, ApJS, 247, 45, doi: 10.3847/1538-4365/ab7377 —

    Rhee, J., Smith, R., Choi, H., et al. 2020, ApJS, 247, 45, doi: 10.3847/1538-4365/ab7377 —. 2017, ApJ, 843, 128, doi: 10.3847/1538-4357/aa6d6c Romero-G´ omez, J., Aguerri, J. A. L., Peletier, R. F., et al. 2024, MNRAS, 527, 9715, doi: 10.1093/mnras/stad3801 S´ anchez Almeida, ...

    2020 doi

  65. [77]

    1984, AJ, 89, 919, doi: 10.1086/113588

    Sandage, A., & Binggeli, B. 1984, AJ, 89, 919, doi: 10.1086/113588

    1984 doi

  66. [78]

    Sandage, A., Binggeli, B., & Tammann, G. A. 1985, AJ, 90, 1759, doi: 10.1086/113875

    1985 doi

  67. [79]

    J., Lucey, J

    Smith, R. J., Lucey, J. R., & Hudson, M. J. 2009, MNRAS, 400, 1690, doi: 10.1111/j.1365-2966.2009.15580.x

    2009

  68. [80]

    J., Marzke, R

    Smith, R. J., Marzke, R. O., Hornschemeier, A. E., et al. 2008, MNRAS, 386, L96, doi: 10.1111/j.1745-3933.2008.00469.x

    2008

  69. [81]

    2010, MNRAS, 404, 1775, doi: 10.1111/j.1365-2966.2010.16427.x

    Silk, J. 2010, MNRAS, 404, 1775, doi: 10.1111/j.1365-2966.2010.16427.x

    2010

  70. [82]

    J., et al

    Toloba, E., Boselli, A., Cenarro, A. J., et al. 2011, A&A, 526, A114, doi: 10.1051/0004-6361/201015344

    2011 doi

  71. [83]

    F., et al

    Toloba, E., Guhathakurta, P., Peletier, R. F., et al. 2014, ApJS, 215, 17, doi: 10.1088/0067-0049/215/2/17

    2014 doi

  72. [84]

    2015, ApJ, 799, 172, doi: 10.1088/0004-637X/799/2/172

    Toloba, E., Guhathakurta, P., Boselli, A., et al. 2015, ApJ, 799, 172, doi: 10.1088/0004-637X/799/2/172

    2015 doi

  73. [85]

    Tully, R. B. 1982, ApJ, 257, 389, doi: 10.1086/159999

    1982 doi

  74. [86]

    B., & Trentham, N

    Tully, R. B., & Trentham, N. 2008, AJ, 135, 1488, doi: 10.1088/0004-6256/135/4/1488 17

    2008 doi

  75. [87]

    2017, A&A, 606, A135, doi: 10.1051/0004-6361/201730897

    Urich, L., Lisker, T., Janz, J., et al. 2017, A&A, 606, A135, doi: 10.1051/0004-6361/201730897

    2017 doi

  76. [88]

    M., Gullieuszik, M., et al

    Vulcani, B., Poggianti, B. M., Gullieuszik, M., et al. 2023, ApJ, 949, 73, doi: 10.3847/1538-4357/acc5e2

    2023 doi

  77. [89]

    R., Tollerud, E

    Wetzel, A. R., Tollerud, E. J., & Weisz, D. R. 2015, ApJL, 808, L27, doi: 10.1088/2041-8205/808/1/L27

    2015 doi

  78. [90]

    I., Cooper, M

    Wheeler, C., Phillips, J. I., Cooper, M. C., Boylan-Kolchin, M., & Bullock, J. S. 2014, MNRAS, 442, 1396, doi: 10.1093/mnras/stu965

    2014 doi

  79. [91]

    2009, MNRAS, 393, 1302, doi: 10.1111/j.1365-2966.2008.14204.x

    Wolf, C., Arag´ on-Salamanca, A., Balogh, M., et al. 2009, MNRAS, 393, 1302, doi: 10.1111/j.1365-2966.2008.14204.x

    2009

  80. [92]

    K., Yoon, S

    Yi, S. K., Yoon, S. J., Kaviraj, S., et al. 2005, ApJL, 619, L111, doi: 10.1086/422811

    2005 doi

  81. [93]

    Yoon, H., Chung, A., Smith, R., & Jaff´ e, Y. L. 2017, ApJ, 838, 81, doi: 10.3847/1538-4357/aa6579

    2017 doi

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