Pith. sign in

REVIEW 4 major objections 6 minor 167 references

From Voids to Clusters: Mergers and Evolutionary Pathways of Star-Forming and Quenched Low-Mass Galaxies

T0 review · 4 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

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

Pith's one-line read Quenched low-mass galaxies in voids undergo roughly three times as many late-time mini mergers as their cluster counterparts, marking a distinct evolutionary pathway.

desk verdict Useful first census of merger types for low-mass galaxies in voids vs clusters, but the headline quenched-void mini-merger excess is resolution-limited and rests on a small sample. read the letter →

arxiv 2506.06711 v2 pith:RYT77MI3 submitted 2025-06-07 astro-ph.GA

Mohammad Reza Shojaei , Saeed Tavasoli , Parsa Ghafour This is my paper
classification astro-ph.GA
keywords low-massgalaxiesgalaxymergerscosmicvoidsclustersquenchingIllustrisTNGmergermassratiosstarformation
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 the merger histories of low-mass galaxies are set by both environment and star-formation state, and that the smallest mergers matter most in the emptiest regions. Using the TNG300-1 cosmological simulation, it splits low-mass galaxies ($10^{8.5}\le M_\star/M_\odot\le 10^{10.5}$) into star-forming and quenched populations in voids and clusters and tracks mini, minor, and major mergers over the last $\sim10.5$ Gyr. The headline result is a late-time surge: quenched void galaxies experience about three times as many mini and minor mergers as their cluster counterparts, while star-forming void galaxies show only a modest boost. If correct, this overturns the simple picture that voids are quiet places for galaxy evolution and instead makes low-density environments the main arena for small-accretion-driven growth.

What carries the argument

The analysis rests on the merger-history catalogues of the TNG300-1 run, with mergers classified by stellar mass ratio into major ($>1/4$), minor ($1/10$–$1/4$), and mini ($<1/10$), and on the void-to-cluster ratio $R$ of cumulative merger fractions across lookback-time bins. The companion-mass statistic MeanStellarMass (the stellar-mass-weighted average secondary mass over the last 8 Gyr) is the device that reveals the bimodality of quenched void galaxies, splitting them into an old low-mass-accretion pathway and a younger higher-mass-merger pathway. Environment is defined by a void finder applied to the density field and by cluster-centric radius $<3R_{200}$ around halos above $10^{13}\,M_\odot$, and star-forming versus quenched status is assigned by both sSFR and UVJ cuts at $z=0$.

What would settle it

Re-run the same merger-fraction analysis at higher resolution (for example TNG50-1, which has roughly ten times better mass resolution) for the same stellar-mass range and look-back bins, and check whether the void-to-cluster mini-merger ratio at late times stays near $R\sim3$; if it collapses toward unity, the central environmental contrast is a resolution artifact. The equivalent observational check is to count resolved low-mass companions around quenched void and cluster galaxies in deep surveys and compare the counts.

Watch

Extended reading notes

Core claim

On its own terms, the paper establishes that environment and quenching state jointly control the assembly of low-mass galaxies ($10^{8.5}\le M_\star/M_\odot\le 10^{10.5}$). The central discovery is that quenched galaxies in voids show dramatically elevated late-time mini and minor merger fractions, with void-to-cluster ratios $R\sim3.0$–$3.3$ for mini and $R\sim2.7$–$2.9$ for minor mergers, while star-forming galaxies show only moderate recent enhancement ($R\sim1.6$–$1.8$) and at intermediate epochs the pattern reverses for quenched cluster galaxies ($R\sim0.6$–$0.8$). The paper also finds that quenched void galaxies are not a single population: the mean mass of merger companions is bimodal, tracing an older pathway built from early low-mass accretion and a younger pathway with more recent, higher-mass mergers. It further shows that mini mergers are the most effective channel for boosting star formation rate and efficiency across all environments, whereas major mergers dominate the gas fractions of low-mass galaxies, and that mergers barely affect already-quenched systems.

Load-bearing premise

The results assume the simulation's tracking reliably recovers very small companion galaxies, down to a few star particles, so the high mini-merger counts in voids are real rather than a by-product of limited resolution.

Editorial extensions

If this is right

  • Late-time assembly of low-mass galaxies is dominated by small accretion events, not just major mergers, so models of low-mass growth must include mini mergers as a primary channel.
  • Quenched galaxies in voids are not uniformly dead: a subpopulation is being assembled recently through relatively higher-mass mergers, alongside an older population built from early low-mass accretion.
  • Merger-triggered star formation is effective only in gas-rich star-forming systems; quenched galaxies show no measurable SFR, SFE, or gas-fraction response to mergers, implying gas content gates merger-driven star formation.
  • The reversal of the void–cluster merger ratio at intermediate epochs indicates that group and cluster assembly were themselves sites of enhanced merger activity for quenched galaxies.

Reading between the lines

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

  • A testable prediction: deep imaging of quenched void galaxies should reveal an excess of very low-mass companions or tidal debris relative to quenched cluster galaxies, mirroring the simulated $R\sim3$ mini-merger contrast.
  • The bimodality in quenched void galaxies predicts two distinct stellar-population age patterns—uniformly old stars in the low-mass-accretion path and a younger population with a recent accretion-triggered burst in the high-mass-merger path.
  • A resolution-convergence test in a higher-resolution run (TNG50-1) that drives the late-time mini-merger ratio toward unity would show the void–cluster contrast to be partly a numerical artifact.
  • The absence of merger effects on quenched galaxies argues that semi-analytic models should make merger-driven star formation depend on the gas fraction of the remnant, not just on merger mass ratio.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 6 minor

Summary. This manuscript analyzes low-mass galaxies (10^8.5 <= Mstar/Msun <= 10^10.5) in the TNG300-1 simulation, comparing star-forming and quenched galaxies in voids versus groups/clusters. Using the Rodriguez-Gomez et al. (2017) and Eisert et al. (2023) merger catalogs, it tracks the last ~10.5 Gyr of evolution, splits mergers into major, minor, and mini classes, mass-matches the four environmental/star-formation samples, and examines merger fractions, merger timescales, companion mass distributions, and the impact of mergers on SFR, SFE, and gas fraction. The headline result is a strong late-time environmental contrast for quenched galaxies: void quenched galaxies show roughly three times more mini and minor mergers than cluster quenched galaxies (R~3.0-3.3 and R~2.7-2.9 in Figure 9), while star-forming galaxies show a more moderate enhancement (R~1.6-1.8). The paper also reports earlier assembly for quenched systems, a bimodal mean merger companion mass for quenched void galaxies, and environment-dependent merger effects on star formation and gas content.

Significance. If the central claims survive scrutiny, this would be a valuable step: it is a first statistical census of mini/minor/major merger histories for low-mass galaxies separately in void and cluster environments, using a publicly available large-volume simulation. The authors make good use of existing merger-tree catalogs, apply explicit mass-matching before environmental comparisons, and separate the analysis by merger mass ratio, galaxy type, and time bin. The distinction between mini and minor mergers, and the emphasis on voids, goes beyond most previous work and could motivate new observational and simulation-based tests. However, the headline void/cluster contrast for quenched galaxies rests on small samples and on merger events whose companion masses are very close to the TNG300-1 resolution limit, so the quantitative ratios in Figure 9 are not yet established at the level the conclusions claim.

major comments (4)
  1. [Section 2.3.2 and Section 2.3.3] The sample construction explicitly excludes galaxies with SFR=0: Section 2.3.2 states "we exclude galaxies without star formation (SFR=0)" for clusters, and Section 2.3.3 describes the void sample as containing galaxies "with SFR,0" (presumably SFR not equal to zero). This removes the most strongly quenched systems from the quenched sample, biasing it toward galaxies with residual star formation. Because the paper's central comparison is between star-forming and quenched populations, and because the largest claimed environmental contrast (Figure 9, R~3 for quenched galaxies) concerns exactly these quenched systems, this exclusion is load-bearing. The authors should either justify why SFR=0 galaxies are excluded, or repeat the analysis including them (for example, with a finite sSFR floor) to show that the qualitative results are unchanged.
  2. [Section 3.4.1, Figure 9, and Section 2.1] The headline mini-merger ratios for quenched galaxies (R~3.0-3.3 in the [0-5] Gyr bin) rely on recovering mergers with secondary stellar masses an order of magnitude below the primary. For a primary at the sample's low-mass edge of 10^8.5 Msun, a mini merger (mass ratio <1/10) involves a companion below ~3.2x10^7 Msun, i.e. only about three TNG300-1 stellar particles (m_bary=1.1x10^7 Msun, Section 2.1). Minor mergers are similarly unresolved below roughly 10^9 Msun primaries. The resolution floor is also environment-dependent: tidal stripping in clusters can destroy or strip low-mass companions before coalescence, selectively suppressing the cluster mini/minor counts and artificially inflating the void/cluster ratio. The caveat in Section 3.5 that "absolute values at the low-mass end may be affected by resolution limitations" is stated for the mean-merger-mass bimodality, not for the Figure 9 ratios, and the claim that "the relative separation between the two subpopulations... remain[s] robust" does not cover the environmental R statistic. To support the central claim, the authors should repeat the ratio analysis using only higher-mass primaries (e.g., Mstar > 10^9 Msun) or otherwise demonstrate that the void/cluster mini-merger contrast is not a resolution artifact.
  3. [Section 3.4.1 and Table 1] After mass matching, the quenched void sample contains only 153 galaxies (Section 3.4), and the Figure 9 ratio for quenched mini mergers in the [0-5] Gyr bin is based on a small absolute number of events. The quoted "propagated 1-sigma uncertainties" are not shown in the main text, and the number of mini-merger events per environment and time bin is not reported. Given the small sample, a difference of only a few cluster events could change R by order unity. The authors should report the actual event counts and confidence intervals for the quenched panels of Figure 9, so the reader can assess whether R~3 is statistically distinguishable from R~1.
  4. [Section 4, final paragraph] The concluding paragraph states that "quenched galaxies in voids typically reside in more massive dark matter haloes and experience fewer recent mergers—particularly major ones—reducing their ability to replenish their gas reservoirs." This is internally inconsistent with the paper's own main result: Figure 9 and conclusion item (5) report that quenched void galaxies undergo far more mini and minor mergers at late times (R~3.0-3.3 and R~2.7-2.9). If the intended statement is restricted to major mergers only, it should say so explicitly; as written, it contradicts the central quantitative finding and will confuse readers.
minor comments (6)
  1. [Section 2.3.3] The phrase "with SFR,0" appears to be a typographical rendering of "SFR not equal to 0"; please write this explicitly.
  2. [Section 3.4.1 and Figure 9] The shaded uncertainty regions described in the text are not visible or reproduced in the main text; consider adding a version of Figure 9 with explicit error bars or event counts, especially for the quenched panels.
  3. [Section 3.5] The definitions of MeanStellarMass, MeanLookbackTime, and AccretedStellarMass appear only in footnotes; moving these definitions to the methods section would improve clarity.
  4. [Section 2.1] The notation for the simulation is inconsistent (TNG300_1 in Section 2.1, TNG300 elsewhere); please standardize.
  5. [Section 3.2] In the text near Figure 5, "relatively by Stellar feedback" appears to be missing words; the sentence should be rephrased.
  6. [Section 3.6] The statement that mergers have "little to no impact on quenched galaxies" is based on z<1 merger incidence and z=0 properties; because the quenched classification is made at z=0, transient merger-induced effects at earlier epochs may be missed. A sentence acknowledging this selection effect would help.

Circularity Check

1 steps flagged · score 4.0 of 10

Central merger-rate comparison is self-contained; secondary claim that mergers do not affect quenched galaxies is partly an artifact of the sSFR selection.

  1. self definitional [Sec. 2.3.5 + Sec. 3.6 (Figs. 12, 13)]
    "In the literature, we commonly define "quenched" galaxies as those whose logarithmic Specific Star Formation Rate (sSFR) falls below a certain fixed threshold at any redshift, namely sSFR≤10−11 yr−1 ... our analysis reveals no significant differences between mergers and non-mergers in the properties of quenched galaxies in both environments suggesting that once star formation has ceased, mergers do not substantially modify their star-forming properties."

    The quenched sample is defined by an sSFR threshold at z=0, so every member has SFR/Mstar below 10^-11 yr^-1 by construction. Comparing the SFR distributions of merger and non-merger subsamples inside this population therefore cannot reveal whether mergers enhance SFR: any merger that pushed SFR above the threshold at z=0 would have excluded the galaxy from the sample. The reported null SFR result is thus inherited from the selection rule rather than measured from merger physics. The SFE and gas-fraction comparisons are less constrained by the definition, but the broad statement that mergers do not substantially modify quenched galaxies leans on the SFR comparison and is presented as an empirical conclusion.

full rationale

The paper's headline result, that void quenched galaxies experience about three times more late-time mini mergers than cluster quenched galaxies (R~3.0-3.3), is not circular: the void/cluster environment assignment and the merger-tree catalogs (Rodriguez-Gomez et al. 2017; Eisert et al. 2023) are independent of the z=0 sSFR/UVJ classification, and the samples are mass-matched before computing merger fractions. The assembly histories, merger-fraction ratios, and mean-companion-mass distributions are all measured quantities that could in principle have come out differently. The only reduction found is the secondary claim in Section 3.6 that mergers have little effect on quenched galaxies: because 'quenched' is defined by an sSFR cutoff, an SFR comparison inside that sample is partly closed by selection. This does not undermine the main environmental merger-rate comparison, but the 'little to no impact' conclusion should be understood as partly definitional rather than a fully independent discovery. The TNG300 resolution floor near 10^8.5 Msun is a real correctness risk for the mini-merger ratios, especially with only 153 quenched void galaxies after mass matching, but that is a numerical validity concern, not circularity.

Assumptions & free parameters 7 free parameters · 4 assumptions · 0 invented entities

The central claims rest on hand-chosen classification thresholds, a public simulation with finite resolution, and pre-built merger catalogs. No new physical entities are introduced. The free parameters are mostly threshold choices from the literature or from the simulation's resolution limits, but their specific values affect the sample sizes and the reported merger ratios.

free parameters (7)
  • sSFR quenching threshold = 10^-11 yr^-1
    Fixed threshold from literature (McGee et al. 2011; Wetzel et al. 2013) used to split quenched versus star-forming; choice affects sample sizes (516 quenched voids by sSFR, 250 after UVJ).
  • UVJ quiescent selection lines = U-V > 0.88(V-J)+0.85 and U-V > 1.3, V-J < 1.6
    Adopted from Donnari et al. 2019 and Whitaker et al. 2011; these cuts define the final quenched sample, which shrinks from 516 to 250 void galaxies.
  • Stellar mass range = 10^8.5 to 10^10.5 Msun
    Lower limit set by TNG300 resolution; upper limit selects the low-mass regime and excludes mass-quenched galaxies.
  • Merger mass ratio boundaries = major >1/4, minor 1/10 to 1/4, mini <1/10
    Standard thresholds from Rodriguez-Gomez et al. 2017 and Eisert et al. 2023; the paper's central mini-merger claims depend on this boundary.
  • Void finder density threshold and minimum radius = R_v > 7 Mpc, density contrast threshold not specified
    AM void finder parameters are tunable; the paper does not state the density threshold used, so void membership depends on an unspecified choice.
  • Cluster selection thresholds = M200 >= 1e13 Msun, R < 3 R200, at least 10 galaxies per halo
    Chosen to define dense environments; results may depend on these radius and mass cuts.
  • Mass-matching bin width and downsampling = 0.1 dex bins, random downsampling, no seed given
    Used to equalize stellar-mass distributions across four samples; downsampling reduces quenched void sample to 153 galaxies.
assumptions (4)
  • domain assumption IllustrisTNG300-1 provides a sufficiently realistic model of low-mass galaxy formation and quenching.
    The paper's entire analysis uses TNG300-1 outputs (Section 2.1) without validation against observed merger rates in this mass range.
  • domain assumption The merger history catalogs (Rodriguez-Gomez et al. 2017; Eisert et al. 2023) correctly identify all mergers and secondary stellar masses, including mini mergers.
    Central claims on mini, minor, and major merger fractions rely on these catalogs (Sections 2.2 and 3.4).
  • domain assumption The AM void finder with the chosen parameters recovers reliable voids and their galaxy membership.
    Void galaxies are defined by the AM algorithm (Section 2.3.3); threshold values are not fully specified.
  • ad hoc to paper Selection at z=0 on quenched or star-forming status does not bias backward merger histories.
    The paper classifies galaxies at z=0 and tracks them backward; the exclusion of SFR=0 galaxies and progenitor bias are not corrected (Sections 2.3 and 3.6).

how reviews work

0 comments
Cite this review

Pith. "Pith review of From Voids to Clusters: Mergers and Evolutionary Pathways of Star-Forming and Quenched Low-Mass Galaxies." pith.science (2026). https://pith.science/paper/RYT77MI3

@misc{pith2026250606711,
  author       = {Pith},
  title        = {Pith review of: From Voids to Clusters: Mergers and Evolutionary Pathways of Star-Forming and Quenched Low-Mass Galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/RYT77MI3}},
  note         = {Machine review of arXiv:2506.06711}
}
abstract

The evolution of low-mass galaxies is shaped by both internal processes and environmental factors, yet the role of environment and mergers in regulating their growth and star formation rates remains poorly understood, especially in the low-density regime. This study aims to compare the evolutionary pathways and merger histories of star-forming and quenched galaxies in dense (cluster) and under-dense (void) environments, focusing on galaxies with stellar masses in the range $10^{8.5} \leq M_\star/M_\odot \leq 10^{10.5}$. It presents the first statistical analysis within this stellar mass range, explicitly distinguishing between mini, minor, and major mergers across varying environments. Using the high-resolution TNG300-1 simulation from the IllustrisTNG project, we classify galaxies as star-forming and quenched based on sSFR and UVJ criteria. We track their physical properties over the last $\sim 10.5$ Gyr ($z < 2$), follow their complete merger histories, distinguishing between major, minor, and mini mergers, and assess the statistical impact of these mergers on star formation and gas content.

Figures

Figures reproduced from arXiv: 2506.06711 by the authors.

Figure 1
Figure 1. Stellar-mass distributions of star-forming and quenched galaxies in void and cluster environments at z = 0 after applying the sSFR and UVJ selection criteria. galaxies. We also use the “Merger History” catalog (Rodriguez￾Gomez et al. 2017) and (Eisert et al. 2023), which contains in￾formation and statistics on the merging history of all subhalos (i.e., galaxies) across time. This paper is organized as follows. Secti… view at source ↗
Figure 2
Figure 2. Distribution of star-forming (green) and quenched (purple) galaxies in groups and clusters (1013 ≤ M200 ≤ 1015 [M⊙]) from the TNG300-1 simulation at z = 0. The x-axis shows R/R200, and the y￾axis shows log M⋆. Histograms depict the distributions of R/R200 and log M⋆[M⊙]. resolution effects in TNG300, we apply a stellar mass cut-off of 108.5M⊙ for the low-mass end of our galaxy sample (Pillepich et al. 2018a). In the… view at source ↗
Figure 3
Figure 3. The UVJ diagram at z = 0 shows the final galaxy samples used in this work: star-forming (blue circles) and quenched (red cir￾cles) galaxies in voids, and star-forming (green triangles) and quenched (purple triangles) galaxies in clusters. The samples are defined by ap￾plying the sSFR and UVJ selection criteria, together with the condition Rcluster-centric < 3R200 for group and cluster galaxies, and restricting the s… view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: Comparative analysis of six key parameters: star formation rates(SFRs), the mass of dark matter (MDM), the mass of gas (Mgas) and the average number density of gas (n), all within twice the half-mass stellar radius for star-forming (blue lines) and quenched (red lines)…
Figure 5
Figure 5. Figure 5: Evolution of star formation rates (SFRs), gas mass (Mgas), stellar mass (Mstar), dark matter mass (MDM) and gas fraction (fgas) within twice the stellar half-mass radius, as a function of lookbacktime ≤ 10.5Gyr (z ≤ 2 ) for star-forming (blue and green) and quenched (r…
Figure 6
Figure 6. Figure 6: Stellar mass assembly histories of star-forming (blue) and quenched (red) galaxies in voids, and star-forming (green) and quenched (purple) galaxies in clusters, shown across four stellar mass bins as a function of lookback time (Gyr). The normalized stellar mass fract…
Figure 7
Figure 7. Figure 7: The normalized histogram of the ex-situ stellar mass fraction (facc) across different galaxy populations, categorized by environment (voids vs. clusters) and star-forming versus quenched galaxies. The small vertical lines indicate the corresponding median values for ea…
Figure 8
Figure 8. Figure 8: Cumulative fraction of galaxies that have experienced at least one merger as a function of lookback time (measured from z = 0), for different stellar mass ratios corresponding to major, minor, and mini mergers for stellar-mass–matched samples. These curves represent th…
Figure 9
Figure 9. Figure 9: Void-to-cluster merger-fraction ratio, R, as a function of lookback time for mini (left), minor (middle), and major (right) mergers for stellar-mass–matched samples, shown separately for all (green), star-forming (blue), and quenched (red) galaxies. The four lookback-t…
Figure 10
Figure 10. Figure 10: Comparison of last major and minor mergers in star-forming and quenched galaxies within voids and clusters, illustrated through box plots of redshift distributions and bar charts displaying absolute differences in redshift (ADR) between star-forming and quenched galax…
Figure 11
Figure 11. Figure 11: Normalized histogram of the log10 mean stellar mass (M⊙) over the last 8 Gyr for the different galaxy populations, categorized by environment (voids vs. clusters) and galaxy type (star-forming vs. quenched). Stars indicate the corresponding median values for each popu…
Figure 12
Figure 12. Figure 12: Histograms comparing the distributions of star formation rate (SFR), star formation efficiency (SFE), and gas fraction (fgas) within the last 8 Gyr (z < 1) for galaxies in void environments. Systems that experienced at least one merger (Mergers ≥ 1) are shown in red a…
Figure 13
Figure 13. Figure 13: Histograms comparing the distributions of star formation rate (SFR), star formation efficiency (SFE), and gas fraction (fgas) within the last 8 Gyr (z < 1) for galaxies in cluster environments. Systems that experienced at least one merger (Mergers ≥ 1) are shown in gr…
Figure 14
Figure 14. Figure 14: Evolution of the star formation rate (SFR; left panels), star formation efficiency (SFE = SFR/Mgas; middle panels), and gas fraction (fgas = Mgas/(M⋆ + Mgas); right panels) as a function of lookback time over the last ∼ 8 Gyr, for star-forming galaxies in void and clu…

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

167 extracted references · 63 canonical work pages

  1. [1]

    & Mähönen, P

    Aikio, J. & Mähönen, P. 1998, The Astrophysical Journal, 497, 534 Argudo-Fernández, M., Hernández, C. G., Verley, S., et al. 2024, Astronomy & Astrophysics, 692, A258

    1998

  2. [2]

    2016, The Astro- physical Journal, 821, 90

    Athanassoula, E., Rodionov, S., Peschken, N., & Lambert, J. 2016, The Astro- physical Journal, 821, 90

    2016

  3. [3]

    Bagla, J. S. 2002, Journal of Astrophysics and Astronomy, 23, 185

    2002

  4. [4]

    M., Loveday, J., & Brunner, R

    Ball, N. M., Loveday, J., & Brunner, R. J. 2008, Monthly Notices of the Royal Astronomical Society, 383, 907

    2008

  5. [5]

    L., McGee, S

    Balogh, M. L., McGee, S. L., Mok, A., et al. 2016, Monthly Notices of the Royal Astronomical Society, 456, 4364

    2016

  6. [6]

    L., Navarro, J

    Balogh, M. L., Navarro, J. F., & Morris, S. L. 2000, The Astrophysical Journal, 540, 113

    2000

  7. [7]

    P., Nichol, R

    Bamford, S. P., Nichol, R. C., Baldry, I. K., et al. 2009, Monthly Notices of the Royal Astronomical Society, 393, 1324

    2009

  8. [8]

    J., Arnold, J

    Barton, E. J., Arnold, J. A., Zentner, A. R., Bullock, J. S., & Wechsler, R. H. 2007, The Astrophysical Journal, 671, 1538

    2007

Show all 167 references
  1. [9]

    H., Hearin, A

    Behroozi, P., Wechsler, R. H., Hearin, A. P., & Conroy, C. 2019, Monthly Notices of the Royal Astronomical Society, 488, 3143

    2019

  2. [10]

    S., Conroy, C., & Wechsler, R

    Behroozi, P. S., Conroy, C., & Wechsler, R. H. 2010, The Astrophysical Journal, 717, 379

    2010

  3. [11]

    S., Wechsler, R

    Behroozi, P. S., Wechsler, R. H., & Conroy, C. 2013, ApJ, 770, 57

    2013

  4. [12]

    J., & Shioya, Y

    Bekki, K., Couch, W. J., & Shioya, Y . 2002, The Astrophysical Journal, 577, 651

    2002

  5. [13]

    F., Naab, T., McIntosh, D

    Bell, E. F., Naab, T., McIntosh, D. H., et al. 2006, The Astrophysical Journal, 640, 241

    2006

  6. [14]

    Benson, A., Hoyle, F., Torres, F., & V ogeley, M. S. 2003, Monthly Notices of the Royal Astronomical Society, 340, 160

    2003

  7. [15]

    R., Eisenstein, D., Hogg, D

    Blanton, M. R., Eisenstein, D., Hogg, D. W., Schlegel, D. J., & Brinkmann, J. 2005, The Astrophysical Journal, 629, 143

    2005

  8. [16]

    F., Conselice, C

    Bluck, A. F., Conselice, C. J., Bouwens, R. J., et al. 2009, Monthly Notices of the Royal Astronomical Society: Letters, 394, L51

    2009

  9. [17]

    Blumenthal, K. A. & Barnes, J. E. 2018, Monthly Notices of the Royal Astro- nomical Society, 479, 3952

    2018

  10. [18]

    P., & Xu, G

    Bode, P., Ostriker, J. P., & Xu, G. 2000, The Astrophysical Journal Supplement Series, 128, 561

    2000

  11. [19]

    R., Kofman, L., & Pogosyan, D

    Bond, J. R., Kofman, L., & Pogosyan, D. 1996, Nature, 380, 603

    1996

  12. [20]

    2022, The Astronomy and astrophysics re- view, 30, 3

    Boselli, A., Fossati, M., & Sun, M. 2022, The Astronomy and astrophysics re- view, 30, 3

    2022

  13. [21]

    M., Popping, G., et al

    Bottrell, C., Yesuf, H. M., Popping, G., et al. 2024, Monthly Notices of the Royal Astronomical Society, 527, 6506

    2024

  14. [22]

    2024, arXiv preprint arXiv:2407.10900

    Boylan-Kolchin, M. 2024, arXiv preprint arXiv:2407.10900

    2024 arXiv

  15. [23]

    2025, Monthly Notices of the Royal Astronomical Society, staf471

    Boylan-Kolchin, M. 2025, Monthly Notices of the Royal Astronomical Society, staf471

    2025

  16. [24]

    D., et al

    Brinchmann, J., Charlot, S., White, S. D., et al. 2004, Monthly notices of the royal astronomical society, 351, 1151

    2004

  17. [25]

    R., Ellison, S

    Brown, W., Patton, D. R., Ellison, S. L., & Faria, L. 2023, Monthly Notices of the Royal Astronomical Society, 522, 5107

    2023

  18. [26]

    Bustamante, S., Sparre, M., Springel, V ., & Grand, R. J. 2018, Monthly Notices of the Royal Astronomical Society, 479, 3381

    2018

  19. [27]

    H., Ellison, S

    Byrne-Mamahit, S., Hani, M. H., Ellison, S. L., Quai, S., & Patton, D. R. 2023, Monthly Notices of the Royal Astronomical Society, 519, 4966 Article number, page 21 of 26 A&A proofs:manuscript no. aanda

    2023

  20. [28]

    G., Patton, D., et al

    Carlberg, R., Cohen, J. G., Patton, D., et al. 2000, The Astrophysical Journal, 532, L1

    2000

  21. [29]

    2003, Publications of the Astronomical Society of the Pacific, 115, 763

    Chabrier, G. 2003, Publications of the Astronomical Society of the Pacific, 115, 763

    2003

  22. [30]

    J., Chapman, S

    Conselice, C. J., Chapman, S. C., & Windhorst, R. A. 2003, The Astrophysical Journal, 596, L5

    2003

  23. [31]

    J., Yang, C., & Bluck, A

    Conselice, C. J., Yang, C., & Bluck, A. F. 2009, Monthly Notices of the Royal Astronomical Society, 394, 1956

    2009

  24. [32]

    2020, The Astrophysical Journal, 889, 156

    Contini, E., Gu, Q., Ge, X., et al. 2020, The Astrophysical Journal, 889, 156

    2020

  25. [33]

    2019, The Astrophysical Journal, 882, 167

    Contini, E., Gu, Q., Kang, X., Rhee, J., & Yi, S. 2019, The Astrophysical Journal, 882, 167

    2019

  26. [34]

    A., Hough, T., Vega-Martínez, C

    Cora, S. A., Hough, T., Vega-Martínez, C. A., & Orsi, Á. A. 2019, Monthly Notices of the Royal Astronomical Society, 483, 1686

    2019

  27. [35]

    2021, Publications of the Astronomical Society of Australia, 38, e035

    Cortese, L., Catinella, B., & Smith, R. 2021, Publications of the Astronomical Society of Australia, 38, e035

    2021

  28. [36]

    S., Primack, J

    Cox, T., Jonsson, P., Somerville, R. S., Primack, J. R., & Dekel, A. 2008, Monthly Notices of the Royal Astronomical Society, 384, 386

    2008

  29. [37]

    A., Schaye, J., Bower, R

    Crain, R. A., Schaye, J., Bower, R. G., et al. 2015, Monthly Notices of the Royal Astronomical Society, 450, 1937

    2015

  30. [38]

    P., Pimbblet, K

    Crossett, J. P., Pimbblet, K. A., Jones, D. H., Brown, M. J., & Stott, J. P. 2017, Monthly Notices of the Royal Astronomical Society, 464, 480

    2017

  31. [39]

    J., Springel, V ., White, S

    Croton, D. J., Springel, V ., White, S. D., et al. 2006, Monthly Notices of the Royal Astronomical Society, 365, 11

    2006

  32. [40]

    S., Fazio, G

    Cybulski, R., Yun, M. S., Fazio, G. G., & Gutermuth, R. A. 2014, Monthly No- tices of the Royal Astronomical Society, 439, 3564 Dalla Vecchia, C. & Schaye, J. 2008, Monthly Notices of the Royal Astronomical Society, 387, 1431

    2014

  33. [41]

    W., Kaviraj, S., Lintott, C

    Darg, D. W., Kaviraj, S., Lintott, C. J., et al. 2010, Monthly Notices of the Royal Astronomical Society, 401, 1043

    2010

  34. [42]

    2016, The Astrophysical Journal, 825, 113

    Darvish, B., Mobasher, B., Sobral, D., et al. 2016, The Astrophysical Journal, 825, 113

    2016

  35. [43]

    2021, arXiv preprint arXiv:2108.05874 Davé, R., Anglés-Alcázar, D., Narayanan, D., et al

    Das, A., Pandey, B., Sarkar, S., & Dutta, A. 2021, arXiv preprint arXiv:2108.05874 Davé, R., Anglés-Alcázar, D., Narayanan, D., et al. 2019, Monthly Notices of the Royal Astronomical Society, 486, 2827

    2021 arXiv

  36. [44]

    J., Robotham, A

    Davies, L. J., Robotham, A. S. G., Driver, S. P., et al. 2015, Monthly Notices of the Royal Astronomical Society, 452, 616

    2015

  37. [45]

    S., & White, S

    Davis, M., Efstathiou, G., Frenk, C. S., & White, S. D. 1985, Astrophysical Jour- nal, Part 1 (ISSN 0004-637X), vol. 292, May 15, 1985, p. 371-394. Research supported by the Science and Engineering Research Council of England and NASA., 292, 371

    1985

  38. [46]

    & Geller, M

    Davis, M. & Geller, M. J. 1976, Astrophysical Journal, V ol. 208, pp. 13-19 (1976)., 208, 13 De Lucia, G., Springel, V ., White, S. D., Croton, D., & Kauffmann, G. 2006, Monthly Notices of the Royal Astronomical Society, 366, 499 De Ravel, L., Le Fèvre, O., Tresse, L., et al. ...

    1976

  39. [47]

    2018, The Astrophysical Journal, 869, 6

    Deger, S., Rudnick, G., Kelkar, K., et al. 2018, The Astrophysical Journal, 869, 6

    2018

  40. [48]

    2017, The Astrophysical Journal, 843, 126

    Delahaye, A., Webb, T., Nantais, J., et al. 2017, The Astrophysical Journal, 843, 126

    2017

  41. [49]

    G., Rodríguez-Martín, J., Díaz-García, L., et al

    Delgado, R. G., Rodríguez-Martín, J., Díaz-García, L., et al. 2022, Astronomy & Astrophysics, 666, A84 Di Matteo, P., Combes, F., Melchior, A.-L., & Semelin, B. 2007, Astronomy & Astrophysics, 468, 61 Di Matteo, T., Springel, V ., & Hernquist, L. 2005, nature, 433, 604

    2022

  42. [50]

    L., Cao, C., Xu, C

    Domingue, D. L., Cao, C., Xu, C. K., et al. 2016, The Astrophysical Journal, 829, 78 Domínguez-Gómez, J., Pérez, I., Ruiz-Lara, T., et al. 2023, Nature, 619, 269

    2016

  43. [51]

    2019, Monthly Notices of the Royal Astronomical Society, 485, 4817

    Donnari, M., Pillepich, A., Nelson, D., et al. 2019, Monthly Notices of the Royal Astronomical Society, 485, 4817

    2019

  44. [52]

    1980, Astrophysical Journal, Part 1, vol

    Dressler, A. 1980, Astrophysical Journal, Part 1, vol. 236, Mar. 1, 1980, p. 351- 365., 236, 351

    1980

  45. [53]

    2023, Monthly Notices of the Royal Astronomical Society, 519, 2199

    Eisert, L., Pillepich, A., Nelson, D., et al. 2023, Monthly Notices of the Royal Astronomical Society, 519, 2199

    2023

  46. [54]

    L., Mendel, J

    Ellison, S. L., Mendel, J. T., Patton, D. R., & Scudder, J. M. 2013, Monthly Notices of the Royal Astronomical Society, 435, 3627

    2013

  47. [55]

    L., Patton, D

    Ellison, S. L., Patton, D. R., Simard, L., & McConnachie, A. W. 2008, The As- tronomical Journal, 135, 1877

    2008

  48. [56]

    L., Viswanathan, A., Patton, D

    Ellison, S. L., Viswanathan, A., Patton, D. R., et al. 2019, Monthly Notices of the Royal Astronomical Society, 487, 2491

    2019

  49. [57]

    L., Patton, D

    Ferreira, L., Ellison, S. L., Patton, D. R., et al. 2025, Monthly Notices of the Royal Astronomical Society: Letters, 538, L31

    2025

  50. [58]

    A., Kannappan, S

    Florez, J., Berlind, A. A., Kannappan, S. J., et al. 2021, The Astrophysical Jour- nal, 906, 97

    2021

  51. [59]

    2015, Monthly Notices of the Royal Astronomical Society, 450, 4486 Gallagher III, J

    Furlong, M., Bower, R., Theuns, T., et al. 2015, Monthly Notices of the Royal Astronomical Society, 450, 4486 Gallagher III, J. S. & Ostriker, J. P. 1972, Astronomical Journal, V ol. 77, p. 288 (1972), 77, 288

    1972

  52. [60]

    2014, Monthly Notices of the Royal Astronomical Society, 445, 175

    Genel, S., V ogelsberger, M., Springel, V ., et al. 2014, Monthly Notices of the Royal Astronomical Society, 445, 175

    2014

  53. [61]

    Ghafour, P., Tavasoli, S., & Shojaei, M. R. 2025, Journal of Cosmology and Astroparticle Physics, 2025, 001

    2025

  54. [62]

    Gunn, J. E. & Gott III, J. R. 1972, Astrophysical Journal, vol. 176, p. 1, 176, 1

    1972

  55. [63]

    H., Gosain, H., Ellison, S

    Hani, M. H., Gosain, H., Ellison, S. L., Patton, D. R., & Torrey, P. 2020, Monthly Notices of the Royal Astronomical Society, 493, 3716

    2020

  56. [64]

    F., Hernquist, L., Cox, T

    Hopkins, P. F., Hernquist, L., Cox, T. J., et al. 2006, The Astrophysical Journal Supplement Series, 163, 1

    2006

  57. [65]

    F., Hernquist, L., Cox, T

    Hopkins, P. F., Hernquist, L., Cox, T. J., & Kereš, D. 2008, The Astrophysical Journal Supplement Series, 175, 356

    2008

  58. [66]

    R., V ogeley, M

    Hoyle, F., Rojas, R. R., V ogeley, M. S., & Brinkmann, J. 2005, The Astrophysical Journal, 620, 618

    2005

  59. [67]

    2012, Monthly Notices of the Royal Astro- nomical Society, 426, 3041 Jaffé, Y

    Hoyle, F., V ogeley, M., & Pan, D. 2012, Monthly Notices of the Royal Astro- nomical Society, 426, 3041 Jaffé, Y . L., Verheijen, M. A., Haines, C. P., et al. 2016, Monthly Notices of the Royal Astronomical Society, 461, 1202

    2012

  60. [68]

    & Yan-chun, S

    Jia-jie, Q. & Yan-chun, S. 2021, Chinese Astronomy and Astrophysics, 45, 31

    2021

  61. [69]

    2022, The Astrophysical Journal, 926, 115

    Jian, H.-Y ., Lin, L., Hsieh, B.-C., et al. 2022, The Astrophysical Journal, 926, 115

    2022

  62. [70]

    2018, Publications of the Astronomical Society of Japan, 70, S23

    Jian, H.-Y ., Lin, L., Oguri, M., et al. 2018, Publications of the Astronomical Society of Japan, 70, S23

    2018

  63. [71]

    & Fairall, A

    Kauffmann, G. & Fairall, A. 1991, Monthly Notices of the Royal Astronomical Society, 248, 313

    1991

  64. [72]

    D., Heckman, T

    Kauffmann, G., White, S. D., Heckman, T. M., et al. 2004, Monthly Notices of the Royal Astronomical Society, 353, 713

    2004

  65. [73]

    E., Aragón-Salamanca, A., et al

    Kelkar, K., Gray, M. E., Aragón-Salamanca, A., et al. 2019, Monthly Notices of the Royal Astronomical Society, 486, 868 Kennicutt Jr, R. C. 1989, Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 344, Sept. 15, 1989, p. 685-703., 344, 685

    2019

  66. [74]

    P., Oemler Jr, A., Schechter, P

    Kirshner, R. P., Oemler Jr, A., Schechter, P. L., & Shectman, S. A. 1981, As- trophysical Journal, Part 2-Letters to the Editor, vol. 248, Sept. 1, 1981, p. L57-L60., 248, L57

    1981

  67. [75]

    H., Cisternas, M., & Querejeta, M

    Knapen, J. H., Cisternas, M., & Querejeta, M. 2015, Monthly Notices of the Royal Astronomical Society, 454, 1742

    2015

  68. [76]

    H., Beygu, B., et al

    Kreckel, K., van Gorkom, J. H., Beygu, B., et al. 2014, Proceedings of the Inter- national Astronomical Union, 11, 591 Laganá, T. F. & Ulmer, M. 2018, Monthly Notices of the Royal Astronomical Society, 475, 523

    2014

  69. [77]

    G., Tissera, P

    Lambas, D. G., Tissera, P. B., Alonso, M. S., & Coldwell, G. 2003, Monthly Notices of the Royal Astronomical Society, 346, 1189

    2003

  70. [78]

    B., Tinsley, B

    Larson, R. B., Tinsley, B. M., & Caldwell, C. N. 1980, Astrophysical Journal, Part 1, vol. 237, May 1, 1980, p. 692-707. Research supported by the Alfred P. Sloan Foundation, 237, 692

    1980

  71. [79]

    & Wandelt, B

    Lavaux, G. & Wandelt, B. D. 2010, Monthly Notices of the Royal Astronomical Society, 403, 1392

    2010

  72. [80]

    2020, The Astrophysical Journal, 902, 75

    Li, P., Wang, H., Mo, H., Wang, E., & Hong, H. 2020, The Astrophysical Journal, 902, 75

    2020

  73. [81]

    2007, Astronomy & Astrophysics, 461, 881

    Limousin, M., Kneib, J., Bardeau, S., et al. 2007, Astronomy & Astrophysics, 461, 881

    2007

  74. [82]

    C., Jian, H.-Y ., et al

    Lin, L., Cooper, M. C., Jian, H.-Y ., et al. 2010, The Astrophysical Journal, 718, 1158

    2010

  75. [83]

    C., Weiner, B

    Lin, L., Koo, D. C., Weiner, B. J., et al. 2007, The Astrophysical Journal, 660, L51

    2007

  76. [84]

    C., Willmer, C

    Lin, L., Koo, D. C., Willmer, C. N., et al. 2004, The Astrophysical Journal, 617, L9

    2004

  77. [85]

    R., Koo, D

    Lin, L., Patton, D. R., Koo, D. C., et al. 2008, The Astrophysical Journal, 681, 232

    2008

  78. [86]

    C., Li, C., Wang, L., & Wang, E

    Lin, Y ., Sodi, B. C., Li, C., Wang, L., & Wang, E. 2014, The Astrophysical Journal, 796, 98

    2014

  79. [87]

    M., Davis, M., Faber, S., et al

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

    2008

  80. [88]

    & Belli, S

    Man, A. & Belli, S. 2018, Nature Astronomy, 2, 695

    2018

  81. [89]

    2018, Monthly Notices of the Royal Astronomical Society, 480, 5113

    Marinacci, F., V ogelsberger, M., Pakmor, R., et al. 2018, Monthly Notices of the Royal Astronomical Society, 480, 5113

    2018

  82. [90]

    L., Balogh, M

    McGee, S. L., Balogh, M. L., Wilman, D. J., et al. 2011, Monthly Notices of the Royal Astronomical Society, 413, 996

    2011

  83. [91]

    M., Cortese, L., Croom, S

    Medling, A. M., Cortese, L., Croom, S. M., et al. 2018, Monthly Notices of the Royal Astronomical Society, 475, 5194

    2018

  84. [92]

    1984, Astrophysical Journal, Part 1 (ISSN 0004-637X), vol

    Merritt, D. 1984, Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 276, Jan. 1, 1984, p. 26-37., 276, 26

    1984

  85. [93]

    & Hernquist, L

    Mihos, C. & Hernquist, L. 1995, arXiv preprint astro-ph/9512099

    1995 arXiv

  86. [94]

    Mihos, J. C. 2004, Clusters of Galaxies: Probes of Cosmological Structure and Galaxy Evolution, 277

    2004

  87. [95]

    M., Moreno, J., White, A., et al

    Moorman, C. M., Moreno, J., White, A., et al. 2016, The Astrophysical Journal, 831, 118

    2016

  88. [96]

    L., et al

    Moreno, J., Torrey, P., Ellison, S. L., et al. 2015, Monthly Notices of the Royal Astronomical Society, 448, 1107 Article number, page 22 of 26 Mohammad Reza Shojaei1 et al.: From V oids to Clusters

    2015

  89. [97]

    L., et al

    Moreno, J., Torrey, P., Ellison, S. L., et al. 2021, Monthly Notices of the Royal Astronomical Society, 503, 3113

    2021

  90. [98]

    L., et al

    Moreno, J., Torrey, P., Ellison, S. L., et al. 2019, Monthly Notices of the Royal Astronomical Society, 485, 1320

    2019

  91. [99]

    P., Naab, T., & White, S

    Moster, B. P., Naab, T., & White, S. D. 2013, Monthly Notices of the Royal Astronomical Society, 428, 3121

    2013

  92. [100]

    2006, The Astrophysical Journal, 636, L81

    Naab, T., Khochfar, S., & Burkert, A. 2006, The Astrophysical Journal, 636, L81

    2006

  93. [101]

    P., Pillepich, A., Springel, V ., et al

    Naiman, J. P., Pillepich, A., Springel, V ., et al. 2018, Monthly Notices of the Royal Astronomical Society, 477, 1206

    2018

  94. [102]

    2015, Astronomy and Computing, 13, 12

    Nelson, D., Pillepich, A., Genel, S., et al. 2015, Astronomy and Computing, 13, 12

    2015

  95. [103]

    2018, Monthly Notices of the Royal Astronomical Society, 475, 624

    Nelson, D., Pillepich, A., Springel, V ., et al. 2018, Monthly Notices of the Royal Astronomical Society, 475, 624

    2018

  96. [104]

    2019, Computational Astrophysics and Cosmology, 6, 1

    Nelson, D., Springel, V ., Pillepich, A., et al. 2019, Computational Astrophysics and Cosmology, 6, 1

    2019

  97. [105]

    Neyrinck, M. C. 2008, Monthly notices of the royal astronomical society, 386, 2101

    2008

  98. [106]

    2004, Monthly Notices of the Royal Astronomical Society, 355, 874 Oemler Jr, A

    Nikolic, B., Cullen, H., & Alexander, P. 2004, Monthly Notices of the Royal Astronomical Society, 355, 874 Oemler Jr, A. 1974, PhD thesis, California Institute of Technology

    2004

  99. [107]

    H., et al

    Oh, S., Kim, K., Lee, J. H., et al. 2018, The Astrophysical Journal Supplement Series, 237, 14

    2018

  100. [108]

    P., Naab, T., Johansson, P

    Oser, L., Ostriker, J. P., Naab, T., Johansson, P. H., & Burkert, A. 2010, The Astrophysical Journal, 725, 2312

    2010

  101. [109]

    1980, Comments on Astrophysics, V ol

    Ostriker, J. 1980, Comments on Astrophysics, V ol. 8, P. 177, 1980, 8, 177

    1980

  102. [110]

    D., Ceccarelli, L., & Lambas, D

    Padilla, N. D., Ceccarelli, L., & Lambas, D. 2005, Monthly Notices of the Royal Astronomical Society, 363, 977

    2005

  103. [111]

    2018, The Astrophysical Journal, 868, 132

    Pan, H.-A., Lin, L., Hsieh, B.-C., et al. 2018, The Astrophysical Journal, 868, 132

    2018

  104. [112]

    G., van Dokkum, P

    Patel, S. G., van Dokkum, P. G., Franx, M., et al. 2013, The Astrophysical Jour- nal, 766, 15

    2013

  105. [113]

    2002, The Astrophysical Journal, 565, 208

    Patton, D., Pritchet, C., Carlberg, R., et al. 2002, The Astrophysical Journal, 565, 208

    2002

  106. [114]

    R., Wilson, K

    Patton, D. R., Wilson, K. D., Metrow, C. J., et al. 2020, Monthly Notices of the Royal Astronomical Society, 494, 4969

    2020

  107. [115]

    J., Kovaˇc, K., et al

    Peng, Y .-j., Lilly, S. J., Kovaˇc, K., et al. 2010, The Astrophysical Journal, 721, 193

    2010

  108. [116]

    J., Renzini, A., & Carollo, M

    Peng, Y .-j., Lilly, S. J., Renzini, A., & Carollo, M. 2012, The Astrophysical Jour- nal, 757, 4

    2012

  109. [117]

    Perez, J., Michel-Dansac, L., & Tissera, P. B. 2011, Monthly Notices of the Royal Astronomical Society, 417, 580

    2011

  110. [118]

    2014, Astronomy & Astrophysics, 562, A1

    Perret, V ., Renaud, F., Epinat, B., et al. 2014, Astronomy & Astrophysics, 562, A1

    2014

  111. [119]

    Platen, E., Van De Weygaert, R., & Jones, B. J. 2007, Monthly notices of the royal astronomical society, 380, 551

    2007

  112. [120]

    & Geller, M

    Postman, M. & Geller, M. 1984, Astrophysical Journal, Part 1 (ISSN 0004- 637X), vol. 281, June 1, 1984, p. 95-99., 281, 95

    1984

  113. [121]

    F., Williams, R

    Quadri, R. F., Williams, R. J., Franx, M., & Hildebrandt, H. 2011, The Astro- physical Journal, 744, 88

    2011

  114. [122]

    W., Markevitch, M., Clowe, D., Gonzalez, A

    Randall, S. W., Markevitch, M., Clowe, D., Gonzalez, A. H., & Bradaˇc, M. 2008, The Astrophysical Journal, 679, 1173

    2008

  115. [123]

    P., Davies, L

    Robotham, A., Driver, S. P., Davies, L. J., et al. 2014, Monthly Notices of the Royal Astronomical Society, 444, 3986

    2014

  116. [124]

    P., et al

    Robotham, A., Liske, J., Driver, S. P., et al. 2013, Monthly Notices of the Royal Astronomical Society, 431, 167

    2013

  117. [125]

    2015, Monthly Notices of the Royal Astronomical Society, 449, 49

    Rodriguez-Gomez, V ., Genel, S., V ogelsberger, M., et al. 2015, Monthly Notices of the Royal Astronomical Society, 449, 49

    2015

  118. [126]

    V ., Genel, S., et al

    Rodriguez-Gomez, V ., Sales, L. V ., Genel, S., et al. 2017, Monthly Notices of the Royal Astronomical Society, 467, 3083 Rodríguez Medrano, A. M., Paz, D. J., Stasyszyn, F. A., & Ruiz, A. N. 2022, Monthly Notices of the Royal Astronomical Society, 511, 2688 Rodríguez-Medrano,...

    2017

  119. [127]

    R., V ogeley, M

    Rojas, R. R., V ogeley, M. S., Hoyle, F., & Brinkmann, J. 2004, The Astrophysical Journal, 617, 50

    2004

  120. [128]

    Rosas-Guevara, Y ., Tissera, P., Lagos, C. d. P., Paillas, E., & Padilla, N. 2022, Monthly Notices of the Royal Astronomical Society, 517, 712

    2022

  121. [129]

    S., Kewley, L

    Rupke, D. S., Kewley, L. J., & Barnes, J. E. 2010, The Astrophysical Journal Letters, 710, L156

    2010

  122. [130]

    Sahni, V ., Sathyaprakash, B., & Shandarin, S. F. 1994, arXiv preprint astro- ph/9403044

    1994

  123. [131]

    J., Fabello, S., et al

    Saintonge, A., Tacconi, L. J., Fabello, S., et al. 2012, The Astrophysical Journal, 758, 73

    2012

  124. [132]

    & Mirabel, I

    Sanders, D. & Mirabel, I. 1996, Annual Review of Astronomy and Astrophysics, 34, 749

    1996

  125. [133]

    A., Bower, R

    Schaye, J., Crain, R. A., Bower, R. G., et al. 2015, Monthly Notices of the Royal Astronomical Society, 446, 521

    2015

  126. [134]

    2015, Astronomy & Astrophysics, 575, A74

    Schreiber, C., Pannella, M., Elbaz, D., et al. 2015, Astronomy & Astrophysics, 575, A74

    2015

  127. [135]

    M., Ellison, S

    Scudder, J. M., Ellison, S. L., Torrey, P., Patton, D. R., & Mendel, J. T. 2012, Monthly Notices of the Royal Astronomical Society, 426, 549

    2012

  128. [136]

    2015, Monthly Notices of the Royal Astronomical Society, 452, 575

    Sijacki, D., V ogelsberger, M., Genel, S., et al. 2015, Monthly Notices of the Royal Astronomical Society, 452, 575

    2015

  129. [137]

    D., et al

    Silva, A., Marchesini, D., Silverman, J. D., et al. 2018, The Astrophysical Jour- nal, 868, 46

    2018

  130. [138]

    & Holley-Bockelmann, K

    Sinha, M. & Holley-Bockelmann, K. 2009, Monthly Notices of the Royal Astro- nomical Society, 397, 190 Sol Alonso, M., Lambas, D. G., Tissera, P., & Coldwell, G. 2006, Monthly No- tices of the Royal Astronomical Society, 367, 1029

    2009

  131. [139]

    S., Hopkins, P

    Somerville, R. S., Hopkins, P. F., Cox, T. J., Robertson, B. E., & Hernquist, L. 2008, Monthly Notices of the Royal Astronomical Society, 391, 481

    2008

  132. [140]

    C., Feldmann, R., et al

    Sparre, M., Hayward, C. C., Feldmann, R., et al. 2017, Monthly Notices of the Royal Astronomical Society, 466, 88

    2017

  133. [141]

    2022, Monthly Notices of the Royal Astronomical Society, 509, 2720

    Sparre, M., Whittingham, J., Damle, M., et al. 2022, Monthly Notices of the Royal Astronomical Society, 509, 2720

    2022

  134. [142]

    2010, Proceedings of the International Astronomical Union, 6, 203

    Springel, V . 2010, Proceedings of the International Astronomical Union, 6, 203

    2010

  135. [143]

    2005, Monthly Notices of the Royal Astronomical Society, 361, 776

    Springel, V ., Di Matteo, T., & Hernquist, L. 2005, Monthly Notices of the Royal Astronomical Society, 361, 776

    2005

  136. [144]

    & Hernquist, L

    Springel, V . & Hernquist, L. 2003, Monthly Notices of the Royal Astronomical Society, 339, 289

    2003

  137. [145]

    2018, Monthly Notices of the Royal Astronomical Society, 475, 676

    Springel, V ., Pakmor, R., Pillepich, A., et al. 2018, Monthly Notices of the Royal Astronomical Society, 475, 676

    2018

  138. [146]

    D., Tormen, G., & Kauffmann, G

    Springel, V ., White, S. D., Tormen, G., & Kauffmann, G. 2001, Monthly Notices of the Royal Astronomical Society, 328, 726

    2001

  139. [147]

    2016, Astronomy & Astrophysics, 591, A51

    Steinhauser, D., Schindler, S., & Springel, V . 2016, Astronomy & Astrophysics, 591, A51

    2016

  140. [148]

    R., Bullock, J

    Stewart, K. R., Bullock, J. S., Wechsler, R. H., & Maller, A. H. 2009, The Astro- physical Journal, 702, 307

    2009

  141. [149]

    M., Lavaux, G., Hamaus, N., et al

    Sutter, P. M., Lavaux, G., Hamaus, N., et al. 2015, Astronomy and Computing, 9, 1

    2015

  142. [150]

    J., Genzel, R., & Sternberg, A

    Tacconi, L. J., Genzel, R., & Sternberg, A. 2020, Annual Review of Astronomy and Astrophysics, 58, 157

    2020

  143. [151]

    G., Vasei, K., & Lehnert, M

    Tavasoli, S., Rahmani, H., Khosroshahi, H. G., Vasei, K., & Lehnert, M. D. 2015, The Astrophysical Journal Letters, 803, L13

    2015

  144. [152]

    2013, Astronomy & Astrophysics, 553, A15

    Tavasoli, S., Vasei, K., & Mohayaee, R. 2013, Astronomy & Astrophysics, 553, A15

    2013

  145. [153]

    & Cen, R

    Tonnesen, S. & Cen, R. 2012, Monthly Notices of the Royal Astronomical Soci- ety, 425, 2313

    2012

  146. [154]

    J., Kewley, L., & Hernquist, L

    Torrey, P., Cox, T. J., Kewley, L., & Hernquist, L. 2012, The Astrophysical Jour- nal, 746, 108

    2012

  147. [155]

    F., V ogelsberger, M., et al

    Torrey, P., Snyder, G. F., V ogelsberger, M., et al. 2015, Monthly Notices of the Royal Astronomical Society, 447, 2753 Van de Weygaert, R. & Platen, E. 2011, in International Journal of Modern Physics: Conference Series, V ol. 1, World Scientific, 41–66 V ogelsberger, M., Gen...

    2015

  148. [156]

    A., Van Dokkum, P

    Wake, D. A., Van Dokkum, P. G., & Franx, M. 2012, The Astrophysical Journal Letters, 751, L44

    2012

  149. [157]

    Wechsler, R. H. & Tinker, J. L. 2018, ARA&A, 56, 435

    2018

  150. [158]

    K., Schawinski, K., Treister, E., Trakhtenbrot, B., & Sanders, D

    Weigel, A. K., Schawinski, K., Treister, E., Trakhtenbrot, B., & Sanders, D. B. 2018, Monthly Notices of the Royal Astronomical Society, 476, 2308

    2018

  151. [159]

    2018, Monthly Notices of the Royal Astronomical Society, 479, 4056

    Weinberger, R., Springel, V ., Pakmor, R., et al. 2018, Monthly Notices of the Royal Astronomical Society, 479, 4056

    2018

  152. [160]

    R., Tinker, J

    Wetzel, A. R., Tinker, J. L., Conroy, C., & Van Den Bosch, F. C. 2013, Monthly Notices of the Royal Astronomical Society, 432, 336

    2013

  153. [161]

    E., Labbé, I., van Dokkum, P

    Whitaker, K. E., Labbé, I., van Dokkum, P. G., et al. 2011, The Astrophysical Journal, 735, 86

    2011

  154. [162]

    E., Van Dokkum, P

    Whitaker, K. E., Van Dokkum, P. G., Brammer, G., et al. 2010, The Astrophysical Journal, 719, 1715

    2010

  155. [163]

    J., Quadri, R

    Williams, R. J., Quadri, R. F., Franx, M., Van Dokkum, P., & Labbé, I. 2009, The Astrophysical Journal, 691, 1879

    2009

  156. [164]

    J., Quadri, R

    Williams, R. J., Quadri, R. F., Franx, M., et al. 2010, The Astrophysical Journal, 713, 738

    2010

  157. [165]

    Woods, D. F. & Geller, M. J. 2007, The Astronomical Journal, 134, 527

    2007

  158. [166]

    Wuyts, S., Schreiber, N. M. F., Lutz, D., et al. 2011, The Astrophysical Journal, 738, 106

    2011

  159. [167]

    1994, arXiv preprint astro-ph/9409021 Article number, page 23 of 26 A&A proofs:manuscript no

    Xu, G. 1994, arXiv preprint astro-ph/9409021 Article number, page 23 of 26 A&A proofs:manuscript no. aanda Appendix A: Additional Merger Statistics Figure A.1 summarizes the merger histories of star-forming and quenched galaxies in voids and clusters. At early times (>10.5 Gyr...

    1994 arXiv

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.