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arxiv: 2606.25995 · v1 · pith:6NKX7V7Xnew · submitted 2026-06-24 · 🌌 astro-ph.GA · astro-ph.CO· astro-ph.SR

The evolution of the galaxy gas-phase mass-metallicity relation from z=15 to z=0 in the COLIBRE cosmological simulations

Piyush Sharda , Joop Schaye , Robert J. McGibbon , Alejandro Ben\'itez-Llambay , Evgenii Chaikin , Carlos S. Frenk , Jacqueline Hodge , Filip Hu\v{s}ko
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Sylvia Ploeckinger Alexander J. Richings Matthieu Schaller
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Pith reviewed 2026-06-25 19:50 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.COastro-ph.SR
keywords mass-metallicity relationgalaxy evolutioncosmological simulationssupernova feedbackAGN feedbackinterstellar mediummetal enrichmentredshift evolution
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The pith

The COLIBRE simulations show the galaxy mass-metallicity relation is already in place at redshift 10 and shows no evolution until redshift 5.

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

COLIBRE cosmological hydrodynamical simulations follow the gas-phase mass-metallicity relation of star-forming galaxies from redshift 15 to the present day. The runs incorporate a multiphase interstellar medium that cools to 10 K, non-equilibrium chemistry for hydrogen and helium, metal diffusion, and a live dust model. These features allow the simulations to match observed relations across all redshifts despite uncertainties in oxygen abundance measurements. The relation forms early at z approximately 10, stays flat until z approximately 5, then develops a shallower slope at lower redshifts.

Core claim

In the COLIBRE simulations the galaxy gas-phase mass-metallicity relation is already in place at cosmic dawn (z approximately 10) and exhibits no evolution until z approximately 5. The relation is reproduced across the full stellar mass range sampled by observations at all redshifts, with the slope becoming shallower at low redshifts. The high-mass end turnover is set primarily by AGN feedback, while the low-mass end depends on core-collapse supernova feedback. Variations in star formation efficiency or oxygen depletion on dust grains have smaller effects.

What carries the argument

The mass-weighted gas-phase mass-metallicity relation for star-forming galaxies, which encodes the competition between metal production in stars and removal or dilution by feedback.

If this is right

  • The mass-metallicity relation exhibits no significant evolution between redshifts 10 and 5.
  • AGN feedback largely sets the turnover at the high-mass end of the relation.
  • Core-collapse supernova feedback controls the slope at the low-mass end.
  • The simulated relation shows numerical convergence across particle masses from 10^5 to 10^7 solar masses and box sizes from 25 to 400 comoving megaparsecs.

Where Pith is reading between the lines

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

  • Metal enrichment must proceed rapidly in the first galaxies to produce the observed relation by redshift 10.
  • Observations targeting low-mass galaxies at redshifts 5 to 10 could test the strength of supernova feedback assumed in the model.
  • The inclusion of live dust opens the possibility of predicting how dust depletion alters inferred metallicities in high-redshift observations.

Load-bearing premise

The fiducial COLIBRE model of the multiphase interstellar medium, non-equilibrium chemistry, metal diffusion, and live dust accurately represents the physical processes that set gas-phase metallicities.

What would settle it

A measurement of strong evolution in the mass-metallicity relation between redshift 10 and redshift 5 at low stellar masses would contradict the reported lack of evolution.

Figures

Figures reproduced from arXiv: 2606.25995 by Alejandro Ben\'itez-Llambay, Alexander J. Richings, Carlos S. Frenk, Evgenii Chaikin, Filip Hu\v{s}ko, Jacqueline Hodge, Joop Schaye, Matthieu Schaller, Piyush Sharda, Robert J. McGibbon, Sylvia Ploeckinger.

Figure 1
Figure 1. Figure 1: Face-on projections within a 50 comoving kpc volume of the gas-phase metallicity (left half of the image in each redshift panel) and integrated stellar light (right half of the image) as would be seen through near-IR JWST filters across cosmic time in a representative massive spiral galaxy from the COLIBRE L025m5 simulation. The metallicity scale is depicted in the top left panel, and stretches from 0.05 Z… view at source ↗
Figure 2
Figure 2. Figure 2: Left panel: Number density of star-forming COLIBRE galaxies as a function of stellar mass, measured in 0.1 dex mass bins and normalized by the simulation volume, at different redshifts in the L200m6 simulation. Increasingly darker shades of orange correspond to distributions at higher redshifts. The vertical hard cutoff at the low mass end in the distributions arises from only selecting galaxies with ≥ 10 … view at source ↗
Figure 3
Figure 3. Figure 3: Evolution of the median gas-phase mass-metallicity relation (MZR) of star-forming galaxies across cosmic time in the COLIBRE simulations at three different mass resolutions: m5 (light blue), m6 (orange), m7 (red). COLIBRE curves transition from solid to dotted if the number of galaxies drops below 20 in a given stellar mass bin, or if the resolution limit is reached (< 10 star particles per galaxy). Shaded… view at source ↗
Figure 4
Figure 4. Figure 4: Gas-phase metallicity as a function of stellar mass for all re￾solved 𝑧 = 11 − 15 star-forming galaxies in the COLIBRE simulations. The smoothed, simulation volume-weighted 2D histogram includes star-forming galaxies at these redshifts at all three resolutions (m5, m6, m7). The contours depict the 1𝜎 and 2𝜎 regions for the galaxy number density distribution per dex stellar mass per dex metallicity. White s… view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p011_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Evolution of the MZR with redshift in galaxies within different stellar mass bins per row (𝑀★ ≈ 107 , 108 , 109 , 1010 , 1011 M⊙), separated into three columns corresponding to different COLIBRE resolutions (m5, m6, m7). Shaded bands denote the 16th − 84th percentile ranges; the shaded bands are hatched for COLIBRE m6 and m7 in the top row to signify that they are affected by the resolution limit. Observat… view at source ↗
Figure 7
Figure 7. Figure 7: Schematic explaining how the free parameters in the broken power￾law model (equation 3) proposed by Curti et al. (2020) determine key aspects of the MZR. resolution, SIMBA predicts systematically lower metallicities than both COLIBRE and TNG 300. However, the simulation contains too few galaxies with 𝑀∗ ≈ 1011 M⊙ beyond 𝑧 ≈ 3 to enable a meaningful comparison with the available observations at higher redsh… view at source ↗
Figure 8
Figure 8. Figure 8: Left panel: Evolution of the median MZR in the COLIBRE L200m6 simulation at different redshifts (solid). Dashed and dotted lines represent broken power-law (BPL, equation 3) and single power-law (SPL, equation 4) fits to the MZRs, respectively. Right panels: Redshift evolution of the best-fit parameters (slope 𝛾, inflection 𝛽, saturation metallicity 𝑍0 and turnover mass 𝑀0) when the median MZRs in the left… view at source ↗
Figure 9
Figure 9. Figure 9: Effects of using different aperture sizes to measure the gas-phase metallicity on the MZR in the COLIBRE L200m6 simulation. Median MZRs from these COLIBRE simulations are shown for three aperture sizes (50 kpc, 3 kpc, and 1 kpc), indicated by progressively darker shades of orange. The shaded band indicates the 16th − 84th percentile range in the fiducial case. The meaning of solid and dotted COLIBRE curves… view at source ↗
Figure 10
Figure 10. Figure 10: The effect of using a different density cut to select gas particles to obtain oxygen abundances. Median MZRs at 𝑧 = 0 from COLIBRE sim￾ulations at m6 resolution and box size 100 Mpc (L100m6) are shown for the different density cuts, indicated by progressively darker shades of orange. The gas temperature threshold remains the same in all the cases (𝑇 < 104.5 K). The shaded band indicates the 16th −84th per… view at source ↗
Figure 12
Figure 12. Figure 12: Impact of variations in the fiducial star formation model implemented in COLIBRE on the median MZR, for a smaller (50 Mpc) box at m7 resolution (L050m7). The fiducial model is from the L400m7 simulation. 𝜖 is the star formation efficiency per freefall time, set to 0.01 in the fiducial model (Schaye et al. 2026, section 3.3). 7 8 9 10 11 log10 M /M 6 7 8 9 1 2 + lo g10 O / H z = 0 7 8 9 10 11 log10 M /M z … view at source ↗
Figure 13
Figure 13. Figure 13: Impact of variations in the fiducial supernova feedback model implemented in COLIBRE on the median MZR, for a smaller (50 Mpc) box at m7 resolution (L050m7). The fiducial model is from the L400m7 simulation. Δ𝐸CCSN refers to the energy added to a star particle due to core collapse supernovae explosions within time Δ𝑡 (Schaye et al. 2026, section 3.7). in this work are largely insensitive to the selection … view at source ↗
Figure 14
Figure 14. Figure 14: Impact of AGN feedback on the median MZR in the COLIBRE simulations at m7 resolution. The fiducial model is plotted for the L400m7 box whereas the model without AGN feedback is for the L050m7 box. Notice that axes limits differ from those in other plots. 9 10 11 log10 M /M 8.0 8.2 8.4 8.6 8.8 9.0 9.2 1 2 + lo g10 O / H z = 0 9 10 11 log10 M /M z = 1 Thermal AGN Feedback [Fiducial] Hybrid AGN Feedback 9 10… view at source ↗
Figure 15
Figure 15. Figure 15: Impact of the mode of AGN feedback (thermal versus hybrid) on the median MZR in the COLIBRE simulations of box size 100 Mpc at m6 resolution (L100m6). The fiducial thermal feedback model only injects thermal energy from AGN into the surroundings, whereas the hybrid feedback model injects both thermal and kinetic jet energy (see Section 4.2.3 for more details). Notice that axes limits differ from those in … view at source ↗
Figure 16
Figure 16. Figure 16: Median fraction of oxygen that is depleted onto dust grains, 𝑓O,depl, as a function of galaxy stellar mass, at different redshifts in the COLIBRE L200m6 simulation. 8 9 10 11 log10 M /M 7.75 8.00 8.25 8.50 8.75 9.00 1 2 + lo g10 O / H z = 0 z = 3 Diffuse Oxygen [Fiducial] Total Oxygen [PITH_FULL_IMAGE:figures/full_fig_p020_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: MZR for the L200m6 COLIBRE simulation at 𝑧 = 0 (solid) and 𝑧 = 3 (dashed), showing the impact of ignoring oxygen depletion onto dust grains. The darker shade of orange corresponds to the total oxygen abundance (gas+dust) whereas the lighter shade corresponds to the fiducial MZR that only takes the abundance of oxygen in the gas-phase into account. more efficient dust production and growth in their ISM. At… view at source ↗
read the original abstract

We present the evolution of the galaxy gas-phase mass-metallicity relation (MZR) from $z=15$ to $z=0$ in the COLIBRE cosmological hydrodynamical simulations. Amongst other novel features, COLIBRE follows the multiphase interstellar medium with gas allowed to cool to $\sim 10\,\mathrm{K}$, and includes a new chemistry model in which hydrogen and helium are tracked in non-equilibrium, metals are allowed to mix and diffuse, and the chemical network is coupled to a self-consistent live dust model. Using fiducial COLIBRE runs spanning particle masses from $10^5\,\mathrm{M_{\odot}}$ to $10^7\,\mathrm{M_{\odot}}$ and box sizes $25 - 400\,\mathrm{cMpc}$, we derive the median, mass-weighted MZRs for star-forming galaxies and compare them with a comprehensive compilation of observational data and other simulations. COLIBRE reproduces the observed MZR across cosmic time, notwithstanding the systematic uncertainties in observational measurements of the gas-phase oxygen abundances. The simulations show excellent numerical convergence and uniquely probe the full stellar mass range sampled by current observations across all redshifts. We find that the MZR is already in place at cosmic dawn ($z \approx 10$), and shows no evolution until $z \approx 5$. The slope of the MZR becomes shallower at low redshifts. The turnover at the high-mass end is largely governed by feedback from active galactic nuclei (AGN), whereas the low-mass end of the MZR sensitively depends on the strength of feedback from core collapse supernovae. Variations in the star formation efficiency or depletion of oxygen on dust grains have a more minor impact on the MZR. We identify key physical processes that shape the MZR across cosmic time and highlight where future observations can further constrain galaxy formation models.

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

0 major / 3 minor

Summary. The paper presents the evolution of the galaxy gas-phase mass-metallicity relation (MZR) from z=15 to z=0 using the COLIBRE cosmological hydrodynamical simulations. These runs incorporate a multiphase ISM cooling to ~10 K, non-equilibrium H/He chemistry, metal diffusion, and a self-consistent live dust model. Across fiducial runs with particle masses 10^5-10^7 M⊙ and box sizes 25-400 cMpc, the median mass-weighted MZRs for star-forming galaxies are shown to reproduce observational compilations at all redshifts. The MZR is already established at z≈10 with no evolution to z≈5; the slope shallows at low z. High-mass turnover is attributed to AGN feedback and low-mass end to core-collapse SN feedback, with star-formation efficiency and dust depletion having minor effects. Numerical convergence is reported as excellent.

Significance. If the central results hold, the work provides a valuable, high-dynamic-range simulation benchmark for the MZR across cosmic time, enabled by the new ISM and chemistry modules. Explicit convergence across resolution and volume, plus targeted feedback variations, strengthen the attribution of MZR features to specific physical processes. This can inform both observational interpretations and future model development, particularly where the simulations uniquely cover the full observed stellar-mass range at high redshift.

minor comments (3)
  1. [Abstract, §3] Abstract and §3: the statement that the MZR 'shows no evolution until z≈5' would benefit from an explicit quantitative definition (e.g., change in normalization or slope below a stated threshold) and a figure showing the redshift-dependent parameters.
  2. [§4] The comparison to observations notes 'systematic uncertainties in observational measurements' but does not specify which abundance calibrations or diagnostics are adopted for the simulated oxygen abundances; a short table or paragraph reconciling the two would improve clarity.
  3. [Figures 2-5] Figure captions and text should explicitly state whether the plotted MZRs are mass-weighted or luminosity-weighted and how star-forming galaxies are selected (e.g., sSFR threshold).

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of the manuscript, including the recognition that it provides a valuable high-dynamic-range benchmark for the MZR across cosmic time, enabled by the new ISM and chemistry modules, with explicit convergence tests and targeted feedback variations strengthening the physical attributions. The recommendation for minor revision is noted. No specific major comments were listed in the report for us to address point by point.

Circularity Check

0 steps flagged

No significant circularity; results are direct simulation outputs compared to external data

full rationale

The paper derives the MZR by running COLIBRE hydrodynamical simulations with explicit multiphase ISM, non-equilibrium chemistry, metal diffusion, and live dust physics, then measures median mass-weighted relations in star-forming galaxies across redshifts and compares them to independent observational compilations. No parameters are fitted to MZR data (variations in AGN/SN feedback, star-formation efficiency, and dust depletion are sensitivity tests, not fits), no self-citations justify core premises or uniqueness theorems, and no ansatzes or renamings reduce the reported evolution to inputs by construction. The claim that the MZR is in place at z≈10 with limited evolution to z≈5 is an emergent output, not a redefinition of the simulation setup. This is a standard, self-contained simulation-vs-observation comparison.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review supplies insufficient detail to enumerate free parameters, axioms, or invented entities; full text required for complete audit.

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Reference graph

Works this paper leans on

298 extracted references · 39 canonical work pages · 19 internal anchors

  1. [1]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aabc4f

  2. [2]

    Astropy: A Community Python Package for Astronomy

    Astropy: A community Python package for astronomy. , keywords =. 2013. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068 2013

  3. [3]

    2006 , series =

    A guide to NumPy , author=. 2006 , series =

    2006

  4. [4]

    , keywords =

    Array Programming with NumPy. , keywords =. doi:10.1038/s41586-020-2649-2 , archivePrefix =. 2006.10256 , primaryClass =

    Pith/arXiv arXiv doi:10.1038/s41586-020-2649-2 2006

  5. [5]

    SciPy 1.0--Fundamental Algorithms for Scientific Computing in Python

    SciPy 1.0: fundamental algorithms for scientific computing in Python. Nature Methods , keywords =. doi:10.1038/s41592-019-0686-2 , archivePrefix =. 1907.10121 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41592-019-0686-2 1907

  6. [6]

    Hunter, J. D. , Title =. Computing in Science & Engineering , Volume =

  7. [7]

    The Journal of Open Source Software , keywords =

    CMasher: Scientific colormaps for making accessible, informative and 'cmashing' plots. The Journal of Open Source Software , keywords =. doi:10.21105/joss.02004 , archivePrefix =. 2003.01069 , primaryClass =

    doi:10.21105/joss.02004 2003

  8. [8]

    The Properties of Starburst-driven Warm Ionized Outflows

    CLASSY III. The Properties of Starburst-driven Warm Ionized Outflows. , keywords =. doi:10.3847/1538-4357/ac6d56 , archivePrefix =. 2204.09181 , primaryClass =

    work page doi:10.3847/1538-4357/ac6d56

  9. [9]

    , keywords =

    A unified model for galactic discs: star formation, turbulence driving, and mass transport. , keywords =. doi:10.1093/mnras/sty852 , archivePrefix =. 1706.00106 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty852

  10. [10]

    , keywords =

    The KMOS ^ 3D Survey: Design, First Results, and the Evolution of Galaxy Kinematics from 0.7 &lt;= z &lt;= 2.7. , keywords =. doi:10.1088/0004-637X/799/2/209 , archivePrefix =. 1409.6791 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/799/2/209

  11. [11]

    , keywords =

    The evolution of turbulent galactic discs: gravitational instability, feedback, and accretion. , keywords =. doi:10.1093/mnras/stac1324 , archivePrefix =. 2202.12331 , primaryClass =

    doi:10.1093/mnras/stac1324

  12. [12]

    , keywords =

    The metallicity's fundamental dependence on both local and global galactic quantities. , keywords =. doi:10.1093/mnras/stac3594 , archivePrefix =. 2210.03755 , primaryClass =

    doi:10.1093/mnras/stac3594

  13. [13]

    , keywords =

    Characterizing mass, momentum, energy, and metal outflow rates of multiphase galactic winds in the FIRE-2 cosmological simulations. , keywords =. doi:10.1093/mnras/stab2714 , archivePrefix =. 2103.06891 , primaryClass =

    doi:10.1093/mnras/stab2714

  14. [14]

    , keywords =

    The cosmic baryon cycle and galaxy mass assembly in the FIRE simulations. , keywords =. doi:10.1093/mnras/stx1517 , archivePrefix =. 1610.08523 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx1517

  15. [15]

    , keywords =

    How supernovae launch galactic winds?. , keywords =. doi:10.1093/mnrasl/slx072 , archivePrefix =. 1704.01579 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnrasl/slx072

  16. [16]

    , keywords =

    First Results from SMAUG: Characterization of Multiphase Galactic Outflows from a Suite of Local Star-forming Galactic Disk Simulations. , keywords =. doi:10.3847/1538-4357/aba962 , archivePrefix =. 2006.16315 , primaryClass =

    work page doi:10.3847/1538-4357/aba962 2006

  17. [17]

    Kinetic Energy Decay Rates of Supersonic and Super-Alfvenic Turbulence in Star-Forming Clouds

    Kinetic Energy Decay Rates of Supersonic and Super-Alfv \'e nic Turbulence in Star-Forming Clouds. , keywords =. doi:10.1103/PhysRevLett.80.2754 , archivePrefix =. astro-ph/9712013 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.80.2754

  18. [18]

    Comparing the statistics of interstellar turbulence in simulations and observations: Solenoidal versus compressive turbulence forcing

    Comparing the statistics of interstellar turbulence in simulations and observations. Solenoidal versus compressive turbulence forcing. , keywords =. doi:10.1051/0004-6361/200912437 , archivePrefix =. 0905.1060 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200912437

  19. [19]

    Nature Astronomy , keywords =

    The sonic scale of interstellar turbulence. Nature Astronomy , keywords =. doi:10.1038/s41550-020-01282-z , archivePrefix =. 2011.06238 , primaryClass =

    work page doi:10.1038/s41550-020-01282-z 2011

  20. [20]

    , keywords =

    The chemical make-up of the Sun: A 2020 vision. , keywords =. doi:10.1051/0004-6361/202140445 , archivePrefix =. 2105.01661 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202140445 2020

  21. [21]

    Planck 2018 results. VI. Cosmological parameters. arXiv e-prints , keywords =

    2018

  22. [22]

    , keywords =

    A Universal, Local Star Formation Law in Galactic Clouds, nearby Galaxies, High-redshift Disks, and Starbursts. , keywords =. doi:10.1088/0004-637X/745/1/69 , archivePrefix =. 1109.4150 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/745/1/69

  23. [23]

    , keywords =

    Cloud-scale Molecular Gas Properties in 15 Nearby Galaxies. , keywords =. doi:10.3847/1538-4357/aac326 , archivePrefix =. 1805.00937 , primaryClass =

    work page doi:10.3847/1538-4357/aac326

  24. [24]

    , keywords =

    The Star Formation Efficiency in Nearby Galaxies: Measuring Where Gas Forms Stars Effectively. , keywords =. doi:10.1088/0004-6256/136/6/2782 , archivePrefix =. 0810.2556 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-6256/136/6/2782

  25. [25]

    , keywords =

    Galactic Stellar and Substellar Initial Mass Function. , keywords =. doi:10.1086/376392 , archivePrefix =. astro-ph/0304382 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/376392

  26. [26]

    , keywords =

    A General Theory of Turbulence-regulated Star Formation, from Spirals to Ultraluminous Infrared Galaxies. , keywords =. doi:10.1086/431734 , archivePrefix =. astro-ph/0505177 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/431734

  27. [27]

    arXiv e-prints , keywords =

    Delayed Massive-Star Mechanical Feedback at Low Metallicity. arXiv e-prints , keywords =

  28. [28]

    , keywords =

    Evidence for supernova feedback sustaining gas turbulence in nearby star-forming galaxies. , keywords =. doi:10.1051/0004-6361/202038223 , archivePrefix =. 2006.10764 , primaryClass =

    doi:10.1051/0004-6361/202038223 2006

  29. [29]

    , keywords =

    Density Studies of MHD Interstellar Turbulence: Statistical Moments, Correlations and Bispectrum. , keywords =. doi:10.1088/0004-637X/693/1/250 , archivePrefix =. 0811.0822 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/693/1/250

  30. [30]

    , keywords =

    Dissipation in Compressible Magnetohydrodynamic Turbulence. , keywords =. doi:10.1086/311718 , archivePrefix =. astro-ph/9809357 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/311718

  31. [31]

    , keywords =

    A Constant Molecular Gas Depletion Time in Nearby Disk Galaxies. , keywords =. doi:10.1088/2041-8205/730/2/L13 , archivePrefix =. 1102.1720 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/2041-8205/730/2/l13 2041

  32. [32]

    , keywords =

    How stellar feedback simultaneously regulates star formation and drives outflows. , keywords =. doi:10.1093/mnras/stw2888 , archivePrefix =. 1510.05650 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stw2888

  33. [33]

    Sub-Eddington Star-Forming Regions are Super-Eddington: Momentum Driven Outflows from Supersonic Turbulence

    Sub-Eddington star-forming regions are super-Eddington: momentum-driven outflows from supersonic turbulence. , keywords =. doi:10.1093/mnras/stv2331 , archivePrefix =. 1411.1769 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2331

  34. [34]

    , keywords =

    A Unified Model for the Coevolution of Galaxies and Their Circumgalactic Medium: The Relative Roles of Turbulence and Atomic Cooling Physics. , keywords =. doi:10.3847/1538-4357/acf3ea , archivePrefix =. 2211.09755 , primaryClass =

    doi:10.3847/1538-4357/acf3ea

  35. [35]

    , keywords =

    The Star Formation Rate in the Gravoturbulent Interstellar Medium. , keywords =. doi:10.3847/1538-4357/aad002 , archivePrefix =. 1801.05428 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aad002

  36. [36]

    , keywords =

    The Star Formation Rate of Turbulent Magnetized Clouds: Comparing Theory, Simulations, and Observations. , keywords =. doi:10.1088/0004-637X/761/2/156 , archivePrefix =. 1209.2856 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/761/2/156

  37. [37]

    , keywords =

    A multishock model for the density variance of anisotropic, highly magnetized, supersonic turbulence. , keywords =. doi:10.1093/mnras/stab1037 , archivePrefix =. 2102.00629 , primaryClass =

    doi:10.1093/mnras/stab1037

  38. [38]

    , keywords =

    The Link between Turbulence, Magnetic Fields, Filaments, and Star Formation in the Central Molecular Zone Cloud G0.253+0.016. , keywords =. doi:10.3847/0004-637X/832/2/143 , archivePrefix =. 1609.05911 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/0004-637x/832/2/143

  39. [39]

    , keywords =

    Testing star formation laws in a starburst galaxy at redshift 3 resolved with ALMA. , keywords =. doi:10.1093/mnras/sty886 , archivePrefix =. 1712.03661 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty886

  40. [40]

    , keywords =

    Testing star formation laws on spatially resolved regions in a z 4.3 starburst galaxy. , keywords =. doi:10.1093/mnras/stz1543 , archivePrefix =. 1906.01173 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stz1543 1906

  41. [41]

    , keywords =

    The Global Schmidt Law in Star-forming Galaxies. , keywords =. doi:10.1086/305588 , archivePrefix =. astro-ph/9712213 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/305588

  42. [42]

    , keywords =

    Feedback-regulated star formation in molecular clouds and galactic discs. , keywords =. doi:10.1093/mnras/stt866 , archivePrefix =. 1301.3905 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stt866

  43. [43]

    , keywords =

    The SAMI galaxy survey: gas velocity dispersions in low-z star-forming galaxies and the drivers of turbulence. , keywords =. doi:10.1093/mnras/staa1272 , archivePrefix =. 2005.04874 , primaryClass =

    doi:10.1093/mnras/staa1272 2005

  44. [44]

    , keywords =

    Galactic star formation and accretion histories from matching galaxies to dark matter haloes. , keywords =. doi:10.1093/mnras/sts261 , archivePrefix =. 1205.5807 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sts261

  45. [45]

    , keywords =

    A new method for spatially resolving the turbulence-driving mixture in the ISM with application to the Small Magellanic Cloud. , keywords =. doi:10.1093/mnras/stad2718 , archivePrefix =. 2309.10755 , primaryClass =

    doi:10.1093/mnras/stad2718

  46. [46]

    , keywords =

    Photoelectric heating of interstellar gas. , keywords =. doi:10.1086/190513 , adsurl =

    doi:10.1086/190513

  47. [47]

    , keywords =

    Rosseland and Planck mean opacities for protoplanetary discs. , keywords =. doi:10.1051/0004-6361:20031279 , archivePrefix =. astro-ph/0308344 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361:20031279

  48. [48]

    , keywords =

    Photodissociation of H _ 2 in protogalaxies: modelling self-shielding in three-dimensional simulations. , keywords =. doi:10.1111/j.1365-2966.2011.19538.x , archivePrefix =. 1106.3523 , primaryClass =

    doi:10.1111/j.1365-2966.2011.19538.x 2011

  49. [49]

    , keywords =

    The photodissociation and chemistry of CO isotopologues: applications to interstellar clouds and circumstellar disks. , keywords =. doi:10.1051/0004-6361/200912129 , archivePrefix =. 0906.3699 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/200912129

  50. [50]

    , keywords =

    Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations. , keywords =. doi:10.3847/1538-4365/ac9b1d , archivePrefix =. 2210.08024 , primaryClass =

    doi:10.3847/1538-4365/ac9b1d

  51. [51]

    Photodissociation regions. I. Basic model. , keywords =. doi:10.1086/163111 , adsurl =

    doi:10.1086/163111

  52. [52]

    , keywords =

    The UMIST Database for Astrochemistry 2022. , keywords =. doi:10.1051/0004-6361/202346908 , archivePrefix =. 2311.03936 , primaryClass =

    doi:10.1051/0004-6361/202346908 2022

  53. [53]

    , keywords =

    Cosmic-Ray--induced Photodissociation and Photoionization Rates of Interstellar Molecules. , keywords =. doi:10.1086/168117 , adsurl =

    doi:10.1086/168117

  54. [54]

    , keywords =

    H I-to-H _ 2 Transitions in Dust-free Interstellar Gas. , keywords =. doi:10.3847/1538-4357/ac167b , archivePrefix =. 2105.01681 , primaryClass =

    doi:10.3847/1538-4357/ac167b

  55. [55]

    , keywords =

    Production of atomic hydrogen by cosmic rays in dark clouds. , keywords =. doi:10.1051/0004-6361/201834008 , archivePrefix =. 1809.04168 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201834008

  56. [56]

    The basic model, library of chemical reactions, and chemistry among C, N, and O compounds

    A model for gas phase chemistry in interstellar clouds: I. The basic model, library of chemical reactions, and chemistry among C, N, and O compounds. , keywords =. doi:10.1086/190665 , adsurl =

    doi:10.1086/190665

  57. [58]

    , keywords =

    The C/CO Ratio in Dense Interstellar Clouds. , keywords =. doi:10.1086/185073 , adsurl =

    doi:10.1086/185073

  58. [59]

    , keywords =

    Photodissociation and photoionisation of atoms and molecules of astrophysical interest. , keywords =. doi:10.1051/0004-6361/201628742 , archivePrefix =. 1701.04459 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201628742

  59. [60]

    , keywords =

    Sensitivity analyses of dense cloud chemical models. , keywords =. doi:10.1051/0004-6361/200913856 , archivePrefix =. 1004.1902 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/200913856 1902

  60. [61]

    On the effect of the Cosmic Microwave Background in high-redshift (sub-)millimeter observations

    On the Effect of the Cosmic Microwave Background in High-redshift (Sub-)millimeter Observations. , keywords =. doi:10.1088/0004-637X/766/1/13 , archivePrefix =. 1302.0844 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/766/1/13

  61. [62]

    CO lines in high redshift galaxies: perspective for future mm instruments

    CO lines in high redshift galaxies: perspective for future MM instruments. , keywords =. doi:10.48550/arXiv.astro-ph/9902286 , archivePrefix =. astro-ph/9902286 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9902286

  62. [63]

    , keywords =

    A Heuristic Prediction of the Cosmic Evolution of the Co-luminosity Functions. , keywords =. doi:10.1088/0004-637X/702/2/1321 , archivePrefix =. 0907.3091 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/702/2/1321

  63. [64]

    UCLCHEM: A Gas-Grain Chemical Code

    UCLCHEM: A Gas-grain Chemical Code for Clouds, Cores, and C-Shocks. , keywords =. doi:10.3847/1538-3881/aa773f , archivePrefix =. 1705.10677 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aa773f

  64. [65]

    , keywords =

    Evaporation of ices near massive stars: models based on laboratory temperature programmed desorption data. , keywords =. doi:10.1111/j.1365-2966.2004.08273.x , archivePrefix =. astro-ph/0406054 , primaryClass =

    doi:10.1111/j.1365-2966.2004.08273.x 2004

  65. [66]

    Astrochem: Abundances of chemical species in the interstellar medium

  66. [68]

    , keywords =

    On the Stability and Evolution of Isolated BOK Globules. , keywords =. doi:10.1086/307823 , adsurl =

    doi:10.1086/307823

  67. [69]

    doi:10.1111/j.1365-2966.2011.18648.x , archiveprefix =

    Approximations for modelling CO chemistry in giant molecular clouds: a comparison of approaches. , keywords =. doi:10.1111/j.1365-2966.2011.20260.x , archivePrefix =. 1102.0670 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.20260.x 2011

  68. [70]

    , keywords =

    Modelling CO formation in the turbulent interstellar medium. , keywords =. doi:10.1111/j.1365-2966.2009.15718.x , archivePrefix =. 0907.4081 , primaryClass =

    doi:10.1111/j.1365-2966.2009.15718.x 2009

  69. [71]

    , keywords =

    Star formation in metal-poor gas clouds. , keywords =. doi:10.1111/j.1365-2966.2012.21737.x , archivePrefix =. 1203.4251 , primaryClass =

    doi:10.1111/j.1365-2966.2012.21737.x 2012

  70. [72]

    , keywords =

    Thermal and Fragmentation Properties of Star-forming Clouds in Low-Metallicity Environments. , keywords =. doi:10.1086/429955 , archivePrefix =. astro-ph/0503010 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/429955

  71. [73]

    Shielded gas

    Non-equilibrium chemistry and cooling in the diffuse interstellar medium - II. Shielded gas. , keywords =. doi:10.1093/mnras/stu1046 , archivePrefix =. 1403.6155 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stu1046

  72. [74]

    CN and HCN in Dense Interstellar Clouds

    CN and HCN in Dense Interstellar Clouds. , keywords =. doi:10.1086/432864 , archivePrefix =. astro-ph/0506535 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/432864

  73. [75]

    , keywords =

    The interstellar gas-phase chemistry of HCN and HNC. , keywords =. doi:10.1093/mnras/stu1089 , archivePrefix =. 1406.1696 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stu1089

  74. [76]

    , keywords =

    KROME - a package to embed chemistry in astrophysical simulations. , keywords =. doi:10.1093/mnras/stu114 , archivePrefix =. 1311.1070 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stu114

  75. [77]

    , keywords =

    Ultraviolet H _ 2 luminescence in molecular clouds induced by cosmic rays. , keywords =. doi:10.1051/0004-6361/202348168 , archivePrefix =. 2312.02062 , primaryClass =

    doi:10.1051/0004-6361/202348168

  76. [78]

    and Wolfire, Mark G

    Gong, Munan and Ostriker, Eve C. and Wolfire, Mark G. , number =. 2016 , journal =. doi:10.3847/1538-4357/aa7561 , arxivId =

    doi:10.3847/1538-4357/aa7561 2016

  77. [79]

    , keywords =

    Modeling primordial gas in numerical cosmology. , keywords =. doi:10.1016/S1384-1076(97)00010-9 , archivePrefix =. astro-ph/9608040 , primaryClass =

    Pith/arXiv arXiv doi:10.1016/s1384-1076(97)00010-9

  78. [80]

    doi:10.1086/171063 , adsurl =

    , keywords =. doi:10.1086/171063 , adsurl =

    doi:10.1086/171063

  79. [81]

    , keywords =

    A Hydrodynamic Approach to Cosmology: Methodology. , keywords =. doi:10.1086/191630 , adsurl =

    doi:10.1086/191630

  80. [82]

    , year = 1973, month = may, volume =

    Radiative and Dielectronic Recombination Coefficients for Complex Ions. , year = 1973, month = may, volume =

    1973

Showing first 80 references.