pith. sign in

arxiv: 2606.10027 · v1 · pith:NUSTIBRKnew · submitted 2026-06-08 · 🌌 astro-ph.GA · astro-ph.CO· astro-ph.IM

Learning the Universe: The Structure of Dust Attenuation Curves in Galaxy Simulations

Laura Sommovigo , Deaglan J. Bartlett , Rachel K. Cochrane , Matthew Ho , Christopher C. Lovell , Rachel S. Somerville This is my paper

Pith reviewed 2026-06-27 15:46 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.COastro-ph.IM
keywords dust attenuation curvesgalaxy simulationssymbolic regressioninformation-ordered bottleneckSED fittingTNG50TNG100dust mixtures
0
0 comments X

The pith

Four parameters suffice to describe the full diversity of dust attenuation curves in galaxy simulations.

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

The paper shows that synthetic attenuation curves generated from TNG50 and TNG100 galaxies, post-processed with the SKIRT radiative transfer code for three different dust mixtures, require exactly four parameters to capture their range of shapes. Information-ordered bottleneck analysis first establishes this minimal number, after which symbolic regression produces an explicit four-parameter functional form. This new model recovers both the attenuation curves themselves and the resulting emergent fluxes more accurately than earlier parameterizations. The parameters correspond to UV bump strength, FUV slope, transition curvature, and optical slope, and they correlate with galaxy properties such as star-formation rate surface density, metallicity, and dust geometry. Scaling relations derived from the same regression connect the parameters directly to quasi-observable quantities, allowing realistic curves to be assigned in SED fitting without repeated radiative-transfer runs.

Core claim

Via Information-Ordered Bottleneck analysis on a library of synthetic attenuation curves from TNG50 and TNG100 galaxies post-processed with SKIRT using three dust mixtures, exactly four parameters are needed to capture the diversity of attenuation curves. Symbolic regression then yields a new four-parameter model that outperforms existing parameterizations in recovering both attenuation curves and emergent fluxes across all mixtures. The four parameters have clear physical interpretations: UV bump strength, FUV slope, UV-bump transition curvature, and large-scale optical slope. Their correlations with galaxy properties are primarily regulated by star-formation rate surface density, metallici

What carries the argument

Information-Ordered Bottleneck analysis to determine parameter count, followed by symbolic regression to obtain an explicit four-parameter attenuation function from the synthetic curve library.

If this is right

  • The four parameters correlate with galaxy properties regulated mainly by star-formation rate surface density, metallicity, and stellar-dust geometry.
  • Correlations are largely preserved across the three dust mixtures, except for parameters tied to the UV bump which retain stronger dependence on grain composition.
  • Symbolic-regression scaling relations connect all four parameters to quasi-observable galaxy properties for direct use in modeling.
  • The model supplies a route to assign realistic attenuation curves in SED fitting and forward modeling of galaxy populations without performing radiative-transfer calculations.

Where Pith is reading between the lines

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

  • The four-parameter structure could be tested by fitting the same functional form to attenuation curves measured in large observational surveys to check consistency with the simulation results.
  • If the scaling relations hold, they would allow attenuation curves to be predicted from readily available photometric or spectroscopic data without needing full hydrodynamic or radiative-transfer runs.
  • The separation of bump-sensitive parameters from the others suggests that grain-composition effects can be isolated from geometric and star-formation effects in future modeling.

Load-bearing premise

The synthetic attenuation curves produced by TNG50 and TNG100 galaxies post-processed with SKIRT using Milky Way, SMC, and stellar dust mixtures represent the true diversity present in real galaxies.

What would settle it

A set of observed attenuation curves from real galaxies, derived independently of the simulations, that cannot be adequately fit by any four-parameter function or where the new model yields systematically worse flux predictions than existing forms.

read the original abstract

Dust attenuation is a major source of systematic uncertainty in both SED fitting and forward modeling of galaxy populations, yet the functional form used to parameterize attenuation curves has received surprisingly little systematic scrutiny. Particular unanswered questions include: how many free parameters are genuinely needed, and which analytic expression best captures the full diversity of attenuation curve shapes in galaxies across cosmic time? Using a large library of synthetic attenuation curves from TNG50 and TNG100 galaxies post-processed with the SKIRT radiative transfer code using three dust mixtures (Milky Way, SMC, and stellar dust), we show via Information-Ordered Bottleneck analysis that exactly four parameters are needed to capture the diversity of attenuation curves. Guided by this result, we use symbolic regression to derive a new, interpretable four-parameter attenuation model that outperforms existing parameterizations in recovering both attenuation curves and emergent fluxes across all dust mixtures explored. The four parameters of this model have clear physical interpretations: UV bump strength, FUV slope, UV-bump transition curvature, and large-scale optical slope. Their correlations with galaxy properties are primarily regulated by star-formation rate surface density, metallicity, and stellar-dust geometry, and are largely preserved across dust mixtures -- except for the bump-sensitive parameters, which retain a stronger dependence on grain composition. We further provide symbolic-regression scaling relations linking all four parameters to quasi-observable galaxy properties, offering a physically motivated route to assign realistic attenuation curves in SED fitting and forward modeling without radiative-transfer calculations.

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 / 0 minor

Summary. The paper generates a library of synthetic dust attenuation curves from TNG50 and TNG100 galaxies post-processed with SKIRT using three dust mixtures (Milky Way, SMC, stellar). Information-Ordered Bottleneck analysis on this library indicates that exactly four parameters suffice to capture the diversity. Symbolic regression then yields a new four-parameter model (UV bump strength, FUV slope, UV-bump transition curvature, large-scale optical slope) that outperforms existing forms when recovering curves and emergent fluxes on the same library. Correlations of the parameters with galaxy properties (regulated primarily by SFR surface density, metallicity, and stellar-dust geometry) are analyzed, and symbolic-regression scaling relations to quasi-observable properties are provided for use in SED fitting.

Significance. If the TNG+SKIRT library is representative, the work supplies an interpretable four-parameter attenuation model with clear physical meanings and scaling relations that could reduce reliance on full radiative-transfer calculations in SED fitting and population synthesis. The Information-Ordered Bottleneck step for determining parameter count and the symbolic-regression derivation for interpretability are methodological strengths that strengthen the case for this specific functional form over ad-hoc choices.

major comments (2)
  1. [Abstract] Abstract: the assertion that four parameters capture the diversity of attenuation curves 'in galaxies across cosmic time' rests on the untested assumption that the TNG50/TNG100+SKIRT synthetic library (with only three dust mixtures) spans the full range of shapes produced by real variations in grain composition, star-dust geometry, and evolutionary states; no comparison to observed attenuation curves (e.g., via UV slope, IRX-β, or Balmer decrement measurements) is described.
  2. [Abstract] Abstract: the scaling relations that map the four parameters to galaxy properties are fitted quantities derived from the identical simulation library used to train and validate the model via symbolic regression, so their claimed physical motivation and applicability beyond the TNG+SKIRT setup require explicit qualification or cross-validation on independent data.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments. We respond to each major comment below, agreeing where revisions are needed to qualify the scope of our simulation-based results.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the assertion that four parameters capture the diversity of attenuation curves 'in galaxies across cosmic time' rests on the untested assumption that the TNG50/TNG100+SKIRT synthetic library (with only three dust mixtures) spans the full range of shapes produced by real variations in grain composition, star-dust geometry, and evolutionary states; no comparison to observed attenuation curves (e.g., via UV slope, IRX-β, or Balmer decrement measurements) is described.

    Authors: We agree that the abstract phrasing risks implying coverage of all real galaxies, which exceeds the scope of our TNG+SKIRT library (limited to three dust mixtures). The four-parameter result and model apply specifically to the diversity within this synthetic library, which spans galaxies across redshifts and properties in TNG50/TNG100. We will revise the abstract to explicitly limit the claim to the TNG+SKIRT library and add a sentence noting the absence of direct observational comparisons (e.g., UV slope or IRX-β) as a limitation of the current work. TNG is calibrated to observed galaxy statistics, but this provides only indirect support; we do not claim the library exhausts all possible grain or geometry variations. revision: yes

  2. Referee: [Abstract] Abstract: the scaling relations that map the four parameters to galaxy properties are fitted quantities derived from the identical simulation library used to train and validate the model via symbolic regression, so their claimed physical motivation and applicability beyond the TNG+SKIRT setup require explicit qualification or cross-validation on independent data.

    Authors: We agree that the scaling relations are derived from the same library used for the Information-Ordered Bottleneck and symbolic regression steps. Their physical motivation is grounded in the correlations identified within the simulations (primarily with SFR surface density, metallicity, and stellar-dust geometry), which are analyzed and shown to be largely preserved across dust mixtures. We will revise the abstract and the discussion of the scaling relations to add explicit qualification that these relations are specific to the TNG+SKIRT setup and that broader applicability would benefit from cross-validation on independent simulations or observations. This does not alter the utility of the relations as a physically motivated starting point within the context of the paper. revision: yes

Circularity Check

0 steps flagged

No circularity: empirical derivation self-contained within synthetic library

full rationale

The paper generates a library of synthetic attenuation curves from TNG50/TNG100+SKIRT, applies Information-Ordered Bottleneck analysis to determine that four parameters suffice for the variation present in that library, then uses symbolic regression on those same curves to obtain an explicit four-parameter functional form and scaling relations to galaxy properties. All steps operate directly on the input simulation outputs without re-using fitted quantities as independent predictions, without self-citations as load-bearing premises, and without redefining inputs in terms of outputs. The resulting model is an empirical compression of the provided data rather than a claim of external derivation; external validity to real galaxies is a separate assumption, not a circularity issue.

Axiom & Free-Parameter Ledger

4 free parameters · 2 axioms · 0 invented entities

The central claim rests on the assumption that the TNG50/TNG100 + SKIRT library with three fixed dust mixtures spans the relevant diversity; the IOB analysis and symbolic regression are treated as standard tools whose outputs directly give the minimal parameter count and optimal form.

free parameters (4)
  • UV bump strength
    One of the four free parameters of the derived model; its value varies per galaxy and is fitted or assigned via scaling relations.
  • FUV slope
    One of the four free parameters of the derived model.
  • UV-bump transition curvature
    One of the four free parameters of the derived model.
  • large-scale optical slope
    One of the four free parameters of the derived model.
axioms (2)
  • domain assumption Information-Ordered Bottleneck analysis correctly identifies the minimal number of parameters required to capture attenuation-curve diversity
    Invoked to conclude that exactly four parameters suffice.
  • domain assumption Symbolic regression recovers an optimal functional form given the target curves and the four-parameter constraint
    Used to derive the explicit model expression.

pith-pipeline@v0.9.1-grok · 5822 in / 1701 out tokens · 32904 ms · 2026-06-27T15:46:33.697571+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

241 extracted references · 213 canonical work pages · 59 internal anchors

  1. [1]

    SKIRT: an Advanced Dust Radiative Transfer Code with a User-Friendly Architecture

    SKIRT: An advanced dust radiative transfer code with a user-friendly architecture. Astronomy and Computing , keywords =. doi:10.1016/j.ascom.2014.10.004 , archivePrefix =. 1410.1629 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.ascom.2014.10.004 2014

  2. [2]

    Predictions for the spatial distribution of the dust continuum emission in 1<z<5 star-forming galaxies

    Predictions for the spatial distribution of the dust continuum emission in 1 < z < 5 star-forming galaxies. , keywords =. doi:10.1093/mnras/stz1736 , archivePrefix =. 1905.13234 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1736 1905

  3. [3]

    arXiv e-prints , keywords =

    CALIMA: On-the-fly dust and PAH evolution for radiation-hydrodynamics galaxy formation simulations. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.21790 , archivePrefix =. 2602.21790 , primaryClass =

    work page doi:10.48550/arxiv.2602.21790

  4. [4]

    , keywords =

    Evolution of galaxy attenuation curves driven by evolving dust mass and grain size distributions. , keywords =. doi:10.1051/0004-6361/202555658 , archivePrefix =. 2508.21157 , primaryClass =

    work page doi:10.1051/0004-6361/202555658

  5. [5]

    , keywords =

    The MOSDEF Survey: The Variation of the Dust Attenuation Curve with Metallicity. , keywords =. doi:10.3847/1538-4357/aba35e , archivePrefix =. 2005.01742 , primaryClass =

    work page doi:10.3847/1538-4357/aba35e 2005

  6. [6]

    , keywords =

    The ALMA REBELS Survey: dust continuum detections at z > 6.5. , keywords =. doi:10.1093/mnras/stac1779 , archivePrefix =. 2203.15136 , primaryClass =

    work page doi:10.1093/mnras/stac1779

  7. [7]

    , keywords =

    SIMBA-EOR: early galaxy formation in the SIMBA simulation including a new sub-grid interstellar medium model. , keywords =. doi:10.1093/mnras/stae2445 , archivePrefix =. 2402.06728 , primaryClass =

    work page doi:10.1093/mnras/stae2445

  8. [8]

    , keywords =

    On the simultaneous modelling of dust and stellar populations for interpretation of galaxy properties. , keywords =. doi:10.1093/mnras/stac1667 , archivePrefix =. 2206.06379 , primaryClass =

    work page doi:10.1093/mnras/stac1667

  9. [9]

    How to Measure Galaxy Star Formation Histories. II. Nonparametric Models. , keywords =. doi:10.3847/1538-4357/ab133c , archivePrefix =. 1811.03637 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab133c

  10. [10]

    , keywords =

    An Updated Dust-to-Star Geometry: Dust Attenuation Does Not Depend on Inclination in 1.3 z 2.6 Star-forming Galaxies from MOSDEF. , keywords =. doi:10.3847/1538-4357/accdd1 , archivePrefix =. 2304.08521 , primaryClass =

    work page doi:10.3847/1538-4357/accdd1

  11. [11]

    , keywords =

    Dust Attenuation Curves at z 0.8 from LEGA-C: Precise Constraints on the Slope and 2175 S Bump Strength. , keywords =. doi:10.3847/1538-4357/abba37 , archivePrefix =. 2010.01147 , primaryClass =

    work page doi:10.3847/1538-4357/abba37 2010

  12. [12]

    Shark: introducing an open source, free and flexible semi-analytic model of galaxy formation

    Shark: introducing an open source, free, and flexible semi-analytic model of galaxy formation. , keywords =. doi:10.1093/mnras/sty2440 , archivePrefix =. 1807.11180 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2440

  13. [13]

    , keywords =

    Modelling the evolution and influence of dust in cosmological simulations that include the cold phase of the interstellar medium. , keywords =. doi:10.1093/mnras/staf2040 , archivePrefix =. 2505.13056 , primaryClass =

    work page doi:10.1093/mnras/staf2040

  14. [14]

    Dust and Grain Size Evolution in Galaxy Simulations: What Matters and What Does Not

    Dust and Grain Size Evolution in Galaxy Simulations: What Matters and What Does Not. arXiv e-prints , keywords =. doi:10.48550/arXiv.2604.06314 , archivePrefix =. 2604.06314 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.06314

  15. [15]

    A first empirical derivation of the average dust attenuation law at 2<z<7

    A first empirical derivation of the average dust attenuation law at 2<z<7. arXiv e-prints , keywords =. doi:10.48550/arXiv.2604.09763 , archivePrefix =. 2604.09763 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.09763

  16. [16]

    Finkelstein and Anthony J

    Katherine Chworowsky and Steven L. Finkelstein and Anthony J. Taylor and Alexa M. Morales and Mark Dickinson and L. Y. Aaron Yung and Pablo Arrabal Haro and Bren E. Backhaus and Davide Bevacqua and Óscar Chávez Ortiz and Adam C. Carnall and Callum T. Donnan and Mauro Giavalisco and Michaela Hirschmann and Kartheik G. Iyer and Anton M. Koekemoer and Rebecc...

    Pith/arXiv arXiv

  17. [17]

    Characterizing Dust Attenuation in Local Star Forming Galaxies: UV and Optical Reddening

    Characterizing Dust Attenuation in Local Star-forming Galaxies: UV and Optical Reddening. , keywords =. doi:10.3847/0004-637X/818/1/13 , archivePrefix =. 1601.00208 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/818/1/13

  18. [18]

    , keywords =

    The dust-continuum size of TNG50 galaxies at z = 1-5: a comparison with the distribution of stellar light, stars, dust, and H _ 2. , keywords =. doi:10.1093/mnras/stab3312 , archivePrefix =. 2101.12218 , primaryClass =

    work page doi:10.1093/mnras/stab3312

  19. [19]

    IQ Collaboratory. III. The Empirical Dust Attenuation Framework-Taking Hydrodynamical Simulations with a Grain of Dust. , keywords =. doi:10.3847/1538-4357/ac4253 , archivePrefix =. 2106.09741 , primaryClass =

    work page doi:10.3847/1538-4357/ac4253

  20. [20]

    , keywords =

    Measuring the dust attenuation law of galaxies using photometric data. , keywords =. doi:10.1093/mnras/stae1373 , archivePrefix =. 2308.13974 , primaryClass =

    work page doi:10.1093/mnras/stae1373

  21. [21]

    , keywords =

    Strategies for Obtaining Robust Spectral Energy Distribution Fitting Parameters for Galaxies at z 1 and z 2 in the Absence of Infrared Data. , keywords =. doi:10.3847/1538-4357/ad17c8 , archivePrefix =. 2401.06865 , primaryClass =

    work page doi:10.3847/1538-4357/ad17c8

  22. [22]

    , keywords =

    Systematic biases in determining dust attenuation curves through galaxy SED fitting. , keywords =. doi:10.1093/mnras/stac132 , archivePrefix =. 2201.05467 , primaryClass =

    work page doi:10.1093/mnras/stac132

  23. [23]

    G.A.S.. II. Dust extinction in galaxies: Luminosity functions and infrared excess. , keywords =. doi:10.1051/0004-6361/201834674 , archivePrefix =. 1901.01747 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201834674 1901

  24. [24]

    Analysis of galaxy SEDs from far-UV to far-IR with CIGALE: Studying a SINGS test sample

    Analysis of galaxy spectral energy distributions from far-UV to far-IR with CIGALE: studying a SINGS test sample. , keywords =. doi:10.1051/0004-6361/200912497 , archivePrefix =. 0909.5439 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200912497

  25. [25]

    , keywords =

    Dust attenuation in galaxies at cosmic dawn from the FirstLight simulations. , keywords =. doi:10.1093/mnras/stad2602 , archivePrefix =. 2304.10150 , primaryClass =

    work page doi:10.1093/mnras/stad2602

  26. [26]

    , keywords =

    Measuring the Dust Attenuation Curves of SINGS/KINGFISH Galaxies Using Swift/UVOT Photometry. , keywords =. doi:10.3847/1538-4357/acd332 , archivePrefix =. 2305.05650 , primaryClass =

    work page doi:10.3847/1538-4357/acd332

  27. [27]

    Correlation of dust attenuation laws with star-to-dust compactness up to z = 4

    The slippery slope of dust attenuation curves. Correlation of dust attenuation laws with star-to-dust compactness up to z = 4. , keywords =. doi:10.1051/0004-6361/202245818 , archivePrefix =. 2304.13713 , primaryClass =

    work page doi:10.1051/0004-6361/202245818

  28. [28]

    F., Petit , P., et al

    Predicting dust extinction from the stellar mass of a galaxy. , keywords =. doi:10.1111/j.1365-2966.2010.17321.x , archivePrefix =. 1007.1145 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17321.x 2010

  29. [29]

    arXiv e-prints , keywords =

    A Dusty Dawn: Galactic Dust Buildup at zrsim5. arXiv e-prints , keywords =. doi:10.48550/arXiv.2408.08962 , archivePrefix =. 2408.08962 , primaryClass =

    work page doi:10.48550/arxiv.2408.08962

  30. [30]

    and Speagle, Joshua S

    Zucker, Catherine and Goodman, Alyssa and Alves, João and Bialy, Shmuel and Koch, Eric W. and Speagle, Joshua S. and Foley, Michael M. and Finkbeiner, Douglas and Leike, Reimar and Enßlin, Torsten and Peek, Joshua E. G. and Edenhofer, Gordian , title =. 2021 , month =. doi:10.3847/1538-4357/ac1f96 , url =

    work page doi:10.3847/1538-4357/ac1f96 2021

  31. [31]

    , keywords =

    A Dusty Locale: evolution of galactic dust populations from Milky Way to dwarf-mass galaxies. , keywords =. doi:10.1093/mnras/stae716 , archivePrefix =. 2401.04766 , primaryClass =

    work page doi:10.1093/mnras/stae716

  32. [32]

    , keywords =

    The galactic dust-up: modelling dust evolution in FIRE. , keywords =. doi:10.1093/mnras/stac1542 , archivePrefix =. 2201.12369 , primaryClass =

    work page doi:10.1093/mnras/stac1542

  33. [33]

    , keywords =

    Fade to grey: systematic variation of galaxy attenuation curves with galaxy properties in the EAGLE simulations. , keywords =. doi:10.1093/mnras/stz3234 , archivePrefix =. 1908.08956 , primaryClass =

    work page doi:10.1093/mnras/stz3234 1908

  34. [34]

    arXiv e-prints , keywords =

    Learning the Universe: Cosmological and Astrophysical Parameter Inference with Galaxy Luminosity Functions and Colours. arXiv e-prints , keywords =. doi:10.48550/arXiv.2411.13960 , archivePrefix =. 2411.13960 , primaryClass =

    work page doi:10.48550/arxiv.2411.13960

  35. [35]

    The Mass-Metallicity Relation with the Direct Method on Stacked Spectra of SDSS Galaxies

    The Mass-Metallicity Relation with the Direct Method on Stacked Spectra of SDSS Galaxies. , keywords =. doi:10.1088/0004-637X/765/2/140 , archivePrefix =. 1211.3418 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/765/2/140

  36. [36]

    The Origin of the Mass--Metallicity Relation: Insights from 53,000 Star-Forming Galaxies in the SDSS

    The Origin of the Mass-Metallicity Relation: Insights from 53,000 Star-forming Galaxies in the Sloan Digital Sky Survey. , keywords =. doi:10.1086/423264 , archivePrefix =. astro-ph/0405537 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/423264

  37. [37]

    Monthly Notices of the Royal Astronomical Society , volume =

    Meert, Alan and Vikram, Vinu and Bernardi, Mariangela , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2014 , month =. doi:10.1093/mnras/stu2333 , url =

    work page doi:10.1093/mnras/stu2333 2014

  38. [38]

    Salim, Samir and Tacchella, Sandro and Osborne, Chandler and Faber, S. M. and Lee, Janice C. and Ellison, Sara L. , title =. 2023 , month =. doi:10.3847/1538-4357/ad04db , url =

    work page doi:10.3847/1538-4357/ad04db 2023

  39. [39]

    and Janowiecki, Steven and Cunha, Elisabete da and Dickinson, Mark and Boquien, Médéric and Burgarella, Denis and Salzer, John J

    Salim, Samir and Lee, Janice C. and Janowiecki, Steven and Cunha, Elisabete da and Dickinson, Mark and Boquien, Médéric and Burgarella, Denis and Salzer, John J. and Charlot, Stéphane , title =. 2016 , month =. doi:10.3847/0067-0049/227/1/2 , url =

    work page doi:10.3847/0067-0049/227/1/2 2016

  40. [40]

    , keywords =

    Realistic mock observations of the sizes and stellar mass surface densities of massive galaxies in FIRE-2 zoom-in simulations. , keywords =. doi:10.1093/mnras/staa3765 , archivePrefix =. 2009.10161 , primaryClass =

    work page doi:10.1093/mnras/staa3765 2009

  41. [41]

    , keywords =

    Predicting sub-millimetre flux densities from global galaxy properties. , keywords =. doi:10.1093/mnras/stac3451 , archivePrefix =. 2211.11702 , primaryClass =

    work page doi:10.1093/mnras/stac3451

  42. [42]

    , keywords =

    Dust attenuation law in JWST galaxies at z 7-8. , keywords =. doi:10.1051/0004-6361/202346723 , archivePrefix =. 2304.11178 , primaryClass =

    work page doi:10.1051/0004-6361/202346723

  43. [43]

    The AURORA Survey: The Nebular Attenuation Curve of a Galaxy at z=4.41 from Ultraviolet to Near-Infrared Wavelengths

    The AURORA Survey: The Nebular Attenuation Curve of a Galaxy at z=4.41 from Ultraviolet to Near-Infrared Wavelengths. arXiv e-prints , keywords =. doi:10.48550/arXiv.2408.05273 , archivePrefix =. 2408.05273 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2408.05273

  44. [44]

    , keywords =

    The impact of AGN-driven winds on physical and observable galaxy sizes. , keywords =. doi:10.1093/mnras/stad1528 , archivePrefix =. 2303.12858 , primaryClass =

    work page doi:10.1093/mnras/stad1528

  45. [45]

    , keywords =

    Disappearing Galaxies: The Orientation Dependence of JWST-bright, HST-dark, Star-forming Galaxy Selection. , keywords =. doi:10.3847/1538-4357/ad02f8 , archivePrefix =. 2310.08829 , primaryClass =

    work page doi:10.3847/1538-4357/ad02f8

  46. [46]

    , keywords =

    Geometry effects on dust attenuation curves with different grain sources at high redshift. , keywords =. doi:10.1093/mnras/stab2242 , archivePrefix =. 2109.03072 , primaryClass =

    work page doi:10.1093/mnras/stab2242

  47. [47]

    A Theory for the Variation of Dust Attenuation Laws in Galaxies

    A Theory for the Variation of Dust Attenuation Laws in Galaxies. , keywords =. doi:10.3847/1538-4357/aaed25 , archivePrefix =. 1805.06905 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aaed25

  48. [48]

    Efficient 3D NLTE dust radiative transfer with SKIRT

    Efficient Three-dimensional NLTE Dust Radiative Transfer with SKIRT. , keywords =. doi:10.1088/0067-0049/196/2/22 , archivePrefix =. 1108.5056 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/196/2/22

  49. [49]

    arXiv e-prints , keywords =

    Dust attenuation evolution in z 2 - 12 JWST galaxies. arXiv e-prints , keywords =. doi:10.48550/arXiv.2402.05996 , archivePrefix =. 2402.05996 , primaryClass =

    work page doi:10.48550/arxiv.2402.05996

  50. [50]

    The stellar population synthesis models

    Stellar population synthesis at the resolution of 2003. , keywords =. doi:10.1046/j.1365-8711.2003.06897.x , archivePrefix =. astro-ph/0309134 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06897.x 2003

  51. [51]

    , keywords =

    A redshift-dependent IRX- dust attenuation relation for TNG50 galaxies. , keywords =. doi:10.1093/mnras/staa1900 , archivePrefix =. 2001.04992 , primaryClass =

    work page doi:10.1093/mnras/staa1900 2001

  52. [52]

    , title = "

    Dekel, Avishai and Krumholz, Mark R. , title = ". Monthly Notices of the Royal Astronomical Society , volume =. 2013 , month =. doi:10.1093/mnras/stt480 , url =

    work page doi:10.1093/mnras/stt480 2013

  53. [53]

    The formation and cosmic evolution of dust in the early Universe. I. Dust sources. arXiv e-prints , keywords =. doi:10.48550/arXiv.2310.00053 , archivePrefix =. 2310.00053 , primaryClass =

    work page doi:10.48550/arxiv.2310.00053

  54. [54]

    arXiv e-prints , keywords =

    The Diversity and Evolution of Dust Attenuation Curves from Redshift z -0.5ex 1 to 9. arXiv e-prints , keywords =. doi:10.48550/arXiv.2509.01795 , archivePrefix =. 2509.01795 , primaryClass =

    work page doi:10.48550/arxiv.2509.01795

  55. [55]

    arXiv e-prints , keywords =

    The Growth of Dust in Galaxies in the First Billion Years with Applications to Blue Monsters. arXiv e-prints , keywords =. doi:10.48550/arXiv.2509.18266 , archivePrefix =. 2509.18266 , primaryClass =

    work page doi:10.48550/arxiv.2509.18266

  56. [56]

    Michael , title =

    A Simple Model for the Absorption of Starlight by Dust in Galaxies. , keywords =. doi:10.1086/309250 , archivePrefix =. astro-ph/0003128 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/309250

  57. [57]

    and Leja, Joel and Johnson, Benjamin D

    Suess, Katherine A. and Leja, Joel and Johnson, Benjamin D. and Bezanson, Rachel and Greene, Jenny E. and Kriek, Mariska and Lower, Sidney and Narayanan, Desika and Setton, David J. and Spilker, Justin S. , year=. Recovering the Star Formation Histories of Recently Quenched Galaxies: The Impact of Model and Prior Choices , volume=. The Astrophysical Journ...

    work page doi:10.3847/1538-4357/ac82b0

  58. [58]

    2001, MNRAS, 327, 799, doi: 10.1046/j.1365-8711.2001.04769.x

    Todini, Paolo and Ferrara, Andrea , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2001 , month =. doi:10.1046/j.1365-8711.2001.04486.x , url =

    work page doi:10.1046/j.1365-8711.2001.04486.x 2001

  59. [59]

    , keywords =

    First Light And Reionisation Epoch Simulations (FLARES) - XII: The consequences of star-dust geometry on galaxies in the EoR. , keywords =. doi:10.1093/mnras/stad3594 , archivePrefix =. 2303.04177 , primaryClass =

    work page doi:10.1093/mnras/stad3594

  60. [60]

    G., Mobasher, B., et al

    Pacifici, Camilla and Iyer, Kartheik G. and Mobasher, Bahram and da Cunha, Elisabete and Acquaviva, Viviana and Burgarella, Denis and Calistro Rivera, Gabriela and Carnall, Adam C. and Chang, Yu-Yen and Chartab, Nima and Cooke, Kevin C. and Fairhurst, Ciaran and Kartaltepe, Jeyhan and Leja, Joel and Małek, Katarzyna and Salmon, Brett and Torelli, Marianna...

    work page doi:10.3847/1538-4357/acacff 2023

  61. [61]

    , keywords =

    Outshining by Recent Star Formation Prevents the Accurate Measurement of High-z Galaxy Stellar Masses. , keywords =. doi:10.3847/1538-4357/ad0966 , archivePrefix =. 2306.10118 , primaryClass =

    work page doi:10.3847/1538-4357/ad0966

  62. [62]

    , keywords =

    Galaxies with grains: unraveling dust evolution and extinction curves with hydrodynamical simulations. , keywords =. doi:10.1051/0004-6361/202449784 , archivePrefix =. 2402.18515 , primaryClass =

    work page doi:10.1051/0004-6361/202449784

  63. [63]

    , keywords =

    Modeling Galaxies in the Early Universe with Supernova Dust Attenuation. , keywords =. doi:10.3847/2041-8213/add15d , archivePrefix =. 2502.14031 , primaryClass =

    work page doi:10.3847/2041-8213/add15d 2041

  64. [64]

    arXiv e-prints , keywords =

    Big, Dusty Galaxies in Blue Jay: Insights into the Relationship Between Morphology and Dust Attenuation at Cosmic Noon. arXiv e-prints , keywords =. doi:10.48550/arXiv.2504.15346 , archivePrefix =. 2504.15346 , primaryClass =

    work page doi:10.48550/arxiv.2504.15346

  65. [65]

    arXiv e-prints , keywords =

    Blue Monsters and Dusty Descendants: Reconciling UV and IR Emission from Galaxies from z=7, up to z= 14. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.18556 , archivePrefix =. 2602.18556 , primaryClass =

    work page doi:10.48550/arxiv.2602.18556

  66. [66]

    The Dust Attenuation Law in Distant Galaxies: Evidence for Variation with Spectral Type

    The Dust Attenuation Law in Distant Galaxies: Evidence for Variation with Spectral Type. , keywords =. doi:10.1088/2041-8205/775/1/L16 , archivePrefix =. 1308.1099 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/775/1/l16 2041

  67. [67]

    Dust formation history of galaxies: a critical role of metallicity for the dust mass growth by accreting materials in the interstellar medium

    Dust formation history of galaxies: A critical role of metallicity* for the dust mass growth by accreting materials in the interstellar medium. Earth, Planets and Space , keywords =. doi:10.5047/eps.2012.04.014 , archivePrefix =. 1206.0817 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.5047/eps.2012.04.014 2012

  68. [68]

    Remodeling the evolution of grain size distribution in galaxies

    Remodelling the evolution of grain size distribution in galaxies. , keywords =. doi:10.1093/mnras/sty2838 , archivePrefix =. 1810.07962 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2838

  69. [69]

    Multiple Scattering in Clumpy Media. II. Galactic Environments. , keywords =. doi:10.1086/308197 , archivePrefix =. astro-ph/9907342 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/308197

  70. [70]

    , keywords =

    Detection of the 2175 A UV bump at z > 7: evidence for rapid dust evolution in a merging reionization-era galaxy. , keywords =. doi:10.1093/mnras/staf1228 , archivePrefix =. 2502.21119 , primaryClass =

    work page doi:10.1093/mnras/staf1228

  71. [71]

    arXiv e-prints , keywords =

    Cloudy-Maraston: Integrating nebular continuum and line emission with the Maraston stellar population synthesis models. arXiv e-prints , keywords =. doi:10.48550/arXiv.2501.03133 , archivePrefix =. 2501.03133 , primaryClass =

    work page doi:10.48550/arxiv.2501.03133

  72. [72]

    , keywords =

    Warm dust in high-z galaxies: origin and implications. , keywords =. doi:10.1093/mnras/staa1959 , archivePrefix =. 2004.09528 , primaryClass =

    work page doi:10.1093/mnras/staa1959 2004

  73. [73]

    , keywords =

    Dust in high-redshift galaxies: reconciling UV attenuation and IR emission. , keywords =. doi:10.1088/1475-7516/2024/09/018 , archivePrefix =. 2401.07893 , primaryClass =

    work page doi:10.1088/1475-7516/2024/09/018 2024

  74. [74]

    Radiative transfer with POLARIS. I. Analysis of magnetic fields through synthetic dust continuum polarization measurements. , keywords =. doi:10.1051/0004-6361/201424930 , archivePrefix =. 1604.05305 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201424930

  75. [75]

    and Tollerud, Erik J

    Astropy: A community Python package for astronomy. , archiveprefix = "arXiv", eprint =. doi:10.1051/0004-6361/201322068 , adsurl =

    work page doi:10.1051/0004-6361/201322068

  76. [76]

    and Bradshaw, R

    Behnel, S. and Bradshaw, R. and Citro, C. and Dalcin, L. and Seljebotn, D.S. and Smith, K. , journal =. Cython: The Best of Both Worlds , year =. doi:10.1109/MCSE.2010.118 , issn =

    work page doi:10.1109/mcse.2010.118 2010

  77. [77]

    Perez and B

    F. Perez and B. E. Granger , journal =. IPython: A System for Interactive Scientific Computing , year =. doi:10.1109/MCSE.2007.53 , issn =

    work page doi:10.1109/mcse.2007.53 2007

  78. [78]

    Positioning and Power in Academic Publishing: Players, Agents and Agendas , editor =

    Jupyter Notebooks, a publishing format for reproducible computational workflows , author =. Positioning and Power in Academic Publishing: Players, Agents and Agendas , editor =. 2016 , pages =

    2016

  79. [79]

    J. D. Hunter , journal =. Matplotlib: A 2D Graphics Environment , year =. doi:10.1109/MCSE.2007.55 , issn =

    work page doi:10.1109/mcse.2007.55 2007

  80. [80]

    van der Walt and S

    S. van der Walt and S. C. Colbert and G. Varoquaux , journal =. The NumPy Array: A Structure for Efficient Numerical Computation , year =. doi:10.1109/MCSE.2011.37 , issn =

    work page doi:10.1109/mcse.2011.37 2011

Showing first 80 references.