pith. sign in

arxiv: 2411.14532 · v2 · submitted 2024-11-21 · 🌌 astro-ph.GA · astro-ph.CO

Hitting the slopes: A spectroscopic view of UV continuum slopes of galaxies reveals a reddening at z > 9.5

Aayush Saxena , Alex J. Cameron , Harley Katz , Andrew J. Bunker , Jacopo Chevallard , Francesco D'Eugenio , Santiago Arribas , Rachana Bhatawdekar
show 21 more authors
Kristan Boyett Phillip A. Cargile Stefano Carniani Stephane Charlot Mirko Curti Emma Curtis-Lake Kevin Hainline Zhiyuan Ji Benjamin D. Johnson Gareth C. Jones Nimisha Kumari Isaac Laseter Michael V. Maseda Brant Robertson Charlotte Simmonds Sandro Tacchella Hannah Ubler Christina C. Williams Chris Willott Joris Witstok Yongda Zhu
This is my paper

Pith reviewed 2026-05-23 17:05 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords UV continuum slopehigh-redshift galaxiesJWST spectroscopynebular continuumdust attenuationgalaxy evolutionLyman continuum leakage
0
0 comments X

The pith

The average UV continuum slope of galaxies begins to redden at redshifts above 9.5, which high-temperature nebular emission can reproduce without dust.

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

The paper measures the UV continuum slope β from JWST spectra of 295 galaxies spanning 5.5 to 14.3 in redshift. It reports that β grows mildly bluer toward higher redshift and fainter magnitudes up to z approximately 9.5, after which the average value turns redder. Stacked spectra tie the bluer slopes mainly to low dust content rather than metallicity or age. Modeling shows that nebular continuum from gas above 15,000 K can match the observed range of slopes at the highest redshifts even in the absence of dust, pointing to hotter conditions in the earliest galaxies.

Core claim

The central claim is that the average β at z > 9.5 begins to redden, breaking the trend of increasing blueness seen at lower redshifts. Stacked spectra link bluer β directly to reduced dust attenuation, while six individual galaxies with β < -3.0 display spectroscopic signs of Lyman-continuum leakage. In the absence of dust, nebular continuum emission from gas at temperatures above 15,000 K reproduces the full range of observed β values; higher temperatures driven by massive stars can simultaneously account for the bright UV luminosities recorded at z > 10.

What carries the argument

The UV continuum slope β, measured directly from NIRSpec/PRISM spectra and tracked across redshift and magnitude bins; nebular continuum emission at gas temperatures above 15,000 K is the mechanism proposed to generate redder β without requiring dust.

If this is right

  • Rapid dust production or a large nebular-continuum contribution must operate by z > 9.5 to explain the observed slopes.
  • Very blue galaxies are expected to leak a significant fraction of their ionizing photons.
  • Hotter gas temperatures from massive stars would simultaneously boost nebular emission and help produce the bright UV luminosities seen at z > 10.

Where Pith is reading between the lines

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

  • If high gas temperatures are common, models of early star formation may need to include a larger fraction of very massive stars than assumed at lower redshifts.
  • The same nebular contribution that reddens β could alter inferred star-formation rates and ionizing-photon budgets used in reionization calculations.
  • Future deeper spectra of individual z > 10 galaxies can test whether the stacked reddening trend persists or is an artifact of sample selection.

Load-bearing premise

The reddening trend at z > 9.5 and the nebular explanation both rest on the premise that the highest-redshift bin contains enough galaxies and that stacking plus fitting introduce no systematic bias that could fake a reddening signal.

What would settle it

Individual β measurements for a larger sample of galaxies at z > 10 that show continued bluing instead of reddening, or spectroscopic line ratios indicating gas temperatures below 15,000 K in the same objects.

Figures

Figures reproduced from arXiv: 2411.14532 by Aayush Saxena, Alex J. Cameron, Andrew J. Bunker, Benjamin D. Johnson, Brant Robertson, Charlotte Simmonds, Christina C. Williams, Chris Willott, Emma Curtis-Lake, Francesco D'Eugenio, Gareth C. Jones, Hannah Ubler, Harley Katz, Isaac Laseter, Jacopo Chevallard, Joris Witstok, Kevin Hainline, Kristan Boyett, Michael V. Maseda, Mirko Curti, Nimisha Kumari, Phillip A. Cargile, Rachana Bhatawdekar, Sandro Tacchella, Santiago Arribas, Stefano Carniani, Stephane Charlot, Yongda Zhu, Zhiyuan Ji.

Figure 1
Figure 1. Figure 1: Left. Overview of the spectroscopic sample considered in this study, which includes some of the highest redshift spectroscopically confirmed sources currently known. The continuum SNR > 2 requirement to measure the UV slopes ensures that the UV magnitudes are robustly measured for all galaxies in our sample. Right. Histogram of the UV slope 𝛽 of star-forming galaxies in this sample, with a median 𝛽 = −2.30… view at source ↗
Figure 2
Figure 2. Figure 2: Binning of the sample in 𝛽 and redshift space, chosen to produce stacked spectra and study the sample averaged evolution of 𝛽 with redshift and other spectroscopic properties. The redshift bins were chosen to ensure coverage of key strong emission lines (as mentioned in the main text), whereas the 𝛽 bins were simply chosen to split the sample into three equally numbered tertiles. We do not split our 𝑧 > 9.… view at source ↗
Figure 3
Figure 3. Figure 3: Left. 𝛽 versus redshift, where the stars show the median and error bars show 1𝜎 standard deviation in redshift bins. 𝛽 becomes bluer between redshifts 𝑧 ∼ 5.5 − 8 but note that the 𝛽 values do not evolve much at 𝑧 ≳ 8. The median and standard deviation of 𝛽 measured in these redshift bins are given in the text. Middle. Violin plots showing the median and standard deviation for the distribution of 𝛽 in the … view at source ↗
Figure 4
Figure 4. Figure 4: Dependence of 𝛽 on the galaxy UV magnitude in different redshift bins. The error bars represent the standard deviation in the bins. At redshifts 5.5 < 𝑧 < 6 and 6 < 𝑧 < 7 we do see a clear correlation between 𝛽 and UV magnitudes. However, there does not appear to be any dependence of 𝛽 on UV magnitude at 𝑧 > 7. This may be indicative of a lack of significant dust attenuation and its appreciable impact on t… view at source ↗
Figure 5
Figure 5. Figure 5: Clockwise from top left: Dependence of galaxy properties such as dust attenuation or E(B-V) (top-left), gas-phase metallicity given by 12+log(O/H) (top-right), O32 ratio (bottom-right) and the Hβ equivalent width (bottom-left) on the 𝛽 measured from stacked spectra in bins of redshift and 𝛽. The redshift bins are represented by different symbols and are used consistently across all panels. We find that dus… view at source ↗
Figure 6
Figure 6. Figure 6: 1D and 2D spectra for the galaxies in our sample that show 𝛽 ≤ −3.0, selected from different tiers of JADES observations. Three out of these six galaxies show extremely bright Lyα emission, which may be indicative of significant LyC escape as well (e.g. Verhamme et al. 2015). GS-210003 at 𝑧 = 5.779 shows a very interesting spectrum, with clear detections of the Si iv+O iv] and He ii+O iii] complexes. The S… view at source ↗
Figure 7
Figure 7. Figure 7: Synthetic spectra generated using pythonFSPS with both stellar and nebular emission (green) and stellar only emission (violet, shaded) for a simple stellar population with log(𝑍/𝑍⊙ ) = −1.5, log(𝑈) = −2.0 and age (time since burst) = 5 Myr. The vertical dashed lines demarcate the wavelength range over which 𝛽 is measured. It is clear that the inclusion of the nebular continuum reddens the measured UV slope… view at source ↗
Figure 8
Figure 8. Figure 8: Left. 𝛽 measured from synthetic spectra generated using FSPS with a Chabrier IMF as a function of age for a single burst of star formation with log(𝑈) = −2.0. Solid lines show measurements from spectra containing both stellar and nebular emission, and dashed line containing only stellar emission. The color bar represents metallicities in units of log(𝑍★/𝑍⊙ ). The dotted line is the median observed 𝛽 for 𝑧 … view at source ↗
Figure 9
Figure 9. Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p016_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Same as [PITH_FULL_IMAGE:figures/full_fig_p016_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Dependence of 𝛽 with gas temperature for a purely nebular domi￾nated rest-frame UV spectrum over the wavelength range where 𝛽 is typically measured, for a range of electron densities. We find that to reproduce the ob￾served distribution of 𝛽 values seen at 𝑧 > 9.5 from our sample in the typically observed density range 𝑛𝑒 = 100 − 1000 cm−3 , a purely nebular dominated UV continuum from gas at temperatures… view at source ↗
read the original abstract

The UV continuum slope of galaxies, $\beta$, is a powerful diagnostic. Understanding the redshift evolution of $\beta$ and its dependence on key galaxy properties can shed light on the evolution of galaxy physical properties over cosmic time. In this study, we present $\beta$ measurements for 295 spectroscopically confirmed galaxies at $5.5<z<14.3$ selected primarily from JADES, where $\beta$ has been measured from high quality JWST NIRSpec/PRISM spectra. We find a median $\beta=-2.3$ across our full sample, and find mild increase in blueness of $\beta$ with increasing redshift and fainter UV magnitudes. Interestingly, we find evidence for the average $\beta$ at $z > 9.5$ to begin to redden, deviating from the trend observed at $z < 9.5$. By producing stacked spectra in bins of redshift and $\beta$, we derive trends between $\beta$ and dust attenuation, metallicity, ionization parameter, and stellar age indicators directly from spectra, finding a lack of dust attenuation to be the dominant driver of bluer $\beta$ values. We further report six galaxies with $\beta<-3.0$, which show a range of spectroscopic properties and signs of significant LyC photon leakage. Finally, we show that the redder $\beta$ values at $z > 9.5$ may require rapid build-up of dust reservoirs in the very early Universe or a significant contribution from the nebular continuum emission to the observed UV spectra, with the nebular continuum fraction depending on the gas temperatures and densities. Our modeling shows that in the absence of dust, nebular emission at $T > 15,000$ K can reproduce the range of $\beta$ that we see in our sample. Higher gas temperatures driven by hot, massive stars can boost the fraction of nebular continuum emission, potentially explaining the observed $\beta$ values as well as bright UV magnitudes seen across galaxies at $z > 10$.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 2 minor

Summary. The manuscript measures UV continuum slopes β directly from JWST NIRSpec/PRISM spectra for 295 spectroscopically confirmed galaxies at 5.5 < z < 14.3 (primarily JADES). It reports a sample median β = −2.3, a mild trend toward bluer β with increasing redshift and fainter M_UV up to z ≈ 9.5, but evidence that the average β reddens at z > 9.5. Stacked spectra link β trends to dust attenuation, metallicity, ionization parameter and stellar age; six objects with β < −3.0 are highlighted. Nebular-continuum modeling at T > 15 000 K is shown to reproduce the observed high-z β range in the absence of dust.

Significance. Direct spectroscopic β measurements at z > 9 provide a valuable anchor for early-galaxy studies. If the z > 9.5 reddening and its nebular explanation are robust, the work constrains the timing of dust production and the contribution of hot gas to UV light, with implications for reionization and galaxy-formation models. The stacking analysis that ties β to physical parameters from the same spectra is a clear strength.

major comments (3)
  1. [§4] §4 (redshift-binned trends): the claim that average β reddens at z > 9.5 rests on the highest-redshift bin; the exact number of galaxies per bin must be stated and the stability of the median β against Poisson noise or single-object removal must be quantified (e.g., via bootstrap resampling).
  2. [§3] §3 (PRISM β fitting): the continuum-fitting procedure used to extract β from rest-frame ~1200–3000 Å PRISM spectra at z > 10 has reduced wavelength leverage and potentially increased line contamination; explicit tests (mock spectra or alternative fitting windows) are required to rule out redshift-dependent systematic bias that could mimic the reported reddening.
  3. [§5] §5 (nebular modeling): the demonstration that T > 15 000 K nebular continuum reproduces the observed β range assumes this temperature without independent constraints from the spectra; the manuscript should test whether plausible variations in density or ionization parameter alone can produce comparable β shifts.
minor comments (2)
  1. [Figure 4] Figure 4 (stacked spectra): the wavelength ranges and bin labels should be annotated directly on the panels for clarity.
  2. [Abstract] Abstract: the statement of a “mild increase in blueness” should be accompanied by the measured dβ/dz or equivalent quantitative slope.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed review, which has helped us identify areas to strengthen the robustness of our analysis. We address each major comment below and will incorporate the suggested additions and tests in the revised manuscript.

read point-by-point responses

  1. Referee: [§4] §4 (redshift-binned trends): the claim that average β reddens at z > 9.5 rests on the highest-redshift bin; the exact number of galaxies per bin must be stated and the stability of the median β against Poisson noise or single-object removal must be quantified (e.g., via bootstrap resampling).

    Authors: We agree that explicitly stating the number of galaxies per redshift bin and quantifying the stability of the median β is essential for supporting the reddening claim at z > 9.5. In the revised manuscript, we will add the exact counts for each bin in §4 and include bootstrap resampling results to assess sensitivity to Poisson noise and individual object removal. These additions will confirm that the trend is robust and not an artifact of small-number statistics. revision: yes

  2. Referee: [§3] §3 (PRISM β fitting): the continuum-fitting procedure used to extract β from rest-frame ~1200–3000 Å PRISM spectra at z > 10 has reduced wavelength leverage and potentially increased line contamination; explicit tests (mock spectra or alternative fitting windows) are required to rule out redshift-dependent systematic bias that could mimic the reported reddening.

    Authors: We acknowledge that the reduced wavelength coverage at z > 10 could introduce potential biases from limited leverage or line contamination. To rule this out, the revised §3 will include explicit tests using mock spectra (with realistic line contamination and redshift-dependent coverage) and alternative fitting windows. These tests will demonstrate that any systematic redshift-dependent bias is negligible and does not drive the observed reddening trend. revision: yes

  3. Referee: [§5] §5 (nebular modeling): the demonstration that T > 15 000 K nebular continuum reproduces the observed β range assumes this temperature without independent constraints from the spectra; the manuscript should test whether plausible variations in density or ionization parameter alone can produce comparable β shifts.

    Authors: The referee is correct that our current modeling emphasizes temperature as the key parameter. While high temperatures are physically motivated by hot stellar populations at these redshifts, we will expand §5 to test independent variations in gas density and ionization parameter. This will clarify whether these factors alone can produce comparable β shifts or if temperature remains the primary driver, providing a fuller assessment of nebular contributions. revision: yes

Circularity Check

0 steps flagged

No circularity: β measured directly from spectra; nebular modeling is explanatory check, not fitted prediction

full rationale

The paper measures β directly from JWST NIRSpec/PRISM spectra of 295 galaxies (abstract and methods). Trends with redshift, dust, metallicity etc. are extracted from stacked spectra. The statement that nebular continuum at T>15,000 K can reproduce observed β values is presented as a forward model check, not a parameter fit to the same β data that then 'predicts' the input. No self-citation chains, uniqueness theorems, or ansatzes imported from prior author work are invoked as load-bearing. The derivation chain is self-contained against external spectral data.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The work rests on standard spectral extraction and fitting assumptions from JWST data reduction pipelines plus domain assumptions about nebular emission models; no new free parameters or invented entities are introduced.

axioms (1)
  • domain assumption Standard assumptions in NIRSpec/PRISM spectral calibration and continuum fitting hold for these high-redshift sources.
    Invoked when deriving beta and stacked properties directly from spectra.

pith-pipeline@v0.9.0 · 6056 in / 1419 out tokens · 47003 ms · 2026-05-23T17:05:44.998025+00:00 · methodology

discussion (0)

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

Forward citations

Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Resolving dust and Ly{\alpha} emission in a lensed galaxy at the epoch of reionization with JWST/CANUCS

    astro-ph.GA 2025-12 conditional novelty 7.0

    Spatially resolved JWST observations of lensed LAE HCM 6A at z=6.57 reveal Lyα escaping from a dust-cleared central clump in the youngest region, with age-dependent Calzetti-like attenuation curves.

  2. Lyman-alpha Radiation Pressure in Dense Star Clusters: Implications for Star Formation and Winds at Cosmic Dawn

    astro-ph.GA 2026-05 conditional novelty 6.0

    Lyα radiation pressure mildly reduces gas-to-star conversion efficiency in dense high-redshift clusters while dominating the launch of rapid outflows.

  3. SPURS: Bursty Star Formation in an Extremely Luminous Weak Emission Line Galaxy at $z=9.3$

    astro-ph.GA 2026-04 unverdicted novelty 6.0

    A massive galaxy at z=9.3 shows bursty star formation with a recent downturn and sits in a small ionized bubble in a neutral IGM.

  4. JWST Advanced Deep Extragalactic Survey (JADES) Data Release 5: Photometrically Selected Galaxy Candidates at z > 8

    astro-ph.GA 2026-01 unverdicted novelty 5.0

    JADES DR5 delivers 2081 z_phot > 8 galaxy candidates with UV slope trends, morphological evidence of clumpy growth, and improved photo-z methods tested on a spectroscopic subsample.

Reference graph

Works this paper leans on

136 extracted references · 136 canonical work pages · cited by 4 Pith papers · 10 internal anchors

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

    work page

  2. [2]

    J., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2a7b , https://ui.adsabs.harvard.edu/abs/2024ApJ...965..169A 965, 169

    Adams N. J., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2a7b , https://ui.adsabs.harvard.edu/abs/2024ApJ...965..169A 965, 169

    work page doi:10.3847/1538-4357/ad2a7b 2024

  3. [3]

    Arrabal Haro P., et al., 2023, @doi [ ] 10.3847/2041-8213/acdd54 , https://ui.adsabs.harvard.edu/abs/2023ApJ...951L..22A 951, L22

    work page doi:10.3847/2041-8213/acdd54 2023

  4. [4]

    Astropy Collaboration et al., 2013, @doi [ ] 10.1051/0004-6361/201322068 , http://adsabs.harvard.edu/abs/2013A

    work page doi:10.1051/0004-6361/201322068 2013

  5. [5]

    Astropy Collaboration et al., 2018, @doi [ ] 10.3847/1538-3881/aabc4f , https://ui.adsabs.harvard.edu/abs/2018AJ....156..123A 156, 123

    work page doi:10.3847/1538-3881/aabc4f 2018

  6. [6]

    arXiv:2404.10751

    Austin D., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2404.10751 , https://ui.adsabs.harvard.edu/abs/2024arXiv240410751A p. arXiv:2404.10751

    work page doi:10.48550/arxiv.2404.10751 2024

  7. [7]

    R., Meyer M

    Bastian N., Covey K. R., Meyer M. R., 2010, @doi [ ] 10.1146/annurev-astro-082708-101642 , https://ui.adsabs.harvard.edu/abs/2010ARA&A..48..339B 48, 339

    work page doi:10.1146/annurev-astro-082708-101642 2010

  8. [8]

    Baumgardt H., H \'e nault-Brunet V., Dickson N., Sollima A., 2023, @doi [ ] 10.1093/mnras/stad631 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.3991B 521, 3991

    work page doi:10.1093/mnras/stad631 2023

  9. [9]

    J., 2021, @doi [ ] 10.3847/1538-4357/abdd3f , https://ui.adsabs.harvard.edu/abs/2021ApJ...909..144B 909, 144

    Bhatawdekar R., Conselice C. J., 2021, @doi [ ] 10.3847/1538-4357/abdd3f , https://ui.adsabs.harvard.edu/abs/2021ApJ...909..144B 909, 144

    work page doi:10.3847/1538-4357/abdd3f 2021

  10. [10]

    Bolamperti A., et al., 2023, @doi [ ] 10.1093/mnras/stad3114 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526.5263B 526, 5263

    work page doi:10.1093/mnras/stad3114 2023

  11. [11]

    J., et al., 2009, @doi [ ] 10.1088/0004-637X/705/1/936 , https://ui.adsabs.harvard.edu/abs/2009ApJ...705..936B 705, 936

    Bouwens R. J., et al., 2009, @doi [ ] 10.1088/0004-637X/705/1/936 , https://ui.adsabs.harvard.edu/abs/2009ApJ...705..936B 705, 936

    work page doi:10.1088/0004-637x/705/1/936 2009

  12. [12]

    J., et al., 2010, @doi [ ] 10.1088/2041-8205/708/2/L69 , https://ui.adsabs.harvard.edu/abs/2010ApJ...708L..69B 708, L69

    Bouwens R. J., et al., 2010, @doi [ ] 10.1088/2041-8205/708/2/L69 , https://ui.adsabs.harvard.edu/abs/2010ApJ...708L..69B 708, L69

    work page doi:10.1088/2041-8205/708/2/l69 2010

  13. [13]

    J., et al., 2014, @doi [ ] 10.1088/0004-637X/793/2/115 , https://ui.adsabs.harvard.edu/abs/2014ApJ...793..115B 793, 115

    Bouwens R. J., et al., 2014, @doi [ ] 10.1088/0004-637X/793/2/115 , https://ui.adsabs.harvard.edu/abs/2014ApJ...793..115B 793, 115

    work page doi:10.1088/0004-637x/793/2/115 2014

  14. [14]

    Bouwens R., Illingworth G., Oesch P., Stefanon M., Naidu R., van Leeuwen I., Magee D., 2023a, @doi [ ] 10.1093/mnras/stad1014 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.1009B 523, 1009

    work page doi:10.1093/mnras/stad1014

  15. [15]

    J., et al., 2023b, @doi [ ] 10.1093/mnras/stad1145 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.1036B 523, 1036

    Bouwens R. J., et al., 2023b, @doi [ ] 10.1093/mnras/stad1145 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.1036B 523, 1036

    work page doi:10.1093/mnras/stad1145

  16. [16]

    J., NIRSPEC Instrument Science Team JAESs Collaboration 2020, in da Cunha E., Hodge J., Afonso J., Pentericci L., Sobral D., eds, Vol

    Bunker A. J., NIRSPEC Instrument Science Team JAESs Collaboration 2020, in da Cunha E., Hodge J., Afonso J., Pentericci L., Sobral D., eds, Vol. 352, Uncovering Early Galaxy Evolution in the ALMA and JWST Era. pp 342--346 ( @eprint arXiv 2112.15207 ), @doi 10.1017/S1743921319009463

    work page doi:10.1017/s1743921319009463 2020

  17. [17]

    J., et al., 2023a, @doi [arXiv e-prints] 10.48550/arXiv.2306.02467 , https://ui.adsabs.harvard.edu/abs/2023arXiv230602467B p

    Bunker A. J., et al., 2023a, @doi [arXiv e-prints] 10.48550/arXiv.2306.02467 , https://ui.adsabs.harvard.edu/abs/2023arXiv230602467B p. arXiv:2306.02467

    work page doi:10.48550/arxiv.2306.02467

  18. [18]

    J., et al., 2023b, @doi [ ] 10.1051/0004-6361/202346159 , https://ui.adsabs.harvard.edu/abs/2023A&A...677A..88B 677, A88

    Bunker A. J., et al., 2023b, @doi [ ] 10.1051/0004-6361/202346159 , https://ui.adsabs.harvard.edu/abs/2023A&A...677A..88B 677, A88

    work page doi:10.1051/0004-6361/202346159

  19. [19]

    J., Conroy, C., & Johnson, B

    Byler N., Dalcanton J. J., Conroy C., Johnson B. D., 2017, @doi [ ] 10.3847/1538-4357/aa6c66 , https://ui.adsabs.harvard.edu/abs/2017ApJ...840...44B 840, 44

    work page doi:10.3847/1538-4357/aa6c66 2017

  20. [20]

    Calabr \`o A., et al., 2021, @doi [ ] 10.1051/0004-6361/202039244 , https://ui.adsabs.harvard.edu/abs/2021A&A...646A..39C 646, A39

    work page doi:10.1051/0004-6361/202039244 2021

  21. [21]

    L., & Storchi-Bergmann, T

    Calzetti D., Kinney A. L., Storchi-Bergmann T., 1994, @doi [ ] 10.1086/174346 , https://ui.adsabs.harvard.edu/abs/1994ApJ...429..582C 429, 582

    work page doi:10.1086/174346 1994

  22. [22]

    J., Katz H., Witten C., Saxena A., Laporte N., Bunker A

    Cameron A. J., Katz H., Witten C., Saxena A., Laporte N., Bunker A. J., 2023a, @doi [arXiv e-prints] 10.48550/arXiv.2311.02051 , https://ui.adsabs.harvard.edu/abs/2023arXiv231102051C p. arXiv:2311.02051

    work page doi:10.48550/arxiv.2311.02051

  23. [24]

    J., Katz H., Rey M

    Cameron A. J., Katz H., Rey M. P., 2023c, @doi [ ] 10.1093/mnrasl/slad046 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522L..89C 522, L89

    work page doi:10.1093/mnrasl/slad046

  24. [25]

    C., et al., 2018, @doi [ ] 10.1093/mnras/sty2169 , 480, 4379

    Carnall A. C., McLure R. J., Dunlop J. S., Dav \'e R., 2018, @doi [ ] 10.1093/mnras/sty2169 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.480.4379C 480, 4379

    work page internal anchor Pith review doi:10.1093/mnras/sty2169 2018

  25. [26]

    Eisenstein, Peter Jakob- sen, Joris Witstok, Benjamin D

    Carniani S., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2405.18485 , https://ui.adsabs.harvard.edu/abs/2024arXiv240518485C p. arXiv:2405.18485

    work page doi:10.48550/arxiv.2405.18485 2024

  26. [27]

    arXiv:2403.10238

    Castellano M., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2403.10238 , https://ui.adsabs.harvard.edu/abs/2024arXiv240310238C p. arXiv:2403.10238

    work page doi:10.48550/arxiv.2403.10238 2024

  27. [28]

    Chabrier G., 2003, @doi [ ] 10.1086/376392 , https://ui.adsabs.harvard.edu/abs/2003PASP..115..763C 115, 763

    work page internal anchor Pith review doi:10.1086/376392 2003

  28. [29]

    Chemerynska I., et al., 2024, @doi [ ] 10.1093/mnras/stae1260 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.531.2615C 531, 2615

    work page doi:10.1093/mnras/stae1260 2024

  29. [30]

    Chisholm J., et al., 2022, @doi [ ] 10.1093/mnras/stac2874 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.517.5104C 517, 5104

    work page doi:10.1093/mnras/stac2874 2022

  30. [31]

    D., 2016, @doi [ ] 10.3847/0004-637X/823/2/102 , https://ui.adsabs.harvard.edu/abs/2016ApJ...823..102C 823, 102

    Choi J., Dotter A., Conroy C., Cantiello M., Paxton B., Johnson B. D., 2016, @doi [ ] 10.3847/0004-637X/823/2/102 , https://ui.adsabs.harvard.edu/abs/2016ApJ...823..102C 823, 102

    work page internal anchor Pith review doi:10.3847/0004-637x/823/2/102 2016

  31. [32]

    Choustikov N., et al., 2024, @doi [ ] 10.1093/mnras/stae776 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.529.3751C 529, 3751

    work page doi:10.1093/mnras/stae776 2024

  32. [33]

    E., 2010, @doi [ ] 10.1088/0004-637X/712/2/833 , https://ui.adsabs.harvard.edu/abs/2010ApJ...712..833C 712, 833

    Conroy C., Gunn J. E., 2010, @doi [ ] 10.1088/0004-637X/712/2/833 , https://ui.adsabs.harvard.edu/abs/2010ApJ...712..833C 712, 833

    work page internal anchor Pith review doi:10.1088/0004-637x/712/2/833 2010

  33. [34]

    E., & White , M

    Conroy C., Gunn J. E., White M., 2009, @doi [ ] 10.1088/0004-637X/699/1/486 , https://ui.adsabs.harvard.edu/abs/2009ApJ...699..486C 699, 486

    work page internal anchor Pith review doi:10.1088/0004-637x/699/1/486 2009

  34. [35]

    Cullen F., et al., 2021, @doi [ ] 10.1093/mnras/stab1340 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.505..903C 505, 903

    work page doi:10.1093/mnras/stab1340 2021

  35. [36]

    Cullen F., et al., 2023a, @doi [ ] 10.1093/mnras/stad073 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.tmp...87C

    work page doi:10.1093/mnras/stad073

  36. [37]

    arXiv:2311.06209

    Cullen F., et al., 2023b, @doi [arXiv e-prints] 10.48550/arXiv.2311.06209 , https://ui.adsabs.harvard.edu/abs/2023arXiv231106209C p. arXiv:2311.06209

    work page doi:10.48550/arxiv.2311.06209

  37. [38]

    Curti M., Mannucci F., Cresci G., Maiolino R., 2020, @doi [ ] 10.1093/mnras/stz2910 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.491..944C 491, 944

    work page doi:10.1093/mnras/stz2910 2020

  38. [39]

    Curti M., et al., 2023, @doi [ ] 10.1093/mnras/stac2737 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518..425C 518, 425

    work page doi:10.1093/mnras/stac2737 2023

  39. [40]

    Curtis-Lake E., et al., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-01918-w , https://ui.adsabs.harvard.edu/abs/2023NatAs...7..622C 7, 622

    work page doi:10.1038/s41550-023-01918-w 2023

  40. [41]

    arXiv:2311.09908

    D'Eugenio F., et al., 2023, @doi [arXiv e-prints] 10.48550/arXiv.2311.09908 , https://ui.adsabs.harvard.edu/abs/2023arXiv231109908D p. arXiv:2311.09908

    work page doi:10.48550/arxiv.2311.09908 2023

  41. [42]

    arXiv:2404.06531

    D'Eugenio F., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2404.06531 , https://ui.adsabs.harvard.edu/abs/2024arXiv240406531D p. arXiv:2404.06531

    work page doi:10.48550/arxiv.2404.06531 2024

  42. [43]

    Dabringhausen J., Kroupa P., Baumgardt H., 2009, @doi [ ] 10.1111/j.1365-2966.2009.14425.x , https://ui.adsabs.harvard.edu/abs/2009MNRAS.394.1529D 394, 1529

    work page doi:10.1111/j.1365-2966.2009.14425.x 2009

  43. [44]

    C., Birnboim Y., Mandelker N., Li Z., 2023, @doi [ ] 10.1093/mnras/stad1557 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.3201D 523, 3201

    Dekel A., Sarkar K. C., Birnboim Y., Mandelker N., Li Z., 2023, @doi [ ] 10.1093/mnras/stad1557 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.523.3201D 523, 3201

    work page doi:10.1093/mnras/stad1557 2023

  44. [45]

    T., McLure, R

    Donnan C. T., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2403.03171 , https://ui.adsabs.harvard.edu/abs/2024arXiv240303171D p. arXiv:2403.03171

    work page doi:10.48550/arxiv.2403.03171 2024

  45. [46]

    Dotter A., 2016, @doi [ ] 10.3847/0067-0049/222/1/8 , https://ui.adsabs.harvard.edu/abs/2016ApJS..222....8D 222, 8

    work page internal anchor Pith review doi:10.3847/0067-0049/222/1/8 2016

  46. [47]

    Ionizing feedback from massive stars in massive clusters: fake bubbles and untriggered star formation

    Dunlop J. S., McLure R. J., Robertson B. E., Ellis R. S., Stark D. P., Cirasuolo M., de Ravel L., 2012, @doi [ ] 10.1111/j.1365-2966.2011.20102.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.420..901D 420, 901

    work page doi:10.1111/j.1365-2966.2011.20102.x 2012

  47. [48]

    Overview of the JWST Advanced Deep Extragalactic Survey (JADES)

    Eisenstein D. J., et al., 2023a, @doi [arXiv e-prints] 10.48550/arXiv.2306.02465 , https://ui.adsabs.harvard.edu/abs/2023arXiv230602465E p. arXiv:2306.02465

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2306.02465

  48. [49]

    J., et al., 2023b, @doi [arXiv e-prints] 10.48550/arXiv.2310.12340 , https://ui.adsabs.harvard.edu/abs/2023arXiv231012340E p

    Eisenstein D. J., et al., 2023b, @doi [arXiv e-prints] 10.48550/arXiv.2310.12340 , https://ui.adsabs.harvard.edu/abs/2023arXiv231012340E p. arXiv:2310.12340

    work page doi:10.48550/arxiv.2310.12340

  49. [50]

    J., Stanway , E

    Eldridge J. J., Stanway E. R., Xiao L., McClelland L. A. S., Taylor G., Ng M., Greis S. M. L., Bray J. C., 2017, @doi [ ] 10.1017/pasa.2017.51 , https://ui.adsabs.harvard.edu/abs/2017PASA...34...58E 34, e058

    work page internal anchor Pith review doi:10.1017/pasa.2017.51 2017

  50. [51]

    P., Whitler, L., et al

    Endsley R., Stark D. P., Whitler L., Topping M. W., Chen Z., Plat A., Chisholm J., Charlot S., 2023, @doi [ ] 10.1093/mnras/stad1919 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.2312E 524, 2312

    work page doi:10.1093/mnras/stad1919 2023

  51. [52]

    J., Gorgas J., Peletier R

    Falc \'o n-Barroso J., S \'a nchez-Bl \'a zquez P., Vazdekis A., Ricciardelli E., Cardiel N., Cenarro A. J., Gorgas J., Peletier R. F., 2011, @doi [ ] 10.1051/0004-6361/201116842 , https://ui.adsabs.harvard.edu/abs/2011A&A...532A..95F 532, A95

    work page doi:10.1051/0004-6361/201116842 2011

  52. [53]

    Faucher-Gigu \`e re C.-A., 2018, @doi [ ] 10.1093/mnras/stx2595 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.473.3717F 473, 3717

    work page doi:10.1093/mnras/stx2595 2018

  53. [54]

    arXiv:2405.20370

    Ferrara A., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2405.20370 , https://ui.adsabs.harvard.edu/abs/2024arXiv240520370F p. arXiv:2405.20370

    work page doi:10.48550/arxiv.2405.20370 2024

  54. [55]

    Ferruit P., et al., 2022, @doi [ ] 10.1051/0004-6361/202142673 , https://ui.adsabs.harvard.edu/abs/2022A&A...661A..81F 661, A81

    work page doi:10.1051/0004-6361/202142673 2022

  55. [56]

    L., Papovich C., Giavalisco M., Reddy N

    Finkelstein S. L., Papovich C., Giavalisco M., Reddy N. A., Ferguson H. C., Koekemoer A. M., Dickinson M., 2010, @doi [ ] 10.1088/0004-637X/719/2/1250 , https://ui.adsabs.harvard.edu/abs/2010ApJ...719.1250F 719, 1250

    work page doi:10.1088/0004-637x/719/2/1250 2010

  56. [57]

    L., et al., 2012, @doi [ ] 10.1088/0004-637X/756/2/164 , https://ui.adsabs.harvard.edu/abs/2012ApJ...756..164F 756, 164

    Finkelstein S. L., et al., 2012, @doi [ ] 10.1088/0004-637X/756/2/164 , https://ui.adsabs.harvard.edu/abs/2012ApJ...756..164F 756, 164

    work page doi:10.1088/0004-637x/756/2/164 2012

  57. [58]

    L., Bagley , M

    Finkelstein S. L., et al., 2022, @doi [ ] 10.3847/2041-8213/ac966e , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L..55F 940, L55

    work page doi:10.3847/2041-8213/ac966e 2022

  58. [59]

    Fosbury R. A. E., et al., 2003, @doi [ ] 10.1086/378228 , https://ui.adsabs.harvard.edu/abs/2003ApJ...596..797F 596, 797

    work page doi:10.1086/378228 2003

  59. [60]

    Fukushima H., Yajima H., 2023, @doi [ ] 10.1093/mnras/stad1956 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.524.1422F 524, 1422

    work page doi:10.1093/mnras/stad1956 2023

  60. [61]

    R., Mirocha J., 2022, @doi [ ] 10.1093/mnras/stac310 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.511.3895F 511, 3895

    Furlanetto S. R., Mirocha J., 2022, @doi [ ] 10.1093/mnras/stac310 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.511.3895F 511, 3895

    work page doi:10.1093/mnras/stac310 2022

  61. [62]

    J., Shuntov M., Atek H., Zitrin A., Richard J., Lehnert M

    Furtak L. J., Shuntov M., Atek H., Zitrin A., Richard J., Lehnert M. D., Chevallard J., 2023, @doi [ ] 10.1093/mnras/stac3717 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.519.3064F 519, 3064

    work page doi:10.1093/mnras/stac3717 2023

  62. [63]

    C., 2011, @doi [ ] 10.1007/s00159-011-0043-7 , https://ui.adsabs.harvard.edu/abs/2011A&ARv..19...43G 19, 43

    Gall C., Hjorth J., Andersen A. C., 2011, @doi [ ] 10.1007/s00159-011-0043-7 , https://ui.adsabs.harvard.edu/abs/2011A&ARv..19...43G 19, 43

    work page doi:10.1007/s00159-011-0043-7 2011

  63. [64]

    2007, , 374, 1413, 10.1111/j.1365-2966.2006.11246.x

    H \"a gele G. F., P \'e rez-Montero E., D \' az \'A . I., Terlevich E., Terlevich R., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10856.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.372..293H 372, 293

    work page doi:10.1111/j.1365-2966.2006.10856.x 2006

  64. [65]

    N., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2404.04325 , https://ui.adsabs.harvard.edu/abs/2024arXiv240404325H p

    Hainline K. N., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2404.04325 , https://ui.adsabs.harvard.edu/abs/2024arXiv240404325H p. arXiv:2404.04325

    work page doi:10.48550/arxiv.2404.04325 2024

  65. [66]

    J., Saldana-Lopez A., Citro A., James B

    Hayes M. J., Saldana-Lopez A., Citro A., James B. L., Mingozzi M., Scarlata C., Martinez Z., Berg D. A., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2411.09262 , https://ui.adsabs.harvard.edu/abs/2024arXiv241109262H p. arXiv:2411.09262

    work page doi:10.48550/arxiv.2411.09262 2024

  66. [67]

    E., Brammer, G

    Heintz K. E., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2404.02211 , https://ui.adsabs.harvard.edu/abs/2024arXiv240402211H p. arXiv:2404.02211

    work page doi:10.48550/arxiv.2404.02211 2024

  67. [68]

    D., 2007, Computing In Science & Engineering, 9, 90

    Hunter J. D., 2007, Computing In Science & Engineering, 9, 90

    work page 2007

  68. [69]

    K., Li W., Ho L

    Inayoshi K., Harikane Y., Inoue A. K., Li W., Ho L. C., 2022, @doi [ ] 10.3847/2041-8213/ac9310 , https://ui.adsabs.harvard.edu/abs/2022ApJ...938L..10I 938, L10

    work page doi:10.3847/2041-8213/ac9310 2022

  69. [70]

    Isobe Y., Ouchi M., Nakajima K., Harikane Y., Ono Y., Xu Y., Zhang Y., Umeda H., 2023, @doi [ ] 10.3847/1538-4357/acf376 , https://ui.adsabs.harvard.edu/abs/2023ApJ...956..139I 956, 139

    work page doi:10.3847/1538-4357/acf376 2023

  70. [71]

    Jakobsen P., et al., 2022, @doi [ ] 10.1051/0004-6361/202142663 , https://ui.adsabs.harvard.edu/abs/2022A&A...661A..80J 661, A80

    work page internal anchor Pith review doi:10.1051/0004-6361/202142663 2022

  71. [72]

    E., Oey M

    Jaskot A. E., Oey M. S., 2013, @doi [ ] 10.1088/0004-637X/766/2/91 , https://ui.adsabs.harvard.edu/abs/2013ApJ...766...91J 766, 91

    work page doi:10.1088/0004-637x/766/2/91 2013

  72. [73]

    E., et al., 2024, @doi [ ] 10.3847/1538-4357/ad5557 , https://ui.adsabs.harvard.edu/abs/2024ApJ...973..111J 973, 111

    Jaskot A. E., et al., 2024, @doi [ ] 10.3847/1538-4357/ad5557 , https://ui.adsabs.harvard.edu/abs/2024ApJ...973..111J 973, 111

    work page doi:10.3847/1538-4357/ad5557 2024

  73. [74]

    J., Sutherland R

    Jin Y., Kewley L. J., Sutherland R. S., 2022, @doi [ ] 10.3847/2041-8213/ac80f3 , https://ui.adsabs.harvard.edu/abs/2022ApJ...934L...8J 934, L8

    work page doi:10.3847/2041-8213/ac80f3 2022

  74. [75]

    Johnson B., et al., 2024, dfm/python-fsps: v0.4.7, @doi 10.5281/zenodo.12447779 , https://doi.org/10.5281/zenodo.12447779

    work page doi:10.5281/zenodo.12447779 2024

  75. [76]

    arXiv:2211.04626

    Katz H., et al., 2022, @doi [arXiv e-prints] 10.48550/arXiv.2211.04626 , https://ui.adsabs.harvard.edu/abs/2022arXiv221104626K p. arXiv:2211.04626

    work page doi:10.48550/arxiv.2211.04626 2022

  76. [77]

    Katz H., et al., 2023, @doi [ ] 10.1093/mnras/stac2657 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518..592K 518, 592

    work page doi:10.1093/mnras/stac2657 2023

  77. [78]

    arXiv:2408.03189

    Katz H., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2408.03189 , https://ui.adsabs.harvard.edu/abs/2024arXiv240803189K p. arXiv:2408.03189

    work page doi:10.48550/arxiv.2408.03189 2024

  78. [79]

    S., Glover S

    Klessen R. S., Glover S. C. O., 2023, @doi [ ] 10.1146/annurev-astro-071221-053453 , https://ui.adsabs.harvard.edu/abs/2023ARA&A..61...65K 61, 65

    work page doi:10.1146/annurev-astro-071221-053453 2023

  79. [80]

    H., Maseda, M

    Laseter I. H., et al., 2024, @doi [ ] 10.1051/0004-6361/202347133 , https://ui.adsabs.harvard.edu/abs/2024A&A...681A..70L 681, A70

    work page doi:10.1051/0004-6361/202347133 2024

  80. [81]

    Lecroq M., et al., 2024, @doi [ ] 10.1093/mnras/stad3838 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.9480L 527, 9480

    work page doi:10.1093/mnras/stad3838 2024

Showing first 80 references.