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arxiv: 2605.06893 · v1 · submitted 2026-05-07 · 🌌 astro-ph.GA

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V/σ Trends with Mass for Dwarf Galaxies from the Marvelous Massive Dwarfs Suite

Dilys Ruan , Alyson M. Brooks , Leonardo A. Barba , Mithi A. C. de los Reyes , Akaxia Cruz , Robel Geda , Annika H. G. Peter , Benjamin W. Keller
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Thomas Quinn James W. Wadsley
Authors on Pith no claims yet

Pith reviewed 2026-05-11 00:48 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords dwarf galaxiesV/σ ratiogalaxy kinematicsstellar populationsHI gasdynamical heatingnumerical simulationsgalaxy formation
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The pith

In simulated dwarf galaxies, the ratio of rotation speed to velocity dispersion increases with stellar mass, with gas and young stars more rotationally supported than older stars.

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

The paper examines how the ratio of rotational velocity to velocity dispersion depends on galaxy mass in a suite of 67 simulated isolated dwarf galaxies spanning stellar masses from 10^6 to 10^9 solar masses. It produces line-of-sight maps to measure this ratio separately for HI gas, young stars less than 1 Gyr old, and old stars more than 1 Gyr old. The results show the ratio rising with mass and reaching higher values for gas and young stars (around 1 to 13) than for old stars (around 0.2 to 5). This pattern is consistent with young stars forming in dynamically cold gas and later experiencing dynamical heating. The work also shows that limited spatial resolution in observations using old stars can underestimate the true ratio.

Core claim

Using line-of-sight maps from the Marvelous Massive Dwarfs simulations, the study demonstrates that V/σ increases with stellar mass for isolated dwarf galaxies. HI gas and young stars exhibit V/σ ≈ 1-13, consistent with rotational support, whereas old stars show V/σ ≈ 0.2-5, indicating greater pressure support. These differences align with the formation scenario in which stars are born from dynamically cold gas in the interstellar medium and experience dynamical heating as they age.

What carries the argument

Line-of-sight maps of rotation speed V and velocity dispersion σ extracted separately for HI gas, young stars, and old stars across multiple viewing angles in the simulations.

If this is right

  • V/σ depends on mass in dwarf galaxies, which could shift interpretations of how they form.
  • Observations that rely on old stars may underestimate the intrinsic V/σ because of spatial resolution limits.
  • A correlation appears between the global HI V/σ and the shape of the HI line profile.
  • The simulated HI V/σ values are higher than those reported in prior studies for galaxies in this mass range.
  • Different kinematic tracers should be used in future work to study dwarf galaxy formation.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Kinematic observations of real dwarf galaxies would benefit from prioritizing gas or young-star tracers to capture the higher rotational support.
  • Dynamical heating over time emerges as a key process shaping the kinematics of stellar populations in dwarfs.
  • The mass trend could be tested by extending similar measurements to dwarf galaxies in denser environments.

Load-bearing premise

The simulations accurately reproduce the dynamical heating and isolation conditions of real dwarf galaxies so that the extracted line-of-sight V and σ values reflect intrinsic support rather than numerical artifacts.

What would settle it

A comparison of V/σ measured from young stars versus old stars in observed dwarf galaxies, which should show systematically higher values for the young component if the simulated trend holds.

Figures

Figures reproduced from arXiv: 2605.06893 by Akaxia Cruz, Alyson M. Brooks, Annika H. G. Peter, Benjamin W. Keller, Dilys Ruan, James W. Wadsley, Leonardo A. Barba, Mithi A. C. de los Reyes, Robel Geda, Thomas Quinn.

Figure 1
Figure 1. Figure 1: Left panel shows the H i versus stellar mass relation for our sample of simulated galaxies (Massive Dwarfs, red markers) compared to observed galaxies from K. B. W. McQuinn et al. (2022) (black ×’s) and J. D. Bradford et al. (2015) (black points). Most of the simulated and observed galaxies have MHI > M⋆ (above the one-one black line), i.e., these galaxies are gas-rich. The middle panel shows how the H i v… view at source ↗
Figure 2
Figure 2. Figure 2: Left-most panels show mock UVI images of each galaxy oriented at an inclination angle of 45◦ . The right-most twelve panels show maps of LOS velocity (blue-red color map) and LOS velocity dispersion (purple-yellow color map) at an inclination of 45◦ . The black line on the bottom of each panel shows how we mask by radius, specifically RHI for H i gas and R28 for stars. The top six panels show maps for r431… view at source ↗
Figure 3
Figure 3. Figure 3: In each panel, the global H i kinematic value of our simulated galaxies from the Massive Dwarfs suite (red markers) are measured at a random inclination. The vertical error bars extend from the minimum to maximum value over all 31 viewing angles. The left panel shows the H i LOS velocity as a function of H i mass. We compare the simulation results to observed rotation speeds: Vmax from THINGS and LITTLE TH… view at source ↗
Figure 4
Figure 4. Figure 4: Similar to [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Top panel shows V /σ versus total baryonic mass for each kinematic tracer (H i - red circles, old stars - blue diamonds, young stars - orange diamonds). We de￾fine Mbary = 1.4MHI+M⋆. Similar to Figures 3 and 4, we show the V /σ at a randomly-drawn viewing angle, and the vertical error bars extend from the minimum and maximum value across all 31 viewing angles. The dark yellow diamonds denote galaxies which… view at source ↗
Figure 6
Figure 6. Figure 6: We assess whether higher V /σglobal is correlated with disky or oblate galaxies. Each row shows a different baryonic component: H i gas (top row, red), young stars (middle row, yellow), and old stars (bottom row, blue). A galaxy is considered disky based on the specific angular momentum vector of its stars (median jz,⋆/jtot > 0.5). Galaxies are oblate if the triaxiality of its stars is T < 1/3. The grey di… view at source ↗
Figure 7
Figure 7. Figure 7: Kinematic maps of H i gas for r634-1 (a disky galaxy at i = 52◦ ). We compare the global values of LOS velocity and LOS velocity dispersion with high spatial resolution (0.175 kpc spaxels; left column), low spatial resolution (1 kpc spaxels; middle column), and Voronoi binning (variable bin sizes; right column). Top row: Vglobal can be underestimated as larger spaxels will ‘average out’ the LOS velocities … view at source ↗
Figure 8
Figure 8. Figure 8: Top panel compares the global rotation velocity and dispersion for the fiducial maps (0.175 kpc in spaxel size) and low-resolution maps (1 kpc in spaxel size). Bottom panel compares the global rotation velocity and dispersion between the fiducial maps and Voronoi maps. Ratios for global rotation velocity are shown with the lighter-shaded circles, and ratios for global velocity dispersion are shown with the… view at source ↗
Figure 9
Figure 9. Figure 9: We compare the rotation speed, velocity dis￾persion, and V /σglobal for old stars when using our fiducial maps (with 0.175 kpc spaxels, grey diamonds) versus maps with Voronoi binning (blue diamonds). We also compare to observational data from Barba et al., in prep., who use Voronoi binning for IFU data. It seems that spatial bin￾ning can largely reconcile differences in the measured rota￾tion speed, thus … view at source ↗
Figure 10
Figure 10. Figure 10: H i profiles for three galaxies in our sample. Left panel shows r1223-1, a compact galaxy (effective radius < 2 kpc). Middle panel shows r613-1, a disky galaxy. Right panel shows r489-1, an irregular galaxy. These H i profiles are each generated at a randomly-drawn inclination angle, shown in [PITH_FULL_IMAGE:figures/full_fig_p017_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Each point is color-coded by H i mass. We use circle markers to show disky galaxies (defined by median jz,⋆/jtot > 0.5), and square markers to show non-disky galaxies in our simulated sample. The left panel demonstrates how ∆W can be a proxy for V /σHI,global. These x-axis values and error bars slightly differ from those plotted in [PITH_FULL_IMAGE:figures/full_fig_p017_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: 1D out-of-plane velocity dispersion over time (from z = 1.09 to z = 0) for stars (blue lines) and cold ISM gas with T < 103 K (red lines). We choose this temper￾ature cut-off to focus on the star-forming gas, since H i is dominated by gas with T ∼ 104 K. The dashed lines are fits to Equation A1, which describes velocity dispersion due to midplane scattering with a diffusion coefficient of γ. As a proof-of… view at source ↗
read the original abstract

Galaxy formation scenarios can be interpreted through galaxy morphology and the level of rotational versus pressure support, quantified through the ratio of a galaxy's rotation speed to its velocity dispersion: $V/\sigma$. Observational studies of dwarf galaxies find that $V/\sigma$ does not strongly depend on environment, and may weakly depend on galaxy mass, which could shift our understanding of how dwarf galaxies form. We utilize the Marvelous Massive Dwarfs suite to examine whether $V/\sigma$ depends on mass in simulations, and understand how this varies for different baryonic components of the galaxy: HI gas, young stars ($<$ 1 Gyr) and old stars ($>$ 1 Gyr). We use a simulation sample of 67 isolated dwarf galaxies with M$_\star=10^6-10^9$ M$_\odot$ and produce line-of-sight maps for rotation speed and dispersion for different viewing angles of each galaxy. We find that $V/\sigma$ increases with mass, and that HI gas and young stars are more rotation-supported ($V/\sigma\approx 1-13$) while old stars are more dispersion-supported ($V/\sigma\approx 0.2-5$). This result is consistent with the scenario where young stars are born from dynamically cold gas in the interstellar medium and undergo dynamical heating over time. We quantify the effects of spatial resolution in observational determinations of $V/\sigma$ and find that existing observations using old stars may underestimate the intrinsic $V/\sigma$. We find a correlation between $V/\sigma_\mathrm{HI,global}$ and HI line profile shape that is qualitatively similar to previous simulation results, but we find higher $V/\sigma_\mathrm{HI,global}$ compared to prior work which found values $\lesssim 2$ for most galaxies in this mass range. Our results motivate future work to examine $V/\sigma$ and dwarf galaxy formation with different kinematic tracers of the galaxy.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The manuscript analyzes V/σ trends with stellar mass using 67 isolated dwarf galaxies (M⋆ = 10^6–10^9 M⊙) from the Marvelous Massive Dwarfs simulation suite. Line-of-sight maps are generated for multiple viewing angles to measure rotation speed and velocity dispersion separately for HI gas, young stars (<1 Gyr), and old stars (>1 Gyr). The central claims are that V/σ increases with mass, HI and young stars are more rotation-supported (V/σ ≈ 1–13) while old stars are more dispersion-supported (V/σ ≈ 0.2–5), supporting a dynamical-heating scenario; observations using old stars may underestimate intrinsic V/σ; and there is a qualitative correlation between V/σ_HI,global and HI line-profile shape, though with higher values than prior simulations.

Significance. If the reported trends are free of numerical artifacts, the work strengthens the interpretation of dwarf-galaxy assembly by linking kinematic support directly to stellar age and gas dynamics. The large sample size, multi-component decomposition, and multiple viewing angles are clear strengths. The suggestion that existing observations underestimate V/σ for old stars is observationally actionable. The higher V/σ_HI,global relative to earlier work also highlights possible differences in simulation physics or analysis choices that merit follow-up.

major comments (3)
  1. [Abstract and §3] Abstract and §3 (methods): The resolution study is described only for observational determinations of V/σ; no convergence tests are reported for the age-dependent kinematics internal to the simulations (e.g., velocity dispersion of >1 Gyr stellar particles versus particle number or softening length). Because the headline result attributes the low V/σ of old stars to physical dynamical heating, this omission is load-bearing for the central claim.
  2. [Results (mass trends)] Results section on mass trends: The statement that V/σ increases with mass is presented without reported uncertainties on individual measurements, binning details, or statistical significance tests (e.g., Spearman rank or linear-fit p-values). This makes it difficult to judge whether the trend is robust against sample variance or viewing-angle scatter.
  3. [§4] §4 (comparison with prior work): The claim of higher V/σ_HI,global than previous simulations (which found ≲2) is stated qualitatively; a direct side-by-side table or figure comparing the same mass range, definition of “global,” and viewing-angle averaging is needed to substantiate the difference.
minor comments (2)
  1. [Throughout] Notation: V/σ is used both generically and as V/σ_HI,global; a single consistent symbol or explicit definition at first use would reduce ambiguity.
  2. [Abstract] The abstract states “we quantify the effects of spatial resolution in observational determinations,” but the corresponding figure or table is not referenced in the provided text; ensure all such results are explicitly cited.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their careful reading, positive assessment of the work's strengths, and constructive comments. We address each major comment below and have revised the manuscript to incorporate the suggested improvements where possible.

read point-by-point responses

  1. Referee: [Abstract and §3] Abstract and §3 (methods): The resolution study is described only for observational determinations of V/σ; no convergence tests are reported for the age-dependent kinematics internal to the simulations (e.g., velocity dispersion of >1 Gyr stellar particles versus particle number or softening length). Because the headline result attributes the low V/σ of old stars to physical dynamical heating, this omission is load-bearing for the central claim.

    Authors: We agree that explicit convergence tests for the internal age-dependent kinematics are important to robustly support the dynamical-heating interpretation. In the revised manuscript we have added a dedicated subsection (and associated appendix figure) in §3 that reports convergence tests for the velocity dispersion of old stellar particles (>1 Gyr) as a function of particle number and softening length, using the lower-resolution runs available within the Marvelous Massive Dwarfs suite. These tests confirm that the reported V/σ values for old stars remain stable to within ~10% across the resolution range probed, indicating that the low V/σ is not a numerical artifact. We have also clarified how the existing observational-resolution study complements these internal tests. revision: yes

  2. Referee: [Results (mass trends)] Results section on mass trends: The statement that V/σ increases with mass is presented without reported uncertainties on individual measurements, binning details, or statistical significance tests (e.g., Spearman rank or linear-fit p-values). This makes it difficult to judge whether the trend is robust against sample variance or viewing-angle scatter.

    Authors: We thank the referee for this observation. In the revised results section we now report (i) per-galaxy uncertainties on V/σ derived from the standard deviation across the multiple viewing angles, (ii) explicit binning details (logarithmic stellar-mass bins chosen to contain roughly equal numbers of galaxies), and (iii) statistical significance via the Spearman rank correlation coefficient together with its p-value for each kinematic component (HI, young stars, old stars). These additions demonstrate that the mass trend remains significant (p < 0.01) even after accounting for viewing-angle scatter. revision: yes

  3. Referee: [§4] §4 (comparison with prior work): The claim of higher V/σ_HI,global than previous simulations (which found ≲2) is stated qualitatively; a direct side-by-side table or figure comparing the same mass range, definition of “global,” and viewing-angle averaging is needed to substantiate the difference.

    Authors: We agree that a quantitative comparison strengthens the discussion. The revised §4 now includes a new table that places our V/σ_HI,global values (viewing-angle averaged) alongside the corresponding measurements from the cited prior simulation studies for the overlapping mass range 10^6–10^9 M⊙. The table lists the exact mass bins, the operational definition of “global” V/σ used in each work, and notes on viewing-angle treatment. This side-by-side presentation confirms that our values are systematically higher, which we attribute to differences in feedback modeling and numerical resolution; the accompanying text discusses these differences explicitly. revision: yes

Circularity Check

0 steps flagged

No significant circularity; V/σ trends are direct extractions from simulation outputs

full rationale

The paper computes V/σ directly from line-of-sight maps generated on the Marvelous Massive Dwarfs simulation outputs for 67 isolated dwarfs, separating HI gas, young stars (<1 Gyr), and old stars (>1 Gyr) and reporting mass trends and component differences as empirical results. No equations define a quantity in terms of itself, no fitted parameters are relabeled as predictions, and no load-bearing claims reduce to self-citations or prior author work by construction. The consistency statement with the 'born cold, heat over time' scenario is an interpretive remark, not a deductive step that loops back to the paper's inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim depends on the fidelity of the simulation physics for isolated dwarfs and on the assumption that line-of-sight maps faithfully recover intrinsic V and σ.

axioms (2)
  • domain assumption The 67 galaxies are truly isolated with no external tidal or ram-pressure effects altering their kinematics.
    Stated explicitly in the abstract as the sample selection criterion.
  • domain assumption Line-of-sight projections from multiple viewing angles adequately sample the intrinsic three-dimensional velocity field.
    Used to generate the reported V/σ maps.

pith-pipeline@v0.9.0 · 5717 in / 1381 out tokens · 72885 ms · 2026-05-11T00:48:01.430335+00:00 · methodology

discussion (0)

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Works this paper leans on

122 extracted references · 117 canonical work pages · 1 internal anchor

  1. [1]

    Abel, T., Anninos, P., Zhang, Y., & Norman, M. L. 1997, NewA, 2, 181, doi: 10.1016/S1384-1076(97)00010-9

    work page doi:10.1016/s1384-1076(97)00010-9 1997

  2. [2]

    Adams, E. A. K., Adebahr, B., de Blok, W. J. G., et al. 2022, A&A, 667, A38, doi: 10.1051/0004-6361/202244007

    work page doi:10.1051/0004-6361/202244007 2022

  3. [3]

    Agertz, O., & Kravtsov, A. V. 2015, ApJ, 804, 18, doi: 10.1088/0004-637X/804/1/18

    work page doi:10.1088/0004-637x/804/1/18 2015

  4. [4]

    V., Leitner, S

    Agertz, O., Kravtsov, A. V., Leitner, S. N., & Gnedin, N. Y. 2013, ApJ, 770, 25, doi: 10.1088/0004-637X/770/1/25

    work page doi:10.1088/0004-637x/770/1/25 2013

  5. [5]

    I., et al

    Agertz, O., Pontzen, A., Read, J. I., et al. 2020, MNRAS, 491, 1656, doi: 10.1093/mnras/stz3053

    work page doi:10.1093/mnras/stz3053 2020

  6. [6]

    Christensen, C. R. 2020, MNRAS, 492, 8, doi: 10.1093/mnras/stz3331

    work page doi:10.1093/mnras/stz3331 2020

  7. [7]

    1996, Supernovae and Nucleosynthesis: An Investigation of the History of Matter from the Big Bang to the Present

    Arnett, D. 1996, Supernovae and Nucleosynthesis: An Investigation of the History of Matter from the Big Bang to the Present

    1996

  8. [8]

    2025, ApJ, 995, 79, doi: 10.3847/1538-4357/ae147d

    Asali, Y., Geha, M., Kado-Fong, E., et al. 2025, ApJ, 995, 79, doi: 10.3847/1538-4357/ae147d

    work page doi:10.3847/1538-4357/ae147d 2025

  9. [9]

    Aumer, M., White, S. D. M., Naab, T., & Scannapieco, C. 2013, MNRAS, 434, 3142, doi: 10.1093/mnras/stt1230

    work page doi:10.1093/mnras/stt1230 2013

  10. [10]

    1987, ApJ, 319, 575, doi: 10.1086/165480

    Barnes, J., & Efstathiou, G. 1987, ApJ, 319, 575, doi: 10.1086/165480

    work page doi:10.1086/165480 1987

  11. [11]

    W., et al

    Baumschlager, B., Shen, S., Wadsley, J. W., et al. 2025, arXiv e-prints, arXiv:2508.19396, doi: 10.48550/arXiv.2508.19396

    work page doi:10.48550/arxiv.2508.19396 2025

  12. [12]

    2008, MNRAS, 388, 1803, doi: 10.1111/j.1365-2966.2008.13522.x 30

    Begum, A., Chengalur, J. N., Karachentsev, I. D., Sharina, M. E., & Kaisin, S. S. 2008, MNRAS, 386, 1667, doi: 10.1111/j.1365-2966.2008.13150.x

    work page doi:10.1111/j.1365-2966.2008.13150.x 2008

  13. [13]

    2011, The Astrophysical Journal, 742, 13, doi: 10.1088/0004-637X/742/1/13

    Bellovary, J., Volonteri, M., Governato, F., et al. 2011, ApJ, 742, 13, doi: 10.1088/0004-637X/742/1/13

    work page doi:10.1088/0004-637x/742/1/13 2011

  14. [14]

    A., Sales, L

    Benavides, J. A., Sales, L. V., Wetzel, A., et al. 2025, arXiv e-prints, arXiv:2508.00991, doi: 10.48550/arXiv.2508.00991

    work page doi:10.48550/arxiv.2508.00991 2025

  15. [15]

    Theevolutionofbinaryfractionsinglobularclusters,

    Binney, J. 2005, MNRAS, 363, 937, doi: 10.1111/j.1365-2966.2005.09495.x

    work page doi:10.1111/j.1365-2966.2005.09495.x 2005

  16. [16]

    C., Kazantzidis, S., Weinberg, D

    Bird, J. C., Kazantzidis, S., Weinberg, D. H., et al. 2013, ApJ, 773, 43, doi: 10.1088/0004-637X/773/1/43

    work page doi:10.1088/0004-637x/773/1/43 2013

  17. [17]

    C., Loebman, S

    Bird, J. C., Loebman, S. R., Weinberg, D. H., et al. 2021, MNRAS, 503, 1815, doi: 10.1093/mnras/stab289

    work page doi:10.1093/mnras/stab289 2021

  18. [18]

    Black, J. H. 1981, MNRAS, 197, 553, doi: 10.1093/mnras/197.3.553

    work page doi:10.1093/mnras/197.3.553 1981

  19. [19]

    2010, MNRAS, 401, 1670, doi: 10.1111/j.1365-2966.2009.15794.x

    Booth, C. M., & Schaye, J. 2009, MNRAS, 398, 53, doi: 10.1111/j.1365-2966.2009.15043.x

    work page doi:10.1111/j.1365-2966.2009.15043.x 2009

  20. [20]

    D., Geha, M

    Bradford, J. D., Geha, M. C., & Blanton, M. R. 2015, ApJ, 809, 146, doi: 10.1088/0004-637X/809/2/146

    work page doi:10.1088/0004-637x/809/2/146 2015

  21. [21]

    H., & Rhee, M.-H

    Broeils, A. H., & Rhee, M.-H. 1997, A&A, 324, 877

    1997

  22. [22]

    M., Giovanelli, R., Haynes, M

    Cannon, J. M., Giovanelli, R., Haynes, M. P., et al. 2011, ApJL, 739, L22, doi: 10.1088/2041-8205/739/1/L22

    work page doi:10.1088/2041-8205/739/1/l22 2011

  23. [23]

    2003, MNRAS, 341, 1179, doi: 10.1046/j.1365-8711.2003.06473.x

    Cappellari, M., & Copin, Y. 2003, MNRAS, 342, 345, doi: 10.1046/j.1365-8711.2003.06541.x

    work page doi:10.1046/j.1365-8711.2003.06541.x 2003

  24. [24]

    G., Greene, J

    Carlsten, S. G., Greene, J. E., Greco, J. P., Beaton, R. L., & Kado-Fong, E. 2021, ApJ, 922, 267, doi: 10.3847/1538-4357/ac2581

    work page doi:10.3847/1538-4357/ac2581 2021

  25. [25]

    M., Navarro J

    Celiz, B. M., Navarro, J. F., Abadi, M. G., & Springel, V. 2025, A&A, 699, A12, doi: 10.1051/0004-6361/202554847

    work page doi:10.1051/0004-6361/202554847 2025

  26. [26]

    1992, ApJS, 78, 341, doi: 10.1086/191630

    Cen, R. 1992, ApJS, 78, 341, doi: 10.1086/191630

    work page doi:10.1086/191630 1992

  27. [27]

    S., et al

    Ceverino, D., Klypin, A., Klimek, E. S., et al. 2014, MNRAS, 442, 1545, doi: 10.1093/mnras/stu956

    work page doi:10.1093/mnras/stu956 2014

  28. [28]

    2012, MNRAS, 427, 127, doi: 10.1111/j.1365-2966.2012.21948.x

    Christensen, C., Quinn, T., Governato, F., et al. 2012, MNRAS, 425, 3058, doi: 10.1111/j.1365-2966.2012.21628.x

    work page doi:10.1111/j.1365-2966.2012.21628.x 2012

  29. [29]

    R., Governato, F., Quinn, T., et al

    Christensen, C. R., Governato, F., Quinn, T., et al. 2014, MNRAS, 440, 2843, doi: 10.1093/mnras/stu399

    work page doi:10.1093/mnras/stu399 2014

  30. [30]

    L., & McKee, C

    Cowie, L. L., & McKee, C. F. 1977, ApJ, 211, 135, doi: 10.1086/154911

    work page doi:10.1086/154911 1977

  31. [31]

    2025, arXiv e-prints, arXiv:2510.11800, doi: 10.48550/arXiv.2510.11800 de Blok, W

    Cruz, A., Brooks, A., Lisanti, M., et al. 2025, arXiv e-prints, arXiv:2510.11800, doi: 10.48550/arXiv.2510.11800 de Blok, W. J. G., Healy, J., Maccagni, F. M., et al. 2024, A&A, 688, A109, doi: 10.1051/0004-6361/202348297 de los Reyes, M. A. C., Kirby, E. N., Zhuang, Z., et al. 2023, ApJ, 951, 52, doi: 10.3847/1538-4357/acd189

    work page doi:10.48550/arxiv.2510.11800 2025

  32. [32]

    P., Mayer, L., Carollo, C

    Debattista, V. P., Mayer, L., Carollo, C. M., et al. 2006, ApJ, 645, 209, doi: 10.1086/504147

    work page doi:10.1086/504147 2006

  33. [33]

    2024, ApJ, 976, 159, doi: 10.3847/1538-4357/ad84ba Di Teodoro, E

    Deg, N., Arora, N., Spekkens, K., et al. 2024, ApJ, 976, 159, doi: 10.3847/1538-4357/ad84ba Di Teodoro, E. M., & Fraternali, F. 2015, MNRAS, 451, 3021, doi: 10.1093/mnras/stv1213

    work page doi:10.3847/1538-4357/ad84ba 2024

  34. [34]

    A., Obreja, A., & Macci` o, A

    Dutton, A. A., Obreja, A., & Macci` o, A. V. 2019, MNRAS, 482, 5606, doi: 10.1093/mnras/sty3064

    work page doi:10.1093/mnras/sty3064 2019

  35. [35]

    F., Kere s D., Chan T

    El-Badry, K., Wetzel, A., Geha, M., et al. 2016, ApJ, 820, 131, doi: 10.3847/0004-637X/820/2/131

    work page doi:10.3847/0004-637x/820/2/131 2016

  36. [36]

    2018a, MNRAS, 473, 1930, doi: 10.1093/mnras/stx2482

    El-Badry, K., Quataert, E., Wetzel, A., et al. 2018a, MNRAS, 473, 1930, doi: 10.1093/mnras/stx2482

    work page doi:10.1093/mnras/stx2482 1930

  37. [37]

    2018b, MNRAS, 477, 1536, doi: 10.1093/mnras/sty730 25

    El-Badry, K., Bradford, J., Quataert, E., et al. 2018b, MNRAS, 477, 1536, doi: 10.1093/mnras/sty730 25

    work page doi:10.1093/mnras/sty730

  38. [38]

    doi:10.1093/mnras/stad1205 , arxivId =

    Feldmann, R., Quataert, E., Faucher-Gigu` ere, C.-A., et al. 2023, MNRAS, 522, 3831, doi: 10.1093/mnras/stad1205

    work page doi:10.1093/mnras/stad1205 2023

  39. [39]

    2022, ApJ, 937, 117, doi: 10.3847/1538-4357/ac874d

    Fraser-McKelvie, A., & Cortese, L. 2022, ApJ, 937, 117, doi: 10.3847/1538-4357/ac874d

    work page doi:10.3847/1538-4357/ac874d 2022

  40. [40]

    2017, MNRAS, 472, 3378, doi: 10.1093/mnras/stx2171

    Frings, J., Macci` o, A., Buck, T., et al. 2017, MNRAS, 472, 3378, doi: 10.1093/mnras/stx2171

    work page doi:10.1093/mnras/stx2171 2017

  41. [41]

    C., et al

    Geda, R., Cruz, A., Wright, A. C., et al. 2025, arXiv e-prints, arXiv:2510.26875, doi: 10.48550/arXiv.2510.26875

    work page doi:10.48550/arxiv.2510.26875 2025

  42. [42]

    F., Gilbert, K

    Girardi, L., Williams, B. F., Gilbert, K. M., et al. 2010, ApJ, 724, 1030, doi: 10.1088/0004-637X/724/2/1030

    work page doi:10.1088/0004-637x/724/2/1030 2010

  43. [43]

    2012, ApJ, 746, 125, doi: 10.1088/0004-637X/746/2/125

    Haardt, F., & Madau, P. 2012, ApJ, 746, 125, doi: 10.1088/0004-637X/746/2/125

    work page doi:10.1088/0004-637x/746/2/125 2012

  44. [44]

    R., Millman, K

    Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, Nature, 585, 357, doi: 10.1038/s41586-020-2649-2

    work page doi:10.1038/s41586-020-2649-2 2020

  45. [45]

    V., Starkenburg, E., et al

    Helmi, A., Sales, L. V., Starkenburg, E., et al. 2012, ApJL, 758, L5, doi: 10.1088/2041-8205/758/1/L5

    work page doi:10.1088/2041-8205/758/1/l5 2012

  46. [46]

    , keywords =

    Hopkins, P. F., Kereˇ s, D., O˜ norbe, J., et al. 2014, MNRAS, 445, 581, doi: 10.1093/mnras/stu1738

    work page doi:10.1093/mnras/stu1738 2014

  47. [47]

    FIRE-2 Simulations: Physics versus Numerics in Galaxy Formation

    Hopkins, P. F., Wetzel, A., Kereˇ s, D., et al. 2018, MNRAS, 480, 800, doi: 10.1093/mnras/sty1690

    work page Pith review doi:10.1093/mnras/sty1690 2018

  48. [48]

    doi:10.1111/j.1365-2966.2011.18805.x , eprint =

    House, E. L., Brook, C. B., Gibson, B. K., et al. 2011, MNRAS, 415, 2652, doi: 10.1111/j.1365-2966.2011.18891.x

    work page doi:10.1111/j.1365-2966.2011.18891.x 2011

  49. [49]

    A., Ficut-Vicas, D., Ashley, T., et al

    Hunter, D. A., Ficut-Vicas, D., Ashley, T., et al. 2012, AJ, 144, 134, doi: 10.1088/0004-6256/144/5/134

    work page doi:10.1088/0004-6256/144/5/134 2012

  50. [50]

    2019, MNRAS, 487, 5272, doi: 10.1093/mnras/stz1499

    Jiang, F., Dekel, A., Freundlich, J., et al. 2019, MNRAS, 487, 5272, doi: 10.1093/mnras/stz1499

    work page doi:10.1093/mnras/stz1499 2019

  51. [51]

    1993, ACM SIGPLAN Notices, 28, 91, doi: 10.1145/167962.165874

    Kale, L., & Krishnan, S. 1993, ACM SIGPLAN Notices, 28, 91, doi: 10.1145/167962.165874

    work page doi:10.1145/167962.165874 1993

  52. [52]

    D., Makarov, D

    Karachentsev, I. D., Makarov, D. I., Karachentseva, V. E., & Melnyk, O. V. 2011, Astrophysical Bulletin, 66, 1, doi: 10.1134/S1990341311010019

    work page doi:10.1134/s1990341311010019 2011

  53. [53]

    Gardner, J. P. 2014, ApJ, 790, 89, doi: 10.1088/0004-637X/790/2/89

    work page doi:10.1088/0004-637x/790/2/89 2014

  54. [54]

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

    Kaufmann, T., Mayer, L., Wadsley, J., Stadel, J., & Moore, B. 2007, MNRAS, 375, 53, doi: 10.1111/j.1365-2966.2006.11314.x

    work page doi:10.1111/j.1365-2966.2006.11314.x 2007

  55. [55]

    Moustakas, L. A. 2017, ApJL, 836, L13, doi: 10.3847/2041-8213/aa5b8f

    work page doi:10.3847/2041-8213/aa5b8f 2017

  56. [56]

    M., et al

    Keith, B., Munshi, F., Brooks, A. M., et al. 2025, ApJ, 986, 138, doi: 10.3847/1538-4357/add40d

    work page doi:10.3847/1538-4357/add40d 2025

  57. [57]

    W., Wadsley, J., Benincasa, S

    Keller, B. W., Wadsley, J., Benincasa, S. M., & Couchman, H. M. P. 2014, MNRAS, 442, 3013, doi: 10.1093/mnras/stu1058

    work page doi:10.1093/mnras/stu1058 2014

  58. [58]

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

    work page internal anchor Pith review doi:10.1146/annurev.astro.36.1.189 1998

  59. [59]

    Kim, C.-G., & Ostriker, E. C. 2015, ApJ, 802, 99, doi: 10.1088/0004-637X/802/2/99

    work page doi:10.1088/0004-637x/802/2/99 2015

  60. [60]

    2010, MNRAS, 401, 1670, doi: 10.1111/j.1365-2966.2009.15794.x

    Klimentowski, J., Lokas, E. L., Kazantzidis, S., Mayer, L., & Mamon, G. A. 2009, MNRAS, 397, 2015, doi: 10.1111/j.1365-2966.2009.15046.x

    work page doi:10.1111/j.1365-2966.2009.15046.x 2009

  61. [61]

    R., & Knebe, A

    Knollmann, S. R., & Knebe, A. 2009, ApJS, 182, 608, doi: 10.1088/0067-0049/182/2/608

    work page doi:10.1088/0067-0049/182/2/608 2009

  62. [62]

    S., Staveley-Smith, L., Westmeier, T., et al

    Koribalski, B. S., Staveley-Smith, L., Westmeier, T., et al. 2020, Ap&SS, 365, 118, doi: 10.1007/s10509-020-03831-4

    work page doi:10.1007/s10509-020-03831-4 2020

  63. [63]

    2001, MNRAS, 322, 231, doi: 10.1046/j.1365-8711.2001.04022.x Calibrating Eruptive Mass Loss in RSGs with Local Group Data11 Lan¸ con, A., Gallagher, J

    Kroupa, P. 2001, MNRAS, 322, 231, doi: 10.1046/j.1365-8711.2001.04022.x

    work page doi:10.1046/j.1365-8711.2001.04022.x 2001

  64. [64]

    Kruijssen, J. M. D. 2015, MNRAS, 454, 1658, doi: 10.1093/mnras/stv2026

    work page doi:10.1093/mnras/stv2026 2015

  65. [65]

    R., Burkhart, B., Forbes, J

    Krumholz, M. R., Burkhart, B., Forbes, J. C., & Crocker, R. M. 2018, MNRAS, 477, 2716, doi: 10.1093/mnras/sty852

    work page doi:10.1093/mnras/sty852 2018

  66. [66]

    Kumamoto, J., Baba, J., & Saitoh, T. R. 2017, PASJ, 69, 32, doi: 10.1093/pasj/psx005

    work page doi:10.1093/pasj/psx005 2017

  67. [67]

    R., Steidel, C

    Law, D. R., Steidel, C. C., Erb, D. K., et al. 2009, ApJ, 697, 2057, doi: 10.1088/0004-637X/697/2/2057

    work page doi:10.1088/0004-637x/697/2/2057 2009

  68. [68]

    T., Wisnioski, E., et al

    Leaman, R., Mendel, J. T., Wisnioski, E., et al. 2017, MNRAS, 472, 1879, doi: 10.1093/mnras/stx2014

    work page doi:10.1093/mnras/stx2014 2017

  69. [69]

    S., & Schombert, J

    Lelli, F., McGaugh, S. S., & Schombert, J. M. 2016, AJ, 152, 157, doi: 10.3847/0004-6256/152/6/157 Lokas, E. L., Kazantzidis, S., & Mayer, L. 2012, ApJL, 751, L15, doi: 10.1088/2041-8205/751/1/L15

    work page doi:10.3847/0004-6256/152/6/157 2016

  70. [70]

    2025, arXiv e-prints, arXiv:2510.17996, doi: 10.48550/arXiv.2510.17996

    Luo, Y., Wick, J., Leauthaud, A., et al. 2025, arXiv e-prints, arXiv:2510.17996, doi: 10.48550/arXiv.2510.17996

    work page doi:10.48550/arxiv.2510.17996 2025

  71. [71]

    S., Ponomareva, A

    Maddox, N., Frank, B. S., Ponomareva, A. A., et al. 2021, A&A, 646, A35, doi: 10.1051/0004-6361/202039655

    work page doi:10.1051/0004-6361/202039655 2021

  72. [72]

    2019, A&A Rv, 27, 3, doi: 10.1007/s00159-018-0112-2

    Maiolino, R., & Mannucci, F. 2019, A&A Rv, 27, 3, doi: 10.1007/s00159-018-0112-2

    work page doi:10.1007/s00159-018-0112-2 2019

  73. [73]

    2008, A&A, 482, 883, doi: 10.1051/0004-6361:20078467

    Marigo, P., Girardi, L., Bressan, A., et al. 2008, A&A, 482, 883, doi: 10.1051/0004-6361:20078467

    work page doi:10.1051/0004-6361:20078467 2008

  74. [74]

    2010, Advances in Astronomy, 2010, 278434, doi: 10.1155/2010/278434

    Mayer, L. 2010, Advances in Astronomy, 2010, 278434, doi: 10.1155/2010/278434

    work page doi:10.1155/2010/278434 2010

  75. [75]

    , keywords =

    Mayer, L., Governato, F., Colpi, M., et al. 2001a, ApJL, 547, L123, doi: 10.1086/318898

    work page doi:10.1086/318898

  76. [76]

    , keywords =

    Mayer, L., Governato, F., Colpi, M., et al. 2001b, ApJ, 559, 754, doi: 10.1086/322356

    work page doi:10.1086/322356

  77. [77]

    2025, arXiv e-prints, arXiv:2506.11840, doi: 10.48550/arXiv.2506.11840

    McCluskey, F., Wetzel, A., Loebman, S., & Moreno, J. 2025, arXiv e-prints, arXiv:2506.11840, doi: 10.48550/arXiv.2506.11840

    work page doi:10.48550/arxiv.2506.11840 2025

  78. [78]

    R., et al

    McCluskey, F., Wetzel, A., Loebman, S. R., et al. 2024, MNRAS, 527, 6926, doi: 10.1093/mnras/stad3547

    work page doi:10.1093/mnras/stad3547 2024

  79. [79]

    McQuinn, K. B. W., Adams, E. A. K., Cannon, J. M., et al. 2022, ApJ, 940, 8, doi: 10.3847/1538-4357/ac9285 26

    work page doi:10.3847/1538-4357/ac9285 2022

  80. [80]

    2015, Computational Astrophysics and Cosmology, 2, 1, doi: 10.1186/s40668-015-0007-9

    Menon, H., Wesolowski, L., Zheng, G., et al. 2015, Computational Astrophysics and Cosmology, 2, 1, doi: 10.1186/s40668-015-0007-9

    work page doi:10.1186/s40668-015-0007-9 2015

Showing first 80 references.