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arxiv: 2606.26445 · v1 · pith:OZWBHBBKnew · submitted 2026-06-24 · 🌌 astro-ph.GA

Columba: isolated dwarf galaxy populations in diverse cosmological environments simulated with a cold interstellar medium

Jemima M. Briggs , Azadeh Fattahi , Robert A. Crain , Yannick M. Bahe , Sylvia Ploeckinger , Matthieu Schaller , Alejandro Ben\'itez-Llambay , Evgenii Chaikin
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Alexander J. Richings Joop Schaye
This is my paper

Pith reviewed 2026-06-26 01:10 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords dwarf galaxiescosmological hydrodynamical simulationsstellar mass-halo mass relationhalo concentrationgalaxy formationlarge-scale environmenthalo assembly bias
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The pith

Large-scale environment sets dwarf galaxy numbers but halo concentration controls their stellar masses and ages.

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

The paper runs zoom-in hydrodynamical simulations of 25 under-dense 5 cMpc regions spanning voids to filaments, resolving galaxies down to 10^6 solar masses with a model that includes cold gas and tuned stellar feedback. It shows that the surrounding 5 cMpc density changes the overall count of haloes and galaxies but leaves the stellar mass to halo mass relation and the fraction of haloes that host galaxies largely unchanged for the 10^6-10^9 solar mass range. Host halo concentration, measured in matched dark-matter-only runs, instead correlates with whether a halo hosts a galaxy, the scatter around the mean relation, and the time of galaxy assembly, so that more concentrated haloes form older and more massive galaxies at fixed halo mass. The offset from the mean relation also tracks the time when 90 percent of the stellar mass has formed.

Core claim

The 5 cMpc environment influences the normalisation of the halo and galaxy mass functions, but does not significantly affect the stellar mass-halo mass relation and halo occupation fraction for galaxies with M⋆=10^6-10^9 solar masses. Host halo concentration, estimated from DM-only counterparts, is more important: both the fraction of haloes hosting a resolved galaxy and the scatter about the SMHM relation correlate positively with concentration. Owing to halo assembly bias, concentration also influences galaxy formation times, such that at fixed halo mass more concentrated haloes host galaxies that are both older and more massive. The offset from the mean SMHM relation also anti-correlates

What carries the argument

Host halo concentration measured from matched dark-matter-only simulations, which drives occupation fraction, SMHM scatter, and formation timing via assembly bias.

If this is right

  • The total number of dwarf galaxies varies with large-scale density on 5 cMpc scales.
  • At fixed halo mass, more concentrated haloes contain galaxies with higher stellar mass and earlier formation times.
  • Scatter around the mean stellar mass-halo mass relation increases with halo concentration.
  • The time when 90 percent of stellar mass assembles anti-correlates with the offset from the mean relation.
  • Halo occupation fraction rises with concentration for these low-mass systems.

Where Pith is reading between the lines

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

  • Surveys that measure both local density and halo concentration proxies could separate the two effects on dwarf galaxy properties.
  • The same concentration-driven trends might appear in the ages and metallicities of observed dwarf satellites.
  • Extending the same simulations to higher halo masses would test whether concentration remains dominant outside the dwarf regime.

Load-bearing premise

The subgrid stellar feedback, calibrated only to match the z=0 galaxy stellar mass function, correctly represents the relevant baryonic processes in these dwarf galaxies across all tested environments.

What would settle it

Observational samples of dwarf galaxies in the 10^6-10^9 solar mass range that show no correlation between host halo concentration proxies and either stellar mass at fixed halo mass or stellar population age.

Figures

Figures reproduced from arXiv: 2606.26445 by Alejandro Ben\'itez-Llambay, Alexander J. Richings, Azadeh Fattahi, Evgenii Chaikin, Jemima M. Briggs, Joop Schaye, Matthieu Schaller, Robert A. Crain, Sylvia Ploeckinger, Yannick M. Bahe.

Figure 1
Figure 1. Figure 1: The distribution of mean enclosed density, relative to the cosmic mean density, of 𝑟 = 5 cMpc spheres, 𝛿5 ≡ 𝜌5/𝜌¯, selected from a parent cubic volume of side length 𝐿 = 400 cMpc, at 𝑧 = 0. The background distribution in a lighter shade corresponds to 2 × 105 randomly-centred spheres, the fore￾ground distribution denotes the subset with no haloes of 𝑀200 > 5×1011 M⊙ within 𝑟 = 5 cMpc of the region centre, … view at source ↗
Figure 3
Figure 3. Figure 3: Projections of the total surface mass density in the dark matter only simulations for the 25 selected spherical regions of 𝑟 = 5 cMpc at 𝑧 = 0. From top to bottom each row corresponds to the (−2, −1, 0, +1, +2) 𝜎 density band, respectively. From left to right, each column corresponds to the (−2, −1, 0, +1, +2) 𝜎 value of 𝑁LMC. For example the bottom row shows the highest density regions that we simulate (t… view at source ↗
Figure 4
Figure 4. Figure 4: The present-day GSMF of the composite galaxy population from all 25 regions, at m5 (maroon curve) and m6 (orange curve) resolutions, rep￾resenting a ‘strong convergence’ test. The grey hatched region indicates the stellar mass regime corresponding to 10 or fewer stellar particles (assuming their initial mass) at m5 resolution, the grey arrow extends to the correspond￾ing scale at m6 resolution. The curves … view at source ↗
Figure 6
Figure 6. Figure 6: The present-day galaxy size (3D half-mass radii) - stellar mass scaling relation of the composite galaxy population from all 25 regions, at m5 (maroon curve) and m6 (orange curve) resolutions, providing a ‘strong scaling’ test. Shaded regions denote the 10th − 90th percentile scatter in 𝑅★ at fixed 𝑀★. Line styles and hatching follow the conventions introduced in [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Upper panel: The aggregated present-day halo mass functions of the five regions comprising each of the five density bands (−2𝜎, ..., +2𝜎) at m5 resolution, with each band denoted by a coloured curve. Only field (cen￾tral) objects are considered. Grey hatching indicates the halo mass regime corresponding to fewer than 100 DM particles at m5 resolution. Curves are drawn with a reduced opacity for bins sample… view at source ↗
Figure 9
Figure 9. Figure 9: The present-day central stellar mass - halo mass scaling relation, at m5 resolution, of the aggregated central galaxy populations of the five regions comprising each of the five density bands. Coloured curves denote, for each density band, the median stellar mass at fixed halo mass, and include the contribution of haloes without a resolved galaxy. The SMHM relations of the semi-empirical models of Behroozi… view at source ↗
Figure 8
Figure 8. Figure 8: Upper panel: The aggregated present-day central galaxy stellar mass functions of the five regions comprising each of the five density bands, with each band denoted by a coloured curve. Grey hatching indicates the stellar mass regime corresponding to fewer than 10 stellar particles at m5 resolution. Curves are drawn with a reduced opacity for bins sampled by fewer than 10 galaxies. Grey symbols show the GSM… view at source ↗
Figure 10
Figure 10. Figure 10: shows the present-day median halo concentration at fixed halo mass obtained from the m5 simulations. The relation is shown for the population of field haloes identified in the hydrodynamical [PITH_FULL_IMAGE:figures/full_fig_p015_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Upper panel: The present-day luminous fraction as a function of mass, at m5 resolution, of the aggregated halo population of the five regions comprising the five density bands (coloured curves denote each density band). We deem haloes to be luminous if they host a galaxy with stellar mass 𝑀★ > 106 M⊙. The luminous fraction is only weakly sensitive to large￾scale environment. The grey dashed curve shows th… view at source ↗
Figure 12
Figure 12. Figure 12: shows the SMHM relation of the composite galaxy population drawn from all 25 regions at m5 resolution. Symbol colour denotes the intrinsic concentration of the halo, 𝑐NFW, and the solid grey curve shows the running median of 𝑀★ as a function of 𝑀200, computed using the locally-weighted scatter plot smoothing method (LOWESS, Cleveland 1979).We use this method rather than a binned median as it enables the c… view at source ↗
Figure 13
Figure 13. Figure 13: The same as [PITH_FULL_IMAGE:figures/full_fig_p018_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: The cumulative star formation histories (SFH) of central galaxies in the simulation suite, divided by their stellar mass at 𝑧 = 0 and their dark matter halo concentration. The left panel corresponds to a present-day stellar mass bin ranging between 107 < 𝑀★/M⊙ < 108 and the right panel corresponds to a present-day halo mass bin of 1010 < 𝑀200/M⊙ < 2 × 1010. In both panels, the sample is split into three b… view at source ↗
Figure 15
Figure 15. Figure 15: Similar to [PITH_FULL_IMAGE:figures/full_fig_p019_15.png] view at source ↗
read the original abstract

We introduce a suite of LambdaCDM cosmological, hydrodynamical simulations that track the evolution of a large population of dwarf galaxies. The suite comprises zoom-in simulations of 25 spherical, under-dense regions of r=5cMpc, selected to span $\approx1.5$ dex in mean enclosed density, covering voids to filamentary structures, whilst excluding haloes of Milky Way-mass or larger. The simulations achieve a mass resolution of $\sim 10^5$ solar masses with a galaxy formation model including cold, dense interstellar gas and whose subgrid stellar feedback efficiency reproduces the z=0 galaxy stellar mass function. We investigate the impact of the cosmic environment on dwarf galaxy formation and evolution. We find that the 5 cMpc environment influences the normalisation of the halo and galaxy mass functions, but does not significantly affect the stellar mass - halo mass (SMHM) relation and halo occupation fraction for galaxies with $M_{\star}=10^6-10^9$ solar masses. Instead, host halo concentration, estimated from DM-only counterparts, is more important: both the fraction of haloes hosting a resolved galaxy and the scatter about the SMHM relation correlate positively with concentration. Owing to halo assembly bias, concentration also influences galaxy formation times, such that at fixed halo mass more concentrated haloes host galaxies that are both older and more massive. The offset from the mean SMHM relation also anti-correlates with $t_{90}$, the time at which 90 percent of a galaxy's stellar mass has assembled. These correlations between halo properties and galaxy star formation histories present testable predictions for forthcoming observational surveys.

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

1 major / 0 minor

Summary. The paper presents a suite of zoom-in hydrodynamical ΣCDM simulations of 25 spherical 5 cMpc regions spanning ~1.5 dex in mean density (voids to filaments), excluding MW-mass halos. With ~10^5 M⊙ mass resolution and a galaxy formation model that includes cold dense ISM and tunes subgrid stellar feedback efficiency to reproduce the z=0 galaxy stellar mass function, the authors report that 5 cMpc-scale environment affects the normalization of halo and galaxy mass functions but does not significantly alter the stellar mass-halo mass (SMHM) relation or halo occupation fraction for M★ = 10^6–10^9 M⊙ galaxies. Host halo concentration (measured in DM-only counterparts) instead correlates positively with occupation fraction and SMHM scatter; due to assembly bias, more concentrated halos at fixed mass host older, more massive galaxies, and the SMHM offset anti-correlates with t90 (time of 90% stellar mass assembly). These yield testable predictions for surveys.

Significance. If robust, the results isolate halo concentration and assembly bias as the dominant drivers of dwarf galaxy properties over large-scale environment in this mass range, while the high-resolution treatment of cold ISM provides concrete, observationally testable correlations between halo properties and star-formation histories. The fixed-parameter approach and direct simulation outputs are strengths for reproducibility within the model.

major comments (1)
  1. [Abstract and galaxy formation model] Abstract and galaxy formation model description: the subgrid stellar feedback efficiency is tuned once to the global z=0 GSMF and held fixed across all 25 regions. No variation of this parameter or environment-specific recalibration is reported, so the claimed absence of environmental influence on the SMHM relation and occupation fraction for M★=10^6–10^9 M⊙ could be partly by construction; any environment-dependent effective feedback (via differing densities or accretion) would be suppressed. A robustness test varying the efficiency or comparing to alternative feedback implementations is needed to establish that the null environmental result is physical rather than model-dependent.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive comments and positive assessment of our work. We address the major comment below.

read point-by-point responses

  1. Referee: [Abstract and galaxy formation model] Abstract and galaxy formation model description: the subgrid stellar feedback efficiency is tuned once to the global z=0 GSMF and held fixed across all 25 regions. No variation of this parameter or environment-specific recalibration is reported, so the claimed absence of environmental influence on the SMHM relation and occupation fraction for M★=10^6–10^9 M⊙ could be partly by construction; any environment-dependent effective feedback (via differing densities or accretion) would be suppressed. A robustness test varying the efficiency or comparing to alternative feedback implementations is needed to establish that the null environmental result is physical rather than model-dependent.

    Authors: We thank the referee for highlighting this point. The subgrid stellar feedback efficiency is tuned once to the global z=0 GSMF and held fixed, as stated in the manuscript. This choice implements a single, universal model across all regions without any environment-specific recalibration. Consequently, the simulations test whether this fixed prescription produces environment-independent SMHM relations and occupation fractions when the resolved physics respond to the varying densities and accretion histories present in voids versus filaments. The null result on large-scale environment is therefore a prediction of the model rather than an imposed outcome. As the referee notes in their summary, the fixed-parameter approach is a strength for reproducibility within the model. We agree that varying the efficiency or testing alternative feedback schemes would further assess model dependence, but such tests require new simulation suites and lie beyond the current scope. We will add a short discussion of this limitation to the revised manuscript. revision: partial

Circularity Check

0 steps flagged

No significant circularity; results emerge from simulation outputs

full rationale

The paper runs a suite of hydrodynamical zoom-in simulations with a fixed subgrid stellar feedback efficiency calibrated once to reproduce the global z=0 galaxy stellar mass function. It then reports that the 5 cMpc environment affects mass function normalizations but not the SMHM relation or occupation fraction for M⋆=10^6–10^9 M⊙, while concentration (from DM-only counterparts) correlates with occupation fraction, scatter, and formation times. These outcomes are measured directly from the simulation data across different initial density regions; no equations, definitions, or claims reduce the reported correlations or environmental independence to the feedback tuning parameter by construction. No self-citations, ansatzes, or renamings are invoked as load-bearing steps. The derivation chain is self-contained.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The work rests on the standard LambdaCDM framework and a single tuned subgrid parameter; no new particles or forces are postulated.

free parameters (1)
  • subgrid stellar feedback efficiency
    Tuned to reproduce the z=0 galaxy stellar mass function
axioms (2)
  • standard math LambdaCDM cosmology
    Framework assumed for all cosmological initial conditions and evolution
  • domain assumption Cold dense interstellar gas component in the galaxy formation model
    Explicitly included as part of the hydrodynamical treatment

pith-pipeline@v0.9.1-grok · 5883 in / 1463 out tokens · 53646 ms · 2026-06-26T01:10:02.540917+00:00 · methodology

discussion (0)

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Reference graph

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