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The S-PLUS Fornax Project (S+FP): Mapping H$\alpha$+[NII] emission in 77 Fornax galaxy members reaching $\sim$4 Rvir

T0 review · 4 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read The paper claims that the PELE pipeline, combining S-PLUS narrow- and broad-band images via the Three Filter Method, reliably maps H$\alpha$+[N II] emission in 77 Fornax cluster members out to about four virial radii, with 91% identified…

desk verdict A valuable new catalog of Hα+[NII] emitters in Fornax out to 4 Rvir, with an honest but incomplete treatment of depth-dependent detection thresholds. read the letter →

arxiv 2505.16738 v1 pith:QLO4CZUW submitted 2025-05-22 astro-ph.GA

A. R. Lopes , A. V. Smith Castelli , A. C. Krabbe , J. A. Hernandez-Jimenez , D. Pallero , S. Torres-Flores , E.Telles , M. Sarzi
show 26 more authors
A. Cortesi J. Thainá-Batista R. Cid Fernandes E. A. D. Lacerda M. Sampaio V. H. Sasse F. R. Herpich I. Andruchow R. Demarco L. A. Gutiérrez-Soto M. Grossi R. F. Haack P. K. Humire C. Lima-Dias G. Limberg C. Lobo L. Lomelí-Núñez P. A. A. Lopes D. E. Olave-Rojas S.V . Werner F. Almeida-Fernandes G.B. Oliveira Schwarz W. Schoenell T. Ribeiro A. Kanaan C. Mendes de Oliveira
This is my paper · ORCID
classification astro-ph.GA
keywords galaxyclustersFornaxclusterHαemissionemission-linegalaxiesphotometricsurveysS-PLUSpre-processingprojectedphasespace
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 establishes that a new semi-automated pipeline, PELE, can recover spatially resolved H$\alpha$+[N II] emission from wide-field S-PLUS images down to a flux of about $2\times10^{-17}$ erg s$^{-1}$ cm$^{-2}$, calibrated against MUSE data. Applied to the Fornax cluster, it produces emission maps for 77 member galaxies with $r<18$ mag out to $\sim4 R_{\rm vir}$, far beyond the reach of integral-field surveys. Among these emitters, 75% are late-type and 25% are early-type; 91% occupy the recent-infall regions of the projected phase-space diagram, and 44% of the late-type emitters show morphological perturbation or merger features. Disturbed, low-mass emitters at projected radii beyond $2.5R_{\rm vir}$ are interpreted as evidence that galaxies begin transforming before entering the cluster. The paper argues that wide-field photometric surveys can therefore trace cluster assembly history and pre-processing without requiring spectroscopy for every galaxy.

What carries the argument

The load-bearing tool is the PELE (Pixel-to-Pixel Emission Line Estimate) pipeline, a semi-automated code that builds 12-band S-PLUS datacubes, masks foreground stars and background sources, homogenizes the point-spread function across filters, applies a Butterworth spatial filter and Voronoi binning to reach a target signal-to-noise of 10 in the J0660 narrow-band, and then estimates the H$\alpha$+[N II] flux per pixel using the Three Filter Method. The Three Filter Method assumes the emission line behaves as a Dirac delta at the line wavelength while the continuum is linear across the J0660 narrow-band and the $r$ and $i$ broad bands; the equation from Vilella-Rojo et al. (2015) converts the three measured fluxes into a line flux. A final 3$\sigma$ clipping removes low-flux pixels that the method systematically overestimates, which sets the detection floor near $2\times10^{-17}$ erg s$^{-1}$ cm$^{-2}$.

What would settle it

If a MUSE-detected galaxy with H$\alpha$ flux above $2\times10^{-17}$ erg s$^{-1}$ cm$^{-2}$ is located in a shallow S-PLUS field and PELE fails to recover it, while an identical source in a deep field is recovered, the claimed uniform detection limit would be falsified.

Watch

Extended reading notes

Core claim

The central discovery is that the PELE pipeline, using S-PLUS images and the Three Filter Method, yields reliable pixel-by-pixel H$\alpha$+[N II] maps for 77 Fornax cluster members out to $\sim4 R_{\rm vir}$, with a detection limit near $2\times10^{-17}$ erg s$^{-1}$ cm$^{-2}$ validated against MUSE observations of 13 galaxies. The recovered sample is dominated by late-type galaxies (75%), and 91% of all emitters lie in phase-space regions associated with infall within the last gigayear. A substantial fraction (38% overall, 44% of late-types) show morphological disturbance or merger signatures, and these disturbed systems preferentially appear at large clustercentric distances. The spatial distribution shows a concentration of emitters in the northwest, possibly tracing a filament connecting Fornax to Eridanus, while the Fornax A group contributes a distinct southwest component. These results are interpreted as direct observational evidence that galaxy preprocessing starts well before the galaxies cross the cluster's virial radius.

Load-bearing premise

The detection threshold of about $2\times10^{-17}$ erg s$^{-1}$ cm$^{-2}$, calibrated on 13 MUSE galaxies and enforced by a post-hoc 3$\sigma$ clipping that removes overestimated low-flux pixels, is assumed to be uniform across all S-PLUS fields even though the survey's depth varies by up to one magnitude from field to field.

Editorial extensions

If this is right

  • The same pipeline can be reused to build H$\alpha$+[N II] maps for other nearby clusters covered by S-PLUS, effectively turning a wide-field photometric survey into a star-formation census of cluster outskirts.
  • The 77 emitters provide a homogeneous target list for future H I and CO follow-up at projected radii beyond $1R_{\rm vir}$, where radio data are currently scarce, to test the pre-processing interpretation directly.
  • The phase-space classification places 91% of emitters as recent infallers, implying that most of the current H$\alpha$ emission in Fornax is tied to galaxies that entered the cluster within roughly the last gigayear.
  • The observed fractions of disturbed, low-mass emitters at large radii set quantitative expectations that cosmological simulations of Fornax-like systems can be compared against.

Reading between the lines

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

  • If the uniform detection threshold holds across S-PLUS fields, the same methodology could be extended to the J0378 narrow-band filter to map [O II] emission in Fornax, doubling the diagnostics available from the same datacubes.
  • The proposed Fornax-Eridanus filament could be tested by running PELE on S-PLUS fields between Fornax and the Eridanus cluster; a continuous chain of emitters would strengthen the filament scenario.
  • A direct test of the depth-uniformity assumption would be to cross-calibrate PELE on overlapping S-PLUS fields of differing depth; if the detection threshold varies, the reported 91% recent-infaller fraction may need to be re-derived as a function of field depth.
  • The comparison to IllustrisTNG-50 suggests a testable prediction: the resolved star-formation efficiency of infalling late-type galaxies should be skewed toward the cluster-facing side, which could be measured with IFU observations of a few nearby emitters.
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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

4 major / 5 minor

Summary. The paper presents PELE, a semi-automated pipeline that produces Hα+[N II] emission maps from S-PLUS 12-band images using the Three Filter Method, and applies it to the Fornax cluster and its outskirts. The pipeline is validated against MUSE/F3D Hα maps for 13 galaxies and cross-checked against literature Hα emitter catalogs. The authors report 77 Hα+[N II] emitters with r<18 mag extending to about 4 Rvir, classify their optical morphologies with ASTROMORPHLIB, place them in the projected phase-space (PPS) diagram, and compare with HI/CO data and with an IllustrisTNG-50 Fornax-like system. They conclude that 91% of the emitters are recent infallers, that 44% of late-type emitters show signs of perturbation or merging, and that disturbed low-mass galaxies at large clustercentric distances indicate pre-processing before cluster entry.

Significance. If the results are robust, this is a valuable demonstration of wide-field narrow-band mapping of Hα+[N II] in a nearby cluster, reaching regions beyond the reach of current IFS surveys. The explicit validation against 13 MUSE galaxies, the recovery of 78% of Drinkwater et al. (2001) emitters, and the systematic morphological and phase-space analysis are strengths, and the appendix maps and table are a useful data product. The scientific conclusions about recent infall and pre-processing are plausible but depend on the uniformity of the detection threshold across fields, the completeness of the parent sample, and the adopted PPS parameters; these points need to be quantified before the headline fractions can be taken at face value.

major comments (4)
  1. [3.1 and 3.2] The paper sets a single global detection limit of about 2e-17 erg/s/cm^2 from 13 F3D/MUSE galaxies, all located within the virial radius of Fornax (Section 2.3), but Section 3.1 notes that S-PLUS depth varies by up to 1 mag from field to field. The limit is implemented as a post-hoc 3-sigma clipping of low-flux pixels, so the effective threshold is not the same in shallower outer fields, where many of the claimed recent infallers and pre-processing candidates lie. This can preferentially remove diffuse, low-surface-brightness emission, which the authors themselves say is the least reliably recovered component (Section 4). Because PELE measures Hα+[N II] while MUSE maps are Hα only, part of the "overestimation" removed by the clipping may be genuine [N II] flux, so the calibration conflates noise rejection with an astrophysical correction. I ask for per-field detection limits derived from the S-PLUS weight/noise images, a plot of the threshold across the fields, and a completeness test as a function of field depth and clustercentric radius.
  2. [4.3] The headline 91% recent-infaller fraction depends on the adopted Vcluster=1442 km/s and sigma=318 km/s, and the paper itself shows that NGC 1380 moves from the ancient-infaller region E to the recent-infaller region C when the Iodice et al. (2019a) values V=1425 km/s and sigma=300 km/s are used. The statement that all other common galaxies occupy consistent locations is not a quantitative sensitivity test. I request the number of the 77 galaxies that change PPS region under reasonable alternative parameter values and under the parameter uncertainties, and an explicit statement of how many galaxies enter the 91% statistic. In addition, ESO 358-11 and ESO 359-25 have no radial velocities in Table A.1 and therefore cannot be placed in Fig. 8; the sample size actually used for the PPS analysis should be stated.
  3. [4.1] The fractions 44% for disturbed late-type emitters and 15% for early-type emitters are central results, but the C, A, Gini, and M20 measurements from ASTROMORPHLIB are presented without uncertainties or robustness tests. Many of the outer-sample galaxies are low-mass objects near the r=18 mag limit, where non-parametric morphology indices are sensitive to background subtraction, segmentation, and surface-brightness limits. I request a robustness check, for example by varying the segmentation/background parameters, excluding low-S/N galaxies, or comparing against visual classifications of disturbance, to show that the disturbed fractions are not driven by measurement systematics.
  4. [2.1 and 4.2] The parent sample of 233 galaxies with velocities is spectroscopically incomplete, and no detection-completeness function is provided for the 77 emitters as a function of radius, magnitude, or emission morphology. Because ancient or intermediate infallers are expected to have weaker Hα+[N II] emission, the conclusion that 91% of emitters are recent infallers could be partly a selection effect. Comparing the PPS distribution of emitters with that of non-emitters, or adding an upper-limit treatment, would substantially strengthen the claim that Hα+[N II] emission traces recent infall rather than simply reflecting which galaxies are detectable. The same incompleteness affects the spatial asymmetry in the northwest and the statement that the eastern region has no distinct substructure.
minor comments (5)
  1. [Abstract and Section 2.1] The abstract says "within the four virial radius of the Fornax cluster"; this should be reworded to "within four times the virial radius" or "out to approximately 4 Rvir" to avoid ambiguity.
  2. [Section 4.2] There is a typo in "marked by an different in the number of objects," and "Fornax AR vir" should read "Fornax A Rvir."
  3. [Section 4.6] The sentence "we find an extended emission in 24 (58%) extended, knots in 20 (42%), and 4 (6%) with central concentration" has percentages that do not sum to 100 and appears to list overlapping categories; please clarify whether the categories are exclusive or whether a galaxy can appear in more than one.
  4. [Figure 12] The y-axis label "RSFE M /yr 1" appears corrupted; it should read "RSFE (yr^-1)" or similar, and the definition of RSFE in Eq. (5) should be stated consistently in the figure caption.
  5. [Table A.1] The radial-velocity entries for ESO 358-11 and ESO 359-25 are blank, and the text says only two of the 77 emitters lack spectroscopic confirmation. Please state explicitly how these objects are treated in the spatial and PPS analyses.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the PELE detection limit is calibrated against independent F3D/MUSE H-alpha maps, and the morphological and phase-space classifications come from external references.

full rationale

The paper's derivation chain is self-contained rather than circular. The central detection claim, that PELE reliably recovers H-alpha+[N II] flux down to ~2e-17 erg/s/cm2, is validated against 13 galaxies with MUSE/F3D H-alpha maps (Section 3.2), which are independent of the 77 Fornax emitters being reported. The detection threshold is therefore an externally calibrated benchmark, not a quantity fitted to the same data used for the physical conclusions. The Three Filter Method is taken from the established formalism of Pascual et al. (2007) and Vilella-Rojo et al. (2015), not from a self-cited ansatz. The PPS regions used to classify recent infallers come from Rhee et al. (2017), and the morphological disturbance/merger criteria come from Lotz et al. (2008) and Krabbe et al. (2024); even though Krabbe is an overlapping author, the criterion is an externally published diagnostic applied post hoc, not derived from the present sample. The IllustrisTNG-50 Fornax-like comparison is an external simulation. The only self-citations that enter the analysis are Paper I (Smith Castelli et al. 2024) for the member list and depth information, and Thainá-Batista et al. (2023) for a preliminary PELE check; neither is a load-bearing premise that forces the conclusions. The paper explicitly flags a real limitation in Section 3.2: the depth of S-PLUS images varies by up to 1 mag across fields, yet a single global detection threshold is adopted. This could affect completeness and bias the emitter sample, but it is a measurement-limitation, not a circular step: no equation reduces the conclusions to the threshold by construction. For these reasons, no circularity is identified.

Assumptions & free parameters 1 free parameters · 5 assumptions · 0 invented entities

The paper introduces no new physical entities. Its main free choice is the sigma-clipping threshold used to set the detection limit. The listed axioms are standard domain assumptions for narrow-band photometric emission-line studies and cluster infall classification.

free parameters (1)
  • sigma_clipping_threshold = 3σ
    Chosen in Sec 3.2 to remove overestimated low-flux pixels identified by comparison with MUSE maps; this threshold defines the detection limit and thus the sample.
assumptions (5)
  • domain assumption The Three Filter Method assumptions hold: the emission line is a Dirac delta centered at the line wavelength and the continuum is linear over the r, i, J0660 filters.
    Sec 3.1, Eq. 1; this underpins the flux estimate.
  • domain assumption All target galaxies are at the cluster mean redshift z=0.0048 for the line wavelength.
    Sec 3.1; a wrong redshift would mis-center the line in the filter band.
  • domain assumption The 233 spectroscopically confirmed members with velocities 600-3000 km/s are the relevant parent population for finding emitters.
    Sec 2.1; incomplete spectroscopy in the outskirts biases the emitter sample location.
  • domain assumption Morphological disturbance boundaries from Krabbe et al. (2024) and Lotz et al. (2008) apply to the Fornax galaxies.
    Sec 4.1; these boundaries were calibrated on other samples.
  • domain assumption IllustrisTNG-50 contains a Fornax-like system (M200=6.7e13 Msun) that is an adequate analog for comparing emitter counts and star-formation distributions.
    Sec 4.7; the comparison is qualitative and depends on the simulation's subgrid physics.

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Cite this review

Pith. "Pith review of The S-PLUS Fornax Project (S+FP): Mapping H$\alpha$+[NII] emission in 77 Fornax galaxy members reaching $\sim$4 Rvir." pith.science (2026). https://pith.science/paper/QLO4CZUW

@misc{pith2026250516738,
  author       = {Pith},
  title        = {Pith review of: The S-PLUS Fornax Project (S+FP): Mapping H$\alpha$+[NII] emission in 77 Fornax galaxy members reaching $\sim$4 Rvir},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/QLO4CZUW}},
  note         = {Machine review of arXiv:2505.16738}
}
abstract

The Fornax cluster, the second-largest galaxy cluster within 20 Mpc, presents an ideal environment for studying environmental effects on galaxy evolution. Utilizing data from the Southern Photometric Local Universe Survey (S-PLUS), this study explores the H$\alpha$+[NII] emission maps across an area of approximately 208 square degrees around NGC 1399. For such, a dedicated semi-automated pipeline, Pixel-to-Pixel Emission Line Estimate (PELE), was developed to generate emission line maps by processing S-PLUS images using the Three Filter Method. A morphological analysis was conducted using the ASTROMORPHLIB package to determine whether H$\alpha$+[NII] emitters exhibit perturbed features. The study successfully detected 77 H$\alpha$+[NII] emitters with $r<18$ mag, extending to four times the virial radius of the Fornax cluster. PELE demonstrated its ability to recover flux down to 2e-17 erg s$^{-1}$ cm$^{-2}$ when compared to H$\alpha$ maps from MUSE/VLT. Among the emitters, 25% are early-type galaxies (ETG) and 75% late-type galaxies (LTG). Signs of morphological perturbation or merger activity are observed in 44% of the LTG and in three ETG located beyond the cluster's virial radius. A significant fraction (91%) of the emitters are identified as recent infallers, primarily located in the northwestern region of the cluster, while others are associated with the infalling group Fornax A in the southwest. Disturbed, low-mass galaxies at larger cluster-centric distances provide evidence of galaxies begin transforming before entering the main cluster. This study demonstrates S-PLUS's effectiveness in detecting emitters, whose distribution reflects the Fornax cluster's assembly history, with LTG linked to recent infall from the field, possibly along a Fornax-Eridanus filament, and ETG may have evolved prior to entry.

Figures

Figures reproduced from arXiv: 2505.16738 by the authors.

Figure 1
Figure 1. The redshift evolution of the observed wavelength of the [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. The workflow associated with the PELE code. The in￾put information is a list of galaxies with ID, RA, Dec and size of the images, followed by the creation of masks, in which the user can check the objects to be masked and labeled as stars and main galaxy. Then the code automatically performs the image processing, including PSF homogenization, Butterworth filter￾ing, binning functions and the Three Filter Method. Pri… view at source ↗
Figure 3
Figure 3. Comparison of the Hα+[N II] maps derived from S-PLUS data with the Hα maps obtained from F3D/MUSE for FCC 263 (top) and FCC 312 (bottom). The left panels display the Legacy Survey images (a combination of g, r, and z bands) at the same scale as the Hα+[N II] maps from S-PLUS (middle panels) and MUSE (right panels).The contours are based on the MUSE Hα map, corresponding to isophotes of 1 × 10−18 (blue), 1 × 10−17 (g… view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: An example of a pixel-by-pixel analysis of the H [PITH_FULL_IMAGE:figures/full_fig_p005_4.png]
Figure 5
Figure 5. Figure 5: Examples of galaxies classified as early- and late-type using images from the DESI Legacy Imaging Surveys. From left to [PITH_FULL_IMAGE:figures/full_fig_p006_5.png]
Figure 6
Figure 6. Figure 6: Concentration versus Asymmetry diagram (top panel) and Gini versus M20 diagram (bottom panel) for 77 Hα+[N II] emitters in the Fornax cluster. The black solid line in the top panel delineates the morphological transition zone boundaries, where the disturbed galaxies li…
Figure 7
Figure 7. Figure 7: Spatial distribution of the Fornax members around NGC 1399 (cyan star) color-coded by radial velocity [PITH_FULL_IMAGE:figures/full_fig_p008_7.png]
Figure 9
Figure 9. Figure 9: Color magnitude relation for Fornax members, with the [PITH_FULL_IMAGE:figures/full_fig_p009_9.png]
Figure 10
Figure 10. Figure 10: Color (g − r) and stellar mass as function of projected distance from NGC 1399 for Hα+[N II] emitters. The galaxy with higher stellar mass located at ∼ 1.8 Rvir is the central galaxy of the group Fornax A. LTG are represented as squares, whereas ETG are denoted as tri…
Figure 11
Figure 11. Figure 11: Spatial distribution of simulated galaxies in the Fornax-like system present in IllustrisTNG-50. [PITH_FULL_IMAGE:figures/full_fig_p012_11.png]
Figure 12
Figure 12. Figure 12: Evidence of misaligned star formation rate for satellite galaxies from the Fornax-like cluster in IllustrisTNG-50. The [PITH_FULL_IMAGE:figures/full_fig_p013_12.png]

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Reference graph

Works this paper leans on

132 extracted references · 55 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]

    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

  4. [4]

    M., McCarthy , I

    Bah \'e , Y. M., McCarthy , I. G., Balogh , M. L., & Font , A. S. 2013, , 430, 3017

    2013

  5. [5]

    L., Morris , S

    Balogh , M. L., Morris , S. L., Yee , H. K. C., Carlberg , R. G., & Ellingson , E. 1999, , 527, 54

    1999

  6. [6]

    L., van der Burg , R

    Balogh , M. L., van der Burg , R. F. J., Muzzin , A., et al. 2021, , 500, 358

    2021

  7. [7]

    C., Cooper , M

    Baxter , D. C., Cooper , M. C., Balogh , M. L., et al. 2022, , 515, 5479

    2022

  8. [8]

    2014, arXiv e-prints, arXiv:1403.5237

    Benitez , N., Dupke , R., Moles , M., et al. 2014, arXiv e-prints, arXiv:1403.5237

    arXiv 2014

Show all 132 references
  1. [9]

    P., Jord \'a n , A., Mei , S., et al

    Blakeslee , J. P., Jord \'a n , A., Mei , S., et al. 2009, , 694, 556

    2009

  2. [10]

    2014, , 570, A69

    Boselli , A., Voyer , E., Boissier , S., et al. 2014, , 570, A69

    2014

  3. [11]

    2020, , 639, A136

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

    2020

  4. [12]

    & Copin , Y

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

    2003

  5. [13]

    N., van Dokkum , P

    Cardamone , C. N., van Dokkum , P. G., Urry , C. M., et al. 2010, , 189, 270

    2010

  6. [14]

    J., Moles , M., Crist \'o bal-Hornillos , D., et al

    Cenarro , A. J., Moles , M., Crist \'o bal-Hornillos , D., et al. 2019, , 622, A176

    2019

  7. [15]

    2003, , 115, 763

    Chabrier , G. 2003, , 115, 763

    2003

  8. [16]

    Chevance , M., Kruijssen , J. M. D., Hygate , A. P. S., et al. 2020, , 493, 2872

    2020

  9. [17]

    1988, , 203, L9

    Combes , F., Dupraz , C., Casoli , F., & Pagani , L. 1988, , 203, L9

    1988

  10. [18]

    Conselice , C. J. 2003, , 147, 1

    2003

  11. [19]

    O., Kasliwal , M

    Cook , D. O., Kasliwal , M. M., Van Sistine , A., et al. 2019, , 880, 7

    2019

  12. [20]

    M., Arag \'o n-Salamanca , A., & Zaritsky , D

    De Lucia , G., Weinmann , S., Poggianti , B. M., Arag \'o n-Salamanca , A., & Zaritsky , D. 2012, , 423, 1277

    2012

  13. [21]

    J., Lang , D., et al

    Dey , A., Schlegel , D. J., Lang , D., et al. 2019, , 157, 168

    2019

  14. [22]

    2009, , 399, 497

    Dolag , K., Borgani , S., Murante , G., & Springel , V. 2009, , 399, 497

    2009

  15. [23]

    2020, arXiv e-prints, arXiv:2008.00004

    Donnari , M., Pillepich , A., Nelson , D., et al. 2020, arXiv e-prints, arXiv:2008.00004

    2020 arXiv

  16. [24]

    1980, , 236, 351

    Dressler , A. 1980, , 236, 351

    1980

  17. [25]

    J., Gregg , M

    Drinkwater , M. J., Gregg , M. D., & Colless , M. 2001, , 548, L139

    2001

  18. [26]

    2020 a , , 637, A26

    Fahrion , K., Lyubenova , M., Hilker , M., et al. 2020 a , , 637, A26

    2020

  19. [27]

    2020 b , , 637, A27

    Fahrion , K., Lyubenova , M., Hilker , M., et al. 2020 b , , 637, A27

    2020

  20. [28]

    2019, , 484, 2212

    Fossati , M., Fumagalli , M., Gavazzi , G., et al. 2019, , 484, 2212

    2019

  21. [29]

    A., Peterson , J

    Frank , K. A., Peterson , J. R., Andersson , K., Fabian , A. C., & Sanders , J. S. 2013, , 764, 46

    2013

  22. [30]

    S., Ajiki , M., Shioya , Y., et al

    Fujita , S. S., Ajiki , M., Shioya , Y., et al. 2003, , 125, 13

    2003

  23. [31]

    E., Smail , I., Best , P

    Geach , J. E., Smail , I., Best , P. N., et al. 2008, , 388, 1473

    2008

  24. [32]

    Gill , S. P. D., Knebe , A., & Gibson , B. K. 2005, , 356, 1327

    2005

  25. [33]

    & Haynes , M

    Giovanelli , R. & Haynes , M. P. 1983, , 88, 881

    1983

  26. [34]

    2004, , 128, 2652

    Glazebrook , K., Tober , J., Thomson , S., Bland-Hawthorn , J., & Abraham , R. 2004, , 128, 2652

    2004

  27. [35]

    Gunn , J. E. & Gott , J. Richard, I. 1972, , 176, 1

    1972

  28. [36]

    F., Smith Castelli , A

    Haack , R. F., Smith Castelli , A. V., Mendes de Oliveira , C., et al. 2024, , 530, 3195

    2024

  29. [37]

    P., Pereira , M

    Haines , C. P., Pereira , M. J., Smith , G. P., et al. 2015, , 806, 101

    2015

  30. [38]

    P., Pereira , M

    Haines , C. P., Pereira , M. J., Smith , G. P., et al. 2013, , 775, 126

    2013

  31. [39]

    D., Haines , C

    Hern \'a ndez-Fern \'a ndez , J. D., Haines , C. P., Diaferio , A., et al. 2014, , 438, 2186

    2014

  32. [40]

    Hernandez-Jimenez , J. A. & Krabbe , A. C. 2022, Astromorphlib: Python scripts to analyze the morphology of isolated and interacting galaxies

    2022

  33. [41]

    R., Almeida-Fernandes , F., Oliveira Schwarz , G

    Herpich , F. R., Almeida-Fernandes , F., Oliveira Schwarz , G. B., et al. 2024, , 689, A249

    2024

  34. [42]

    2014, , 444, 2938

    Hirschmann , M., De Lucia , G., Wilman , D., et al. 2014, , 444, 2938

    2014

  35. [43]

    1995, , 303, 361

    Horellou , C., Casoli , F., & Dupraz , C. 1995, , 303, 361

    1995

  36. [44]

    2024, , 965, L24

    Hou , M., Hu , Z., & Li , Z. 2024, , 965, L24

    2024

  37. [45]

    2016, , 820, 42

    Iodice , E., Capaccioli , M., Grado , A., et al. 2016, , 820, 42

    2016

  38. [46]

    2019 a , , 627, A136

    Iodice , E., Sarzi , M., Bittner , A., et al. 2019 a , , 627, A136

    2019

  39. [47]

    2017, , 839, 21

    Iodice , E., Spavone , M., Capaccioli , M., et al. 2017, , 839, 21

    2017

  40. [48]

    2019 b , , 623, A1

    Iodice , E., Spavone , M., Capaccioli , M., et al. 2019 b , , 623, A1

    2019

  41. [49]

    J \'a chym , P., Sun , M., Kenney , J. D. P., et al. 2017, , 839, 114

    2017

  42. [50]

    A., Shane , N

    James , P. A., Shane , N. S., Knapen , J. H., Etherton , J., & Percival , S. M. 2005, , 429, 851

    2005

  43. [51]

    1997, , 482, 143

    Jones , C., Stern , C., Forman , W., et al. 1997, , 482, 143

    1997

  44. [52]

    M., White , S

    Kauffmann , G., Heckman , T. M., White , S. D. M., et al. 2003, , 341, 33

    2003

  45. [53]

    A., Salzer , J

    Kellar , J. A., Salzer , J. J., Wegner , G., Gronwall , C., & Williams , A. 2012, , 143, 145

    2012

  46. [54]

    Kenney , J. D. P., Rubin , V. C., Planesas , P., & Young , J. S. 1995, , 438, 135

    1995

  47. [55]

    A., Malhotra , S., Rhoads , J

    Khostovan , A. A., Malhotra , S., Rhoads , J. E., et al. 2020, , 493, 3966

    2020

  48. [56]

    M., et al

    Kleiner , D., Serra , P., Maccagni , F. M., et al. 2021, , 648, A32

    2021

  49. [57]

    C., Hernandez-Jimenez , J

    Krabbe , A. C., Hernandez-Jimenez , J. A., Mendes de Oliveira , C., et al. 2024, , 528, 1125

    2024

  50. [58]

    A., Schinnerer , E., et al

    Kreckel , K., Blanc , G. A., Schinnerer , E., et al. 2016, , 827, 103

    2016

  51. [59]

    Kron , R. G. 1980, , 43, 305

    1980

  52. [60]

    A., Gal \'a n-de Anta , P

    Lara-L \'o pez , M. A., Gal \'a n-de Anta , P. M., Sarzi , M., et al. 2022, , 660, A105

    2022

  53. [61]

    2021, , 648, A31

    Loni , A., Serra , P., Kleiner , D., et al. 2021, , 648, A31

    2021

  54. [62]

    Lopes , P. A. A., Ribeiro , A. L. B., & Brambila , D. 2024, , 527, L19

    2024

  55. [63]

    M., Davis , M., Faber , S

    Lotz , J. M., Davis , M., Faber , S. M., et al. 2008, , 672, 177

    2008

  56. [64]

    M., Primack , J., & Madau , P

    Lotz , J. M., Primack , J., & Madau , P. 2004, , 128, 163

    2004

  57. [65]

    I., Mosia , K., Serra , P., et al

    Loubser , S. I., Mosia , K., Serra , P., et al. 2024, , 527, 7158

    2024

  58. [66]

    C., Dale , D

    Ly , C., Lee , J. C., Dale , D. A., et al. 2011, , 726, 109

    2011

  59. [67]

    M., Murgia , M., Serra , P., et al

    Maccagni , F. M., Murgia , M., Serra , P., et al. 2020, , 634, A9

    2020

  60. [68]

    2019, , 490, 1666

    Maddox , N., Serra , P., Venhola , A., et al. 2019, , 490, 1666

    2019

  61. [69]

    A., & Raychaudhury , S

    Mahajan , S., Mamon , G. A., & Raychaudhury , S. 2011, , 416, 2882

    2011

  62. [70]

    2014, , 570, A13

    Makarov , D., Prugniel , P., Terekhova , N., Courtois , H., & Vauglin , I. 2014, , 570, A13

    2014

  63. [71]

    2018, , 480, 5113

    Marinacci , F., Vogelsberger , M., Pakmor , R., et al. 2018, , 480, 5113

    2018

  64. [72]

    L., Balogh , M

    McGee , S. L., Balogh , M. L., Bower , R. G., Font , A. S., & McCarthy , I. G. 2009, , 400, 937

    2009

  65. [73]

    L., van der Burg , R

    McNab , K., Balogh , M. L., van der Burg , R. F. J., et al. 2021, , 508, 157

    2021

  66. [74]

    2019, , 489, 241

    Mendes de Oliveira , C., Ribeiro , T., Schoenell , W., et al. 2019, , 489, 241

    2019

  67. [75]

    B., Steiner , J

    Menezes , R. B., Steiner , J. E., & Ricci , T. V. 2014, , 438, 2597

    2014

  68. [76]

    Moles , M., Ben \' tez , N., Aguerri , J. A. L., et al. 2008, , 136, 1325

    2008

  69. [77]

    2022, , 263, 40

    Morokuma-Matsui , K., Bekki , K., Wang , J., et al. 2022, , 263, 40

    2022

  70. [78]

    M., et al

    Morokuma-Matsui , K., Serra , P., Maccagni , F. M., et al. 2019, , 71, 85

    2019

  71. [79]

    Muzzin , A., van der Burg , R. F. J., McGee , S. L., et al. 2014, , 796, 65

    2014

  72. [80]

    G., de Freitas Pacheco , J

    Nasonova , O. G., de Freitas Pacheco , J. A., & Karachentsev , I. D. 2011, , 532, A104

    2011

  73. [81]

    2019, , 490, 3234

    Nelson , D., Pillepich , A., Springel , V., et al. 2019, , 490, 3234

    2019

  74. [82]

    2018, , 475, 624

    Nelson , D., Pillepich , A., Springel , V., et al. 2018, , 475, 624

    2018

  75. [83]

    Oman , K. A. & Hudson , M. J. 2016, , 463, 3083

    2016

  76. [84]

    A., Padilla , N

    Pallero , D., G \'o mez , F. A., Padilla , N. D., et al. 2022, , 511, 3210

    2022

  77. [85]

    A., Padilla , N

    Pallero , D., G \'o mez , F. A., Padilla , N. D., et al. 2019, , 488, 847

    2019

  78. [86]

    2007, , 119, 30

    Pascual , S., Gallego , J., & Zamorano , J. 2007, , 119, 30

    2007

  79. [87]

    2019, , 484, 1702

    Pasquali , A., Smith , R., Gallazzi , A., et al. 2019, , 484, 1702

    2019

  80. [88]

    2022, , 511, 5180

    Pedrini , A., Fossati , M., Gavazzi , G., et al. 2022, , 511, 5180

    2022

  81. [89]

    G., Cava , A., Barro , G., et al

    P \'e rez-Gonz \'a lez , P. G., Cava , A., Barro , G., et al. 2013, , 762, 46

    2013

  82. [90]

    2018, , 475, 648

    Pillepich , A., Nelson , D., Hernquist , L., et al. 2018, , 475, 648

    2018

  83. [91]

    2019, , 490, 3196

    Pillepich , A., Nelson , D., Springel , V., et al. 2019, , 490, 3196

    2019

  84. [92]

    2019 a , , 625, A95

    Pinna , F., Falc \'o n-Barroso , J., Martig , M., et al. 2019 a , , 625, A95

    2019

  85. [93]

    2019 b , , 623, A19

    Pinna , F., Falc \'o n-Barroso , J., Martig , M., et al. 2019 b , , 623, A19

    2019

  86. [94]

    M., Lyubenova , M., et al

    Poci , A., McDermid , R. M., Lyubenova , M., et al. 2021, , 647, A145

    2021

  87. [95]

    A., Iodice , E., Napolitano , N

    Raj , M. A., Iodice , E., Napolitano , N. R., et al. 2020, , 640, A137

    2020

  88. [96]

    A., Iodice , E., Napolitano , N

    Raj , M. A., Iodice , E., Napolitano , N. R., et al. 2019, , 628, A4

    2019

  89. [97]

    2017, , 843, 128

    Rhee , J., Smith , R., Choi , H., et al. 2017, , 843, 128

    2017

  90. [98]

    F., Lotz , J

    Rodriguez-Gomez , V., Snyder , G. F., Lotz , J. M., et al. 2019, , 483, 4140

    2019

  91. [99]

    F., Aguerri , J

    Romero-G \'o mez , J., Peletier , R. F., Aguerri , J. A. L., & Smith , R. 2024, , 689, A40

    2024

  92. [100]

    A., Milone , A

    Rosa , D. A., Milone , A. C., Krabbe , A. C., & Rodrigues , I. 2018, , 363, 131

    2018

  93. [101]

    J., Carr , D

    Salzer , J. J., Carr , D. J., Sieben , J., Brunker , S. W., & Hirschauer , A. S. 2023, , 166, 81

    2023

  94. [102]

    M., de Carvalho , R

    Sampaio , V. M., de Carvalho , R. R., Arag \'o n-Salamanca , A., et al. 2024, , 532, 982

    2024

  95. [103]

    2018, , 616, A121

    Sarzi , M., Iodice , E., Coccato , L., et al. 2018, , 616, A121

    2018

  96. [104]

    A., Zurek , D

    Scharf , C. A., Zurek , D. R., & Bureau , M. 2005, , 633, 154

    2005

  97. [105]

    M., Kleiner , D., et al

    Serra , P., Maccagni , F. M., Kleiner , D., et al. 2019, , 628, A122

    2019

  98. [106]

    V., Cortesi , A., Haack , R

    Smith Castelli , A. V., Cortesi , A., Haack , R. F., et al. 2024, , 530, 3787

    2024

  99. [107]

    N., Geach , J

    Sobral , D., Best , P. N., Geach , J. E., et al. 2009, , 398, 75

    2009

  100. [108]

    2022, , 663, A135

    Spavone , M., Iodice , E., D'Ago , G., et al. 2022, , 663, A135

    2022

  101. [109]

    2020, , 639, A14

    Spavone , M., Iodice , E., van de Ven , G., et al. 2020, , 639, A14

    2020

  102. [110]

    S., Suess , K

    Spilker , J. S., Suess , K. A., Setton , D. J., et al. 2022, , 936, L11

    2022

  103. [111]

    W., Sarzi , M., Gal \'a n-de Anta , P

    Spriggs , T. W., Sarzi , M., Gal \'a n-de Anta , P. M., et al. 2021, , 653, A167

    2021

  104. [112]

    W., Sarzi , M., Napiwotzki , R., et al

    Spriggs , T. W., Sarzi , M., Napiwotzki , R., et al. 2020, , 637, A62

    2020

  105. [113]

    2018, , 475, 676

    Springel , V., Pakmor , R., Pillepich , A., et al. 2018, , 475, 676

    2018

  106. [114]

    Springel , V., White , S. D. M., Tormen , G., & Kauffmann , G. 2001, , 328, 726

    2001

  107. [115]

    H., Salo , H., Janz , J., et al

    Su , A. H., Salo , H., Janz , J., et al. 2021, , 647, A100

    2021

  108. [116]

    Taniguchi , Y., Kajisawa , M., Kobayashi , M. A. R., et al. 2015, , 67, 104

    2015

  109. [117]

    N., Hopkins , A

    Taylor , E. N., Hopkins , A. M., Baldry , I. K., et al. 2011, , 418, 1587

    2011

  110. [118]

    R., et al

    Thain \'a -Batista , J., Cid Fernandes , R., Herpich , F. R., et al. 2023, , 526, 1874

    2023

  111. [119]

    van der Burg , R. F. J., Rudnick , G., Balogh , M. L., et al. 2020, , 638, A112

    2020

  112. [120]

    2018, , 620, A165

    Venhola , A., Peletier , R., Laurikainen , E., et al. 2018, , 620, A165

    2018

  113. [121]

    2019, , 625, A143

    Venhola , A., Peletier , R., Laurikainen , E., et al. 2019, , 625, A143

    2019

  114. [122]

    2017, , 608, A142

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

    2017

  115. [123]

    F., Salo , H., et al

    Venhola , A., Peletier , R. F., Salo , H., et al. 2022, , 662, A43

    2022

  116. [124]

    2015, , 580, A47

    Vilella-Rojo , G., Viironen , K., L \'o pez-Sanjuan , C., et al. 2015, , 580, A47

    2015

  117. [125]

    2009, , 496, 669

    Vollmer , B., Soida , M., Chung , A., et al. 2009, , 496, 669

    2009

  118. [126]

    J., Webster , R

    Waugh , M., Drinkwater , M. J., Webster , R. L., et al. 2002, , 337, 641

    2002

  119. [127]

    Wetzel , A. R. 2011, , 412, 49

    2011

  120. [128]

    R., Tinker , J

    Wetzel , A. R., Tinker , J. L., Conroy , C., & van den Bosch , F. C. 2013, , 432, 336

    2013

  121. [129]

    W., et al

    Wolf , C., Meisenheimer , K., Rix , H. W., et al. 2003, , 401, 73

    2003

  122. [130]

    J., Lagos , C

    Wright , R. J., Lagos , C. d. P., Davies , L. J. M., et al. 2018, ArXiv e-prints [ [arXiv] 1810.07335 ]

    2018 arXiv

  123. [131]

    A., Smith , M

    Zabel , N., Davis , T. A., Smith , M. W. L., et al. 2019, , 483, 2251

    2019

  124. [132]

    I., Zaritsky , D., Lin , H., et al

    Zabludoff , A. I., Zaritsky , D., Lin , H., et al. 1996, , 466, 104

    1996

Pith tools

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