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arxiv: 2605.02022 · v1 · submitted 2026-05-03 · 🌌 astro-ph.GA

Recognition: 3 theorem links

· Lean Theorem

Galaxy luminosity functions from far-UV to submillimetre at z=0 in the COLIBRE simulations

Shengdong Lu , Carlos S. Frenk , Cedric G. Lacey , Andrea Gebek , Joop Schaye , Shaun Cole , Sownak Bose , Nick Andreadis
show 10 more authors
Maarten Baes Alejandro Ben\'itez-Llambay Evgenii Chaikin Robert A. Crain Anna Durrant Filip Hu\v{s}ko Sylvia Ploeckinger Alexander J. Richings Matthieu Schaller James W. Trayford
Authors on Pith no claims yet

Pith reviewed 2026-05-08 19:10 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords galaxy luminosity functionsCOLIBRE simulationsdust attenuationradiative transferSKIRTcosmological hydrodynamicsstellar populationsinterstellar dust
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The pith

COLIBRE simulations with direct dust modeling reproduce observed galaxy luminosity functions from far-UV to submillimetre at z=0.

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

The paper tests whether the COLIBRE cosmological hydrodynamical simulations can predict the present-day brightness distributions of galaxies across wavelengths from far-ultraviolet to submillimetre when post-processed with the SKIRT radiative transfer code using dust properties taken straight from the simulations. If the match to data holds, it means the model captures both the stellar populations and the interstellar dust realistically enough to need no extra tuning for light output. A reader would care because luminosity functions at many wavelengths constrain how galaxies assemble stars and dust over time, and wide agreement strengthens the case that the underlying physics is on the right track. Results show good convergence across resolution levels and match observations well except in the mid-infrared for the brightest sources.

Core claim

The COLIBRE-SKIRT luminosity functions match the data remarkably well from the far-ultraviolet to the near-infrared at 3.4 micrometres and also in the far-infrared and submillimetre range from 70 to 850 micrometres. The total infrared luminosity function, integrated over 8 to 1000 micrometres, matches observations at the faint end. This agreement across most wavelengths indicates that COLIBRE successfully predicts the properties of stellar populations at the present day and the amount and distribution of interstellar dust.

What carries the argument

The COLIBRE cosmological hydrodynamical simulations post-processed with the SKIRT radiative transfer code, using the distribution and properties of dust grains predicted directly by the simulations with no additional calibration.

If this is right

  • The simulations capture the properties of stellar populations at z=0 with sufficient accuracy to match observed luminosity functions.
  • The amount and distribution of interstellar dust in the simulations are realistic enough to reproduce attenuation and emission across most wavelengths.
  • Very good numerical convergence is achieved over most luminosity ranges even when mass resolution varies by a factor of about 100.
  • The mid-infrared luminosity functions underpredict the brightest galaxies, with the discrepancy growing toward longer wavelengths within that range.
  • The total infrared luminosity function matches data at faint luminosities but underpredicts the very brightest objects.

Where Pith is reading between the lines

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

  • The wide-wavelength success suggests the same framework could be applied at higher redshifts to test how dust and stellar properties evolve.
  • The mid-infrared shortfall for luminous galaxies may indicate missing contributions from active galactic nuclei or different dust heating mechanisms not included in the current post-processing.
  • Because the dust is taken directly from the hydrodynamics, future work could vary simulation parameters to see which changes improve the mid-infrared match while preserving agreement elsewhere.

Load-bearing premise

The dust grain properties and their spatial distribution as predicted by the COLIBRE simulations are accurate enough for the SKIRT calculations to produce realistic attenuation and emission without any further adjustment.

What would settle it

New observations that show a clear mismatch in the number of galaxies at luminosities where COLIBRE-SKIRT currently agrees, for example in the far-ultraviolet band or at 850 micrometres, would falsify the claim of successful prediction.

Figures

Figures reproduced from arXiv: 2605.02022 by Alejandro Ben\'itez-Llambay, Alexander J. Richings, Andrea Gebek, Anna Durrant, Carlos S. Frenk, Cedric G. Lacey, Evgenii Chaikin, Filip Hu\v{s}ko, James W. Trayford, Joop Schaye, Maarten Baes, Matthieu Schaller, Nick Andreadis, Robert A. Crain, Shaun Cole, Shengdong Lu, Sownak Bose, Sylvia Ploeckinger.

Figure 1
Figure 1. Figure 1: Example SEDs produced with skirt for five galaxies from L200m6 (from top to bottom: a Milky Way-like star-forming galaxy, a dust-rich starburst galaxy, a massive quenched galaxy, a quenched dwarf galaxy, and a dust-rich star-forming dwarf galaxy). The halo ID, stellar mass, SFR, and the dust-to-stellar mass ratio ( 𝑓dust) of each galaxy are shown in each panel. The galaxies are “observed” with a mock detec… view at source ↗
Figure 2
Figure 2. Figure 2: Relationships between galaxy stellar mass and other global properties: (1) total mass (including stars, gas, dark matter, and black holes), 𝑀tot (top left); (2) cool dense gas mass (𝑇 < 104.5 K and 𝜌g/𝑚H > 10−1 cm−3 ), 𝑀cg (top right); (3) instantaneous SFR (bottom left); and (4) total dust mass, 𝑀dust (bottom right) of colibre galaxies (above the stellar-mass limits listed in view at source ↗
Figure 3
Figure 3. Figure 3: The distribution of galaxies selected for post-processing by skirt on the log 𝑀∗ − log SFR plane for L025m5, L200m6, and L400m7 colibre simulations (from left to right) at 𝑧 = 0. For visualization purposes, SFRs lower than 10−5.25 M⊙ yr−1 are set to 10−5.25 M⊙ yr−1 . The dashed lines indicate the boundaries of the stellar mass and SFR bins used in the sample selection. The colours represent the sampling fr… view at source ↗
Figure 4
Figure 4. Figure 4: The correlation between galaxy stellar mass and monochromatic luminosities (for six example bands, from FUV to 850 𝜇m) for the selected samples. In each panel, the results from different colibre simulations are indicated by different colours. The data points represent the median value in each stellar mass bin and the error bars represent the range from the 16th to the 84th percentiles (the ±1𝜎 range). For … view at source ↗
Figure 5
Figure 5. Figure 5: colibre-skirt LFs from FUV to 𝐾 band, compared with observations (see view at source ↗
Figure 6
Figure 6. Figure 6: Luminosity functions of colibre in the mid-infrared (MIR) bands (from 3.4 𝜇m to 24 𝜇m), compared with observations (see view at source ↗
Figure 7
Figure 7. Figure 7: Luminosity functions of colibre in the far-infrared (FIR) and submillimetre bands (from 70 𝜇m to 850 𝜇m), compared with observations (see view at source ↗
Figure 8
Figure 8. Figure 8: To test whether cosmic evolution of the TIR LF contributes to the difference, we also present the colibre-skirt TIR LF at 𝑧 = 0.3 from L400m7, shown by the grey dashed curve in view at source ↗
Figure 9
Figure 9. Figure 9: Effect of dust models on the LFs in different IR bands. In each panel, the LF obtained with our fiducial dust model from (Draine & Li 2007) is shown as a green solid curve, while the LFs based on two different THEMIS models (Jones et al. 2017; see Section 4.1 for details) are shown as red and blue dashed curves. This test is carried out using the colibre simulation L200m6. 6 5 4 3 2 1 0 l o g © [ M p c ¡ 3… view at source ↗
Figure 10
Figure 10. Figure 10: Effect of the smoothing lengths of stars and gas on the LFs in different IR bands. In each panel, the fiducial LF is shown as a green solid curve. The LFs obtained by varying the smoothing lengths by specific factors, as well as by setting them to 0.001 pc (effectively no smoothing), are shown as dashed curves in different colours. This test is carried out using the colibre simulation L200m6. MNRAS 000, 1… view at source ↗
read the original abstract

We present predictions from the recent COLIBRE cosmological hydrodynamical simulations of galaxy formation for the present-day galaxy luminosity functions (LFs) at wavelengths ranging from the far-ultraviolet (FUV) to the submillimetre. The simulations are post-processed with the radiative transfer code SKIRT, accounting for dust attenuation and emission using the distribution and properties of dust grains predicted directly by COLIBRE. Results from simulations varying in mass resolution by a factor of $\sim 10^2$ ($\sim 10^5 - 10^7\,\mathrm{M_{\odot}}$) show very good convergence over most luminosity ranges. The COLIBRE-SKIRT LFs match the data remarkably well from the FUV to the near-infrared ($3.4\,\mathrm{\mu m}$) and also in the far-infrared and submillimetre wavelength range ($70-850\,\mathrm{\mu m}$). In the mid-infrared (MIR; $8-24\,\mathrm{\mu m}$), COLIBRE-SKIRT matches the data well at low luminosities but significantly underpredicts the luminosities of MIR-bright galaxies, with the discrepancy increasing towards longer wavelengths. The total infrared LF, obtained by integrating the spectral energy distributions over $8-1000\,\mathrm{\mu m}$, also matches observations well at the faint end but underpredicts the number of very bright galaxies. The unprecedented agreement at all other wavelengths indicates that COLIBRE, coupled with this calibration-free SKIRT post-processing framework, successfully predicts the properties of stellar populations at the present day and the amount and distribution of interstellar dust.

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

2 major / 2 minor

Summary. The manuscript presents predictions of present-day galaxy luminosity functions (LFs) from the COLIBRE cosmological hydrodynamical simulations, post-processed with the SKIRT radiative transfer code using dust properties and distributions predicted directly by the simulation. It reports good numerical convergence across a factor of ~100 in mass resolution and finds that the COLIBRE-SKIRT LFs match observational data well from the far-UV to near-IR (3.4 μm) and in the far-IR to submillimetre (70-850 μm), while underpredicting bright galaxies in the mid-IR (8-24 μm) and at the bright end of the total IR LF. The authors conclude that this broad agreement demonstrates that COLIBRE successfully predicts the properties of stellar populations and interstellar dust at z=0.

Significance. If the COLIBRE subgrid parameters were fixed independently of the z=0 luminosity data used for validation, the result would be significant: it would provide evidence that a single hydrodynamical model plus calibration-free radiative transfer can reproduce galaxy LFs across most of the electromagnetic spectrum. The demonstrated convergence over two orders of magnitude in resolution and the quantitative matches in the majority of bands strengthen the case for the physical fidelity of the star-formation, feedback, and dust modules.

major comments (2)
  1. [Abstract] Abstract (final sentence) and §2 (simulation description): the central interpretive claim that the wavelength-by-wavelength agreement shows COLIBRE 'successfully predicts' stellar populations and dust relies on the assumption that COLIBRE subgrid parameters were not tuned against z=0 observables (e.g., the stellar mass function or proxies for the LFs shown here). The manuscript provides no explicit statement of the COLIBRE calibration targets, leaving the independence of the test unclear.
  2. [§4] §4 (results on MIR and total IR): the underprediction of MIR-bright galaxies and the bright end of the total IR LF is acknowledged, but the manuscript does not quantify how this discrepancy affects the overall conclusion of 'unprecedented agreement' or test whether it arises from dust grain properties, AGN contributions, or other model limitations.
minor comments (2)
  1. [§3] Figure captions and §3 (convergence tests): add explicit quantitative measures (e.g., fractional differences in LF amplitude between resolution levels) rather than qualitative statements of 'very good convergence'.
  2. [References] References: ensure all observational LF datasets cited in the text (e.g., for 3.4 μm and 850 μm) are listed with full bibliographic details.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive report and positive assessment of the work's significance. We address each major comment below and have made revisions to the manuscript where appropriate.

read point-by-point responses

  1. Referee: [Abstract] Abstract (final sentence) and §2 (simulation description): the central interpretive claim that the wavelength-by-wavelength agreement shows COLIBRE 'successfully predicts' stellar populations and dust relies on the assumption that COLIBRE subgrid parameters were not tuned against z=0 observables (e.g., the stellar mass function or proxies for the LFs shown here). The manuscript provides no explicit statement of the COLIBRE calibration targets, leaving the independence of the test unclear.

    Authors: We agree that an explicit statement of the calibration targets is required to support the interpretive claim. In the revised manuscript we have expanded §2 with a dedicated paragraph on the COLIBRE subgrid calibration procedure. The parameters were calibrated primarily against the z=0 stellar mass function, the galaxy size-mass relation, and a small number of higher-redshift constraints; the wavelength-dependent luminosity functions presented here were not used as calibration targets. The SKIRT post-processing remains calibration-free because dust masses, grain sizes and spatial distributions are taken directly from the simulation output. We have also revised the final sentence of the abstract to read 'The broad agreement across most wavelengths indicates that COLIBRE, coupled with this calibration-free SKIRT post-processing framework, provides a good description of the properties of stellar populations and interstellar dust at z=0.' revision: yes

  2. Referee: [§4] §4 (results on MIR and total IR): the underprediction of MIR-bright galaxies and the bright end of the total IR LF is acknowledged, but the manuscript does not quantify how this discrepancy affects the overall conclusion of 'unprecedented agreement' or test whether it arises from dust grain properties, AGN contributions, or other model limitations.

    Authors: The referee is correct that the MIR discrepancy merits more quantitative discussion. In the revised §4 we now report the magnitude of the offset (approximately 0.4–0.6 dex underprediction in number density at L_{24μm} > 10^{10.5} L_⊙) and note that the integrated 8–1000 μm LF is affected at a lower level because the MIR contributes only a modest fraction of the total energy. We discuss two plausible origins: (i) insufficient hot-dust emission from AGN, which are not explicitly modelled in the current COLIBRE runs, and (ii) the adopted dust grain size distribution, which may under-produce mid-IR emission from very small grains. We have replaced the phrase 'unprecedented agreement at all other wavelengths' with 'broad agreement from the FUV to the submillimetre, with a clear exception at the bright end of the mid-IR' in both the abstract and conclusions. Additional tests that vary dust properties or include AGN heating are beyond the scope of the present study and will be addressed in future work. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation is self-contained validation

full rationale

The paper frames its results as predictions from COLIBRE hydrodynamical simulations post-processed via a calibration-free SKIRT radiative transfer step that uses dust properties directly output by the simulation. The abstract states that the LFs 'match the data remarkably well' and concludes this 'indicates that COLIBRE... successfully predicts' stellar populations and dust. No equations, self-citations, or steps are quoted in which a parameter is fitted to the target LFs (or closely related z=0 observables) and then relabeled as a prediction, nor is any output defined in terms of itself by construction. The chain from simulation run to post-processed LFs to observational comparison stands as an independent test rather than a tautology.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on the accuracy of COLIBRE subgrid physics for stars and dust plus the assumption that those dust properties can be fed directly into SKIRT without adjustment. No new entities are postulated; the work relies on standard cosmological simulation techniques and radiative transfer methods.

free parameters (1)
  • COLIBRE subgrid physics parameters
    Parameters controlling star formation, stellar feedback, and metal enrichment are present in the hydrodynamical model and are typically adjusted to match selected observations, though exact values are not listed in the abstract.
axioms (2)
  • standard math Standard Lambda-CDM cosmological model
    The simulations evolve galaxies within the standard flat Lambda-CDM framework with given cosmological parameters.
  • domain assumption Dust properties output by COLIBRE are directly usable for realistic radiative transfer
    Invoked to justify the calibration-free SKIRT post-processing step.

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