pith. sign in

arxiv: 2605.14922 · v1 · pith:P2KKRPZCnew · submitted 2026-05-14 · 🌌 astro-ph.GA

DREAMS. JWST Spectroscopy of a z=8.3 Galaxy with an ALMA Dust Continuum Detection: Early Dust, Very High T_(rm dust), and a Multi-wavelength [OIII] Ratio Discrepancy

Kana Takechi , Masami Ouchi , Kimihiko Nakajima , Tomokazu Kiyota , Yoichi Tamura , Yuichi Harikane , Yurina Nakazato , Tom J. L. C. Bakx
show 5 more authors
Akio K. Inoue Hidenobu Yajima Masato Hagimoto Yoshiaki Ono Yi Xu
This is my paper

Pith reviewed 2026-06-30 20:12 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords high-redshift galaxiesJWST spectroscopyALMA dust continuumAGN activitydust mass and temperature[OIII] emission linesmetallicityearly dust formation
0
0 comments X

The pith

MACS0416-Y1 at z=8.3 shows broad-line AGN, low dust-to-gas ratio of -3.6, dust temperature of 91 K, and [OIII]88um to [OIII]5007 ratio of 0.26 exceeding nebular models.

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

The paper presents JWST/NIRSpec spectroscopy of MACS0416-Y1, a z=8.312 galaxy with the highest-redshift ALMA dust detection, combined with archival data to measure its gas, dust, and line properties. It identifies a broad H beta line of width 1100 km/s as evidence for AGN activity, a metallicity of 0.15 solar, unusually low dust mass relative to gas and metals, and a high dust temperature. The central result is the elevated total [OIII]88um/[OIII]5007 flux ratio of 0.26, which lies above predictions from single-zone ionized nebular models at any density. This leads the authors to conclude that the infrared and optical [OIII] lines arise from largely distinct regions, with the optical line suppressed in dusty zones, requiring revised approaches to combining JWST and ALMA line data for early galaxies.

Core claim

MACS0416-Y1 shows a broad H beta line of width ~1100 km s^{-1} interpreted as a broad-line AGN, metallicity 12+log(O/H)=7.86^{+0.09}_{-0.08} (0.15 Zsun), log(Mdust/Mgas)=-3.60^{+0.29}_{-0.22}, Tdust ≃ 91^{+62}_{-35} K, and total [OIII]88μm/[OIII]5007 = 0.26 ± 0.06, above single ionized nebular model predictions at any density, suggesting the lines trace largely distinct regions with the optical line suppressed in dusty nebulae.

What carries the argument

The [OIII]88μm/[OIII]5007 flux ratio together with dust continuum and [CII]158μm emission used to derive dust mass, temperature, and gas mass, plus the broad H beta profile for AGN classification.

If this is right

  • At metallicity near the 0.1-0.2 Zsun critical value, dust growth is expected and accounts for the observed low dust-to-gas and dust-to-metal ratios plus the small total dust mass of ~10^6 solar masses.
  • Intense UV radiation from the AGN can heat dust to ~91 K, boosting the continuum emission enough for ALMA detection despite the low dust mass.
  • The [OIII] line ratio discrepancy implies that optical and infrared lines must be treated as sampling different physical zones when used together in JWST+ALMA analyses of high-redshift galaxies.
  • The system is caught in an early phase of dust buildup, consistent with its redshift and metallicity.

Where Pith is reading between the lines

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

  • If the high dust temperature is AGN-driven, similar temperature boosts may appear in other z>8 AGN hosts and affect dust mass estimates from continuum detections.
  • Multi-phase or multi-region nebular models will be needed to reconcile optical and far-infrared line ratios in dusty high-redshift systems.
  • The critical metallicity threshold for dust growth can be tested by measuring dust ratios in additional z~8 galaxies with comparable metallicities.

Load-bearing premise

The broad H beta line is produced by AGN activity consistent across the galaxy's clumps and the high [OIII] ratio results from the two lines tracing separate regions rather than a breakdown in the nebular models.

What would settle it

Spatially resolved maps of the [OIII]88um and [OIII]5007 emission that show whether the two lines arise from the same or clearly offset spatial regions within the galaxy.

Figures

Figures reproduced from arXiv: 2605.14922 by Akio K. Inoue, Hidenobu Yajima, Kana Takechi, Kimihiko Nakajima, Masami Ouchi, Masato Hagimoto, Tom J. L. C. Bakx, Tomokazu Kiyota, Yi Xu, Yoichi Tamura, Yoshiaki Ono, Yuichi Harikane, Yurina Nakazato.

Figure 1
Figure 1. Figure 1: JWST/NIRSpec F150W image (rest-frame UV continuum) of Y1 in grayscale with 850µm continuum con￾tours at 2σ, 3σ, 4σ, 5σ, 6σ, and 7σ levels overlaid in yellow. The rest-frame UV peaks, E, C, and W, are labeled in white, while the dust continuum peaks, D1 and D2, are marked in yellow. The red boxes indicate the slit footprint, with each segment corresponding to an individual spaxel [PITH_FULL_IMAGE:figures/f… view at source ↗
Figure 3
Figure 3. Figure 3: Color map of [Oiii] 5007 moment-0 map, overlaid with the green contours of NIRCam F150W image at 2σ, 5σ, 8σ, 11σ, 14σ, and 17σ levels, and the red (blue) box denotes the MSA slit integration region (IFU aperture) used for spectral extraction. The IFU aperture size is determined from a growth-curve analysis. 0 10 3.00 3.25 3.50 3.75 4.00 4.25 4.50 4.75 5.00 Wavelength [µm] 0.0 0.5 1.0 1.5 f¸ [1 0 ¡ 1 9 e r … view at source ↗
Figure 4
Figure 4. Figure 4: Top: JWST/NIRSpec MSA two-dimensional spectrum of Y1. Bottom: Extracted one-dimensional spec￾trum integrated over the spaxels shown by the red box in Fig￾ure 1. Emission lines are marked with dashed vertical lines. Flux density is shown in units of 10−19 erg s−1 cm−2 ˚A −1 as a function of observed wavelength. The red box in [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: JWST/NIRSpec IFU one-dimensional spectrum integrated over the blue box in [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Emission-line profile fitting of (a)Hβ and (b)[Oiii] 5007, extracted from the spaxel marked by red box in [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: JWST/NIRCam F150W image of Y1 overlaid with ALMA 850 µm continuum contours at 2σ, 3σ, 4σ, 5σ, 6σ, and 7σ levels in yellow. The rest-frame UV peaks, E, C, and W, are labeled in white. The dust continuum peaks, D1 and D2, are marked in yellow. The red box indicates the position of the spaxel with broad Hβ emission. The lower panel of [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Mass–Excitation (MEx) diagram showing log10([Oiii]5007/Hβ) versus stellar mass. The dashed curve marks the empirical division between star-form￾ing galaxies (MEx-SF) and AGN-dominated systems (MEx-AGN) (Juneau et al. 2011). The measured values for clumps E (red), C (blue), and W (green) are shown with uncertainties. Stellar masses are taken from Harshan et al. (2024). ture are normalized to the IFU-integra… view at source ↗
Figure 8
Figure 8. Figure 8: Top: Color criterion used to identify the char￾acteristic V-shaped spectral energy distributions (SEDs) of LRDs in the F277W − F444W versus F115W − F200W plane. The green shaded region indicates the selection win￾dow for V-shaped spectral sources, while the blue region marks the locations of cool dwarfs. Bottom: Color criterion used to identify red sources in the F277W − F444W versus F277W − F356W plane. T… view at source ↗
Figure 10
Figure 10. Figure 10: Spectra and best-fit profiles of Hγ and [Oiii] 4363. The IFU-integrated spectrum, MSA spectrum, and the IFU spectrum integrated over the MSA aperture are shown in thick black, green, and blue, respectively. The MSA spectrum and the IFU spectrum integrated over the MSA aperture are normalized to the IFU-integrated spectrum at the peak of Hγ. The red curve shows the best-fit model to the IFU-integrated spec… view at source ↗
Figure 11
Figure 11. Figure 11: Metallicity 12 + log(O/H) derived from R3 using the Hirschmann et al. (2023) relation. Spaxels with S/N< 5 are masked. The contours correspond to the NIR￾Cam F150W image at 2σ, 5σ, 8σ, 11σ, 14σ, and 17σ levels. The gray circle indicates the PSF at the observed wavelength of [Oiii] 5007. Because the PSF FWHMs at the observed wavelengths of [Oiii] 5007 and Hβ differ by only ∼ 0. ′′01, no PSF matching is app… view at source ↗
Figure 12
Figure 12. Figure 12: Left: Example spaxel-wise Gaussian fits to the [Oii] 3726,3729 doublet for a 3 × 3 grid. Center: Integrated [Oii] spectrum constructed by summing only spaxels with S/N > 5. Solid red curves show the best-fit Gaussian profile to the [Oii] doublet, and blue dashed curves show the individual components. Right: Spatial distribution of electron density on a logarithmic scale. Spaxels with S/N < 5 are masked. T… view at source ↗
Figure 13
Figure 13. Figure 13: Left: Ratio of [Oiii] 88µm to [Oiii] 5007 as a function of electron density (n [OIII] e ). The black curve shows the theoretical relation assuming an electron temperature of Te = 17300 ± 1500 K, corresponding to the value measured for Y1, and the gray shaded region represents the uncertainty. The red horizontal line and shaded region indicate the observed ratio and its uncertainty for Y1. The vertical das… view at source ↗
Figure 15
Figure 15. Figure 15: Dust mass as a function of gas-phase metallicity. The red diamond marks Y1. The gray shaded region indi￾cates the critical metallicity range (0.1–0.2 Z⊙). The blue squares and green pentagons represent the REBELS (z ∼7; Algera et al. 2025) and ALESS (z ∼1–6; da Cunha et al. 2015) samples, respectively. The black contours and points show the distribution of galaxies at 4 < z < 11 from CEERS (Burgarella et … view at source ↗
Figure 16
Figure 16. Figure 16: Left: Dust-to-gas ratio, log(Mdust/Mgas), as a function of gas-phase metallicity, 12 + log(O/H). The blue squares, light blue pentagons, green heptagons, and black points show REBELS galaxies (z ∼7; Algera et al. 2025), Quintet YD1 and YD4YD6 (z ∼ 7.9; Umehata et al. 2025), submillimeter galaxies (SMGs) (z ∼2; Shapley et al. 2020) and local galaxies (De Vis et al. 2019; Casasola et al. 2020), respectively… view at source ↗
Figure 17
Figure 17. Figure 17: Velocity-offset profiles of [Oii] 3726 (blue) and [Oiii] 5007 (red) relative to [Oiii] 88µm (black; reference frame). Solid curves show Gaussian fits to each profile. Verti￾cal dashed lines mark the center velocity of each component. common in high-z ISM environments (Choustikov et al. 2026). One possible explanation is that the [Oiii] 88µm and optical emission lines originate from physically and kine￾mat… view at source ↗
Figure 18
Figure 18. Figure 18: Schematic illustration of the spatial origin of the emission lines and the effects of dust attenuation. The system consists of a dust-rich inner region and a dust-poor outer region. The innermost compact high-density region, associated with an AGN, is dust-obscured and contributes little to the observed [Oiii] 88µm emission because of its high electron density. Surrounding this component is a lower-den￾si… view at source ↗
read the original abstract

We present a deep DREAMS JWST/NIRSpec MSA medium-grating spectrum of MACS0416-Y1, a galaxy at $z=8.312$ with the highest-redshift ALMA dust continuum detection to date, in order to characterize its properties together with archival IFU and ALMA data. The deep NIRSpec spectrum reveals a broad H$\beta$ line with a width of $\sim1100$ km s$^{-1}$. We interpret it as a broad-line AGN whose line diagnostics are consistent with AGN activity across its clumpy structure, given the absence of little red dot signatures. MACS0416-Y1 clearly shows [OIII]4363 emission, suggesting a moderately low metallicity of $12+\log(\mathrm{O/H})=7.86^{+0.09}_{-0.08}$ ($0.15~Z_\odot$). The combination of [CII]158$\mu$m and dust continuum emission indicates low dust mass ratios of $\log (M_{\rm dust}/M_{\rm gas})=-3.60^{+0.29}_{-0.22}$ and $\log (M_{\rm dust}/M_{\rm metal})=-0.95^{+0.29}_{-0.20}$. Because the metallicity of MACS0416-Y1 is around the critical metallicity of $0.1\textrm{-}0.2~Z_\odot$, the system is expected to undergo dust growth, explaining these low dust mass ratios as well as its small dust mass, $M_{\rm dust}\sim10^6~M_\odot$. The intense UV radiation from the AGN may contribute to a high dust temperature of $T_{\rm dust}\simeq 91^{+62}_{-35}$ K, boosting the dust-continuum emission above the ALMA detection limit despite the small $M_{\rm dust}$ at $z>8$. We find a very high total flux ratio of [OIII]88$\mu$m/[OIII]5007 = $0.26 \pm 0.06$ in MACS0416-Y1, above predictions from single ionized nebular models at any electron density. This discrepancy suggests that the [OIII]88$\mu$m and [OIII]5007 trace largely distinct regions, with the optical line suppressed in dusty nebulae, and thus requires careful interpretation when combining optical and infrared emission lines in JWST+ALMA studies.

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 manuscript reports deep JWST/NIRSpec MSA medium-grating spectroscopy of the z=8.312 galaxy MACS0416-Y1 (highest-redshift ALMA dust detection), combined with archival IFU and ALMA data. It identifies a broad Heta line (~1100 km s^{-1}) as a broad-line AGN with diagnostics consistent across the clumpy structure, derives metallicity 12+log(O/H)=7.86^{+0.09}_{-0.08} (0.15 Z_⊙) from [OIII]4363, reports low dust-to-gas and dust-to-metal ratios (log(M_dust/M_gas)=-3.60^{+0.29}_{-0.22}), small M_dust~10^6 M_⊙ near critical metallicity, high T_dust ≃ 91^{+62}_{-35} K possibly boosted by AGN UV, and a high total [OIII]88μm/[OIII]5007 ratio of 0.26±0.06 exceeding single ionized nebular model predictions at any density, implying the lines trace largely distinct regions with optical suppression in dusty gas.

Significance. If the results hold, the work supplies one of the earliest multi-wavelength characterizations of a dust-detected source at z>8, with direct line detections and continuum measurements (including uncertainties) that constrain dust growth, AGN presence, and high-z line-ratio diagnostics. These observational anchors are useful for future modeling even if some interpretations require refinement.

major comments (2)
  1. [Abstract] Abstract: the headline claim that [OIII]88μm/[OIII]5007 = 0.26 ± 0.06 lies above single ionized nebular model predictions at any electron density (implying distinct regions with optical-line suppression) rests on comparison to standard stellar-photoionization HII-region grids. The manuscript simultaneously classifies the source as a broad-line AGN; harder AGN continua can elevate the far-IR to optical [OIII] ratio via higher T_e or altered level populations, so the paper must explicitly test whether AGN photoionization models can reach the observed ratio before the distinct-region conclusion is load-bearing.
  2. [Abstract] Abstract: the interpretation that the broad Heta component arises from AGN activity that is consistent across the clumpy, lensed morphology (and therefore that AGN models are appropriate for the line-ratio analysis) is stated but not quantitatively demonstrated against possible differential magnification or spatially varying ionization; this underpins both the AGN classification and the subsequent use of non-stellar ionizing spectra.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive feedback. We agree that both major comments identify areas where the manuscript can be strengthened with additional analysis, and we will revise accordingly.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the headline claim that [OIII]88μm/[OIII]5007 = 0.26 ± 0.06 lies above single ionized nebular model predictions at any electron density (implying distinct regions with optical-line suppression) rests on comparison to standard stellar-photoionization HII-region grids. The manuscript simultaneously classifies the source as a broad-line AGN; harder AGN continua can elevate the far-IR to optical [OIII] ratio via higher T_e or altered level populations, so the paper must explicitly test whether AGN photoionization models can reach the observed ratio before the distinct-region conclusion is load-bearing.

    Authors: We agree this is a valid point. The current analysis compares to stellar HII-region grids, but given the broad-line AGN classification, we will add explicit tests using AGN photoionization models (e.g., CLOUDY grids with appropriate SEDs) to check whether the observed [OIII]88μm/[OIII]5007 ratio of 0.26 can be reproduced. The revised manuscript will report these results and adjust the interpretation of distinct regions if needed. This addresses the concern directly. revision: yes

  2. Referee: [Abstract] Abstract: the interpretation that the broad Hβ component arises from AGN activity that is consistent across the clumpy, lensed morphology (and therefore that AGN models are appropriate for the line-ratio analysis) is stated but not quantitatively demonstrated against possible differential magnification or spatially varying ionization; this underpins both the AGN classification and the subsequent use of non-stellar ionizing spectra.

    Authors: We acknowledge that while the manuscript notes consistency of line diagnostics across the clumpy structure (and absence of little red dot signatures), a more quantitative demonstration against differential magnification or ionization variations would strengthen the case. In revision, we will incorporate additional analysis using the archival IFU data to compare line ratios spatially and discuss lensing models to assess magnification effects. This will support the AGN classification and use of non-stellar spectra. revision: yes

Circularity Check

0 steps flagged

No significant circularity; direct measurements compared to external models

full rationale

The paper reports observed line fluxes, widths (~1100 km s^{-1} for broad Hβ), [OIII]4363-based metallicity (12+log(O/H)=7.86), dust-to-gas ratio from [CII]+continuum, T_dust, and the [OIII]88μm/[OIII]5007=0.26±0.06 ratio. These are computed from spectra and compared to standard external nebular grids (single-zone, stellar photoionization) without any fitted parameters renamed as predictions, self-definitional loops, or load-bearing self-citations. The derivation chain is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

Analysis rests on standard nebular emission models and dust continuum assumptions; fitted quantities such as metallicity and dust temperature are derived from the data rather than serving as free inputs to the central claims.

free parameters (2)
  • Metallicity from [OIII]4363
    Fitted value 7.86 with asymmetric errors derived from the observed line strength.
  • Dust temperature
    Fitted value ~91 K with large uncertainties from continuum and line data.
axioms (1)
  • domain assumption Single-zone ionized nebular models accurately predict [OIII] line ratios at all densities
    Invoked when stating the observed ratio exceeds model predictions at any electron density.

pith-pipeline@v0.9.1-grok · 6089 in / 1612 out tokens · 36747 ms · 2026-06-30T20:12:41.321403+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 1 Pith paper

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

  1. Lyman-alpha Pressure Strongly Enhances Pre-Supernova Feedback at Cosmic Dawn: The First Multi-Dimensional Lyman-alpha Radiation Hydrodynamics Simulations

    astro-ph.GA 2026-06 conditional novelty 8.0

    First 2D Lyα RHD simulations show Lyman-alpha radiation pressure yields radiative forces of 2-16 times L_bol/c and force multipliers of 10-60, dominating other pre-supernova feedback in metal-poor environments.

Reference graph

Works this paper leans on

106 extracted references · 101 canonical work pages · cited by 1 Pith paper · 6 internal anchors

  1. [1]

    doi:10.1109/TAC.1974.1100705

    Akaike, H.\ 1974, IEEE Transactions on Automatic Control, 19, 716. doi:10.1109/TAC.1974.1100705

    work page doi:10.1109/tac.1974.1100705 1974

  2. [2]

    doi:10.48550/arXiv.2509.16071

    Algera, H., Rowland, L., Smit, R., et al.\ 2025, arXiv:2509.16071. doi:10.48550/arXiv.2509.16071

    work page doi:10.48550/arxiv.2509.16071 2025

  3. [3]

    S., Takeuchi, T

    Asano, R. S., Takeuchi, T. T., Hirashita, H., et al.\ 2013, Earth, Planets and Space, 65, 3, 213. doi:10.5047/eps.2012.04.014

    work page doi:10.5047/eps.2012.04.014 2013

  4. [4]

    , keywords =

    Asplund, M., Grevesse, N., Sauval, A. J., et al.\ 2009, , 47, 1, 481. doi:10.1146/annurev.astro.46.060407.145222

    work page doi:10.1146/annurev.astro.46.060407.145222 2009

  5. [5]

    Bakx, T. J. L. C., Tamura, Y., Hashimoto, T., et al.\ 2020, , 493, 3, 4294. doi:10.1093/mnras/staa509

    work page doi:10.1093/mnras/staa509 2020

  6. [6]

    Bakx, T. J. L. C., Sommovigo, L., Tamura, Y., et al.\ 2025, , 544, 2, 1502. doi:10.1093/mnras/staf1714

    work page doi:10.1093/mnras/staf1714 2025

  7. [7]

    , archivePrefix = "arXiv", eprint =

    B \'e thermin, M., Daddi, E., Magdis, G., et al.\ 2015, , 573, A113. doi:10.1051/0004-6361/201425031

    work page doi:10.1051/0004-6361/201425031 2015

  8. [8]

    A., Gillman, S., Melinder, J., et al.\ 2024, , 969, 1, 27

    Boogaard, L. A., Gillman, S., Melinder, J., et al.\ 2024, , 969, 1, 27. doi:10.3847/1538-4357/ad43e5

    work page doi:10.3847/1538-4357/ad43e5 2024

  9. [9]

    , keywords =

    Bouwens, R. J., Smit, R., Schouws, S., et al.\ 2022, , 931, 2, 160. doi:10.3847/1538-4357/ac5a4a

    work page doi:10.3847/1538-4357/ac5a4a 2022

  10. [10]

    doi:10.1051/0004-6361/202554231

    Burgarella, D., Buat, V., Theul \'e , P., et al.\ 2025, , 699, A336. doi:10.1051/0004-6361/202554231

    work page doi:10.1051/0004-6361/202554231 2025

  11. [11]

    P., & Anderson, D

    Burnham, K. P., & Anderson, D. R.\ 2004, Sociological Methods & Research, 33, 2, 261

    2004

  12. [12]

    The Dust Content and Opacity of Actively Star-Forming Galaxies

    Calzetti, D., Armus, L., Bohlin, R. C., et al.\ 2000, , 533, 2, 682. doi:10.1086/308692

    work page internal anchor Pith review doi:10.1086/308692 2000

  13. [13]

    doi:10.1093/mnras/223.4.811

    Campbell, A., Terlevich, R., & Melnick, J.\ 1986, , 223, 811. doi:10.1093/mnras/223.4.811

    work page doi:10.1093/mnras/223.4.811 1986

  14. [14]

    CASA, the Common Astronomy Software Applications for Radio Astronomy

    CASA Team, Bean, B., Bhatnagar, S., et al.\ 2022, , 134, 1041, 114501. doi:10.1088/1538-3873/ac9642

    work page internal anchor Pith review doi:10.1088/1538-3873/ac9642 2022

  15. [15]

    doi:10.1051/0004-6361/201936665

    Casasola, V., Bianchi, S., De Vis, P., et al.\ 2020, , 633, A100. doi:10.1051/0004-6361/201936665

    work page doi:10.1051/0004-6361/201936665 2020

  16. [16]

    doi:10.1051/0004-6361/202452282

    Casavecchia, B., Maio, U., P \'e roux, C., et al.\ 2025, , 693, A119. doi:10.1051/0004-6361/202452282

    work page doi:10.1051/0004-6361/202452282 2025

  17. [17]

    , keywords =

    Casey, C. M.\ 2012, , 425, 4, 3094. doi:10.1111/j.1365-2966.2012.21455.x

    work page doi:10.1111/j.1365-2966.2012.21455.x 2012

  18. [18]

    J., et al.\ 2026, The Open Journal of Astrophysics, 9, 58199

    Choustikov, N., Katz, H., Cameron, A. J., et al.\ 2026, The Open Journal of Astrophysics, 9, 58199. doi:10.33232/001c.158199

    work page doi:10.33232/001c.158199 2026

  19. [19]

    doi:10.1051/0004-6361/201424980

    Cicone, C., Maiolino, R., Gallerani, S., et al.\ 2015, , 574, A14. doi:10.1051/0004-6361/201424980

    work page doi:10.1051/0004-6361/201424980 2015

  20. [20]

    R., et al.\ 2015, , 806, 1, 110

    da Cunha, E., Walter, F., Smail, I. R., et al.\ 2015, , 806, 1, 110. doi:10.1088/0004-637X/806/1/110

    work page doi:10.1088/0004-637x/806/1/110 2015

  21. [21]

    Nature Astronomy , keywords =

    D'Eugenio, F., P \'e rez-Gonz \'a lez, P. G., Maiolino, R., et al.\ 2024, Nature Astronomy, 8, 1443. doi:10.1038/s41550-024-02345-1

    work page doi:10.1038/s41550-024-02345-1 2024

  22. [22]

    doi:10.1051/0004-6361/201834444

    De Vis, P., Jones, A., Viaene, S., et al.\ 2019, , 623, A5. doi:10.1051/0004-6361/201834444

    work page doi:10.1051/0004-6361/201834444 2019

  23. [23]

    T.\ 2011,

    Draine, B. T.\ 2011,

    2011

  24. [24]

    A., Boyle, B

    Dunne, L., Eales, S., Edmunds, M., et al.\ 2000, , 315, 1, 115. doi:10.1046/j.1365-8711.2000.03386.x

    work page doi:10.1046/j.1365-8711.2000.03386.x 2000

  25. [25]

    doi:10.1086/305829

    Dwek, E.\ 1998, , 501, 643. doi:10.1086/305829

    work page doi:10.1086/305829 1998

  26. [26]

    doi:10.1051/0004-6361/202453214

    Fern \'a ndez Aranda, R., D \' az Santos, T., Hatziminaoglou, E., et al.\ 2025, , 695, L15. doi:10.1051/0004-6361/202453214

    work page doi:10.1051/0004-6361/202453214 2025

  27. [27]

    W., Lang, D., et al.\ 2013, , 125, 306

    Foreman-Mackey, D., Hogg, D. W., Lang, D., et al.\ 2013, , 125, 925, 306. doi:10.1086/670067

    work page doi:10.1086/670067 2013

  28. [28]

    doi:10.3847/1538-4357/aa93e6

    Fujimoto, S., Ouchi, M., Shibuya, T., et al.\ 2017, , 850, 1, 83. doi:10.3847/1538-4357/aa93e6

    work page doi:10.3847/1538-4357/aa93e6 2017

  29. [29]

    doi:10.3847/1538-4357/ad235c

    Fujimoto, S., Ouchi, M., Nakajima, K., et al.\ 2024, , 964, 2, 146. doi:10.3847/1538-4357/ad235c

    work page doi:10.3847/1538-4357/ad235c 2024

  30. [30]

    Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al.\ 2021, , 649, A1. doi:10.1051/0004-6361/202039657

    work page doi:10.1051/0004-6361/202039657 2021

  31. [31]

    D., Clayton, G

    Gordon, K. D., Clayton, G. C., Misselt, K. A., et al.\ 2003, , 594, 1, 279. doi:10.1086/376774

    work page doi:10.1086/376774 2003

  32. [32]

    Greene, J. E. & Ho, L. C.\ 2005, , 630, 1, 122. doi:10.1086/431897

    work page internal anchor Pith review doi:10.1086/431897 2005

  33. [33]

    E., Seth, A., Kim, M., et al.\ 2016, , 826, 2, L32

    Greene, J. E., Seth, A., Kim, M., et al.\ 2016, , 826, 2, L32. doi:10.3847/2041-8205/826/2/L32

    work page doi:10.3847/2041-8205/826/2/l32 2016

  34. [34]

    , keywords =

    Greene, J. E., Labbe, I., Goulding, A. D., et al.\ 2024, , 964, 1, 39. doi:10.3847/1538-4357/ad1e5f

    work page doi:10.3847/1538-4357/ad1e5f 2024

  35. [35]

    K., et al.\ 2025, , 990, 1, 29

    Hagimoto, M., Tamura, Y., Inoue, A. K., et al.\ 2025, , 990, 1, 29. doi:10.3847/1538-4357/ade87e

    work page doi:10.3847/1538-4357/ade87e 2025

  36. [36]

    , keywords =

    Harikane, Y., Zhang, Y., Nakajima, K., et al.\ 2023, , 959, 1, 39. doi:10.3847/1538-4357/ad029e

    work page doi:10.3847/1538-4357/ad029e 2023

  37. [37]

    L., Ellis, R., et al.\ 2025, , 993, 2, 204

    Harikane, Y., Sanders, R. L., Ellis, R., et al.\ 2025, , 993, 2, 204. doi:10.3847/1538-4357/ae0e53

    work page doi:10.3847/1538-4357/ae0e53 2025

  38. [38]

    S., et al.\ 2024, , 977, 2, L36

    Harshan, A., Tripodi, R., Martis, N. S., et al.\ 2024, , 977, 2, L36. doi:10.3847/2041-8213/ad9741

    work page doi:10.3847/2041-8213/ad9741 2024

  39. [39]

    S.\ 2023, , 526, 3, 3504

    Hirschmann, M., Charlot, S., & Somerville, R. S.\ 2023, , 526, 3, 3504. doi:10.1093/mnras/stad2745

    work page doi:10.1093/mnras/stad2745 2023

  40. [40]

    doi:10.1088/0004-637X/815/1/18

    Infante, L., Zheng, W., Laporte, N., et al.\ 2015, , 815, 1, 18. doi:10.1088/0004-637X/815/1/18

    work page doi:10.1088/0004-637x/815/1/18 2015

  41. [41]

    K., Tamura, Y., Matsuo, H., et al.\ 2016, Science, 352, 6293, 1559

    Inoue, A. K., Tamura, Y., Matsuo, H., et al.\ 2016, Science, 352, 6293, 1559. doi:10.1126/science.aaf0714

    work page doi:10.1126/science.aaf0714 2016

  42. [42]

    doi:10.3847/1538-4357/acf376

    Isobe, Y., Ouchi, M., Nakajima, K., et al.\ 2023, , 956, 2, 139. doi:10.3847/1538-4357/acf376

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

  43. [43]

    doi:10.1051/0004-6361:20053763 , Eprint =

    Izotov, Y. I., Stasi \'n ska, G., Meynet, G., et al.\ 2006, , 448, 3, 955. doi:10.1051/0004-6361:20053763

    work page doi:10.1051/0004-6361:20053763 2006

  44. [44]

    C., Witstok, J., Concas, A., et al.\ 2024, , 529, 1, L1

    Jones, G. C., Witstok, J., Concas, A., et al.\ 2024, , 529, 1, L1. doi:10.1093/mnrasl/slad189

    work page doi:10.1093/mnrasl/slad189 2024

  45. [45]

    M., et al.\ 2011, , 736, 2, 104

    Juneau, S., Dickinson, M., Alexander, D. M., et al.\ 2011, , 736, 2, 104. doi:10.1088/0004-637X/736/2/104

    work page doi:10.1088/0004-637x/736/2/104 2011

  46. [46]

    Resolving the Dust Budget Crisis at $z \sim 8$ with Optically Thick, High-Density Molecular Clumps: MACS0416_Y1

    Kano, R. R., Takeuchi, T. T., Kawamoto, E. R., et al.\ 2026, arXiv:2604.19928. doi:10.48550/arXiv.2604.19928

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.19928 2026

  47. [47]

    doi:10.3847/0004-637X/819/2/114

    Kawamata, R., Oguri, M., Ishigaki, M., et al.\ 2016, , 819, 2, 114. doi:10.3847/0004-637X/819/2/114

    work page doi:10.3847/0004-637x/819/2/114 2016

  48. [48]

    J., Maier, C., Yabe, K., et al.\ 2013, , 774, 1, L10

    Kewley, L. J., Maier, C., Yabe, K., et al.\ 2013, , 774, 1, L10. doi:10.1088/2041-8205/774/1/L10

    work page doi:10.1088/2041-8205/774/1/l10 2013

  49. [49]

    M., et al.\ 2012, , 759, 2, 139

    Kirkpatrick, A., Pope, A., Alexander, D. M., et al.\ 2012, , 759, 2, 139. doi:10.1088/0004-637X/759/2/139

    work page doi:10.1088/0004-637x/759/2/139 2012

  50. [50]

    doi:10.3847/1538-4357/ae1cc3

    Kiyota, T., Ouchi, M., Xu, Y., et al.\ 2025, , 995, 2, 150. doi:10.3847/1538-4357/ae1cc3

    work page doi:10.3847/1538-4357/ae1cc3 2025

  51. [51]

    doi:10.48550/arXiv.2601.18149

    Kiyota, T., Ouchi, M., Iono, D., et al.\ 2026, arXiv:2601.18149. doi:10.48550/arXiv.2601.18149

    work page doi:10.48550/arxiv.2601.18149 2026

  52. [52]

    Kormendy, J. & Ho, L. C.\ 2013, , 51, 1, 511. doi:10.1146/annurev-astro-082708-101811

    work page internal anchor Pith review doi:10.1146/annurev-astro-082708-101811 2013

  53. [53]

    , keywords =

    Matthee, J., Naidu, R. P., Brammer, G., et al.\ 2024, , 963, 2, 129. doi:10.3847/1538-4357/ad2345

    work page doi:10.3847/1538-4357/ad2345 2024

  54. [54]

    E., et al.\ 2024, , 971, 2, 161

    Mitsuhashi, I., Harikane, Y., Bauer, F. E., et al.\ 2024, , 971, 2, 161. doi:10.3847/1538-4357/ad5675

    work page doi:10.3847/1538-4357/ad5675 2024

  55. [55]

    K., et al.\ 2026, arXiv:2602.07347

    Nakazato, Y., Matsumoto, K., Inoue, A. K., et al.\ 2026, arXiv:2602.07347. doi:10.48550/arXiv.2602.07347

    work page doi:10.48550/arxiv.2602.07347 2026

  56. [56]

    doi:10.1051/0004-6361/201425040

    Laporte, N., Streblyanska, A., Kim, S., et al.\ 2015, , 575, A92. doi:10.1051/0004-6361/201425040

    work page doi:10.1051/0004-6361/201425040 2015

  57. [57]

    M., Koekemoer, A., Coe, D., et al.\ 2017, , 837, 1, 97

    Lotz, J. M., Koekemoer, A., Coe, D., et al.\ 2017, , 837, 1, 97. doi:10.3847/1538-4357/837/1/97

    work page doi:10.3847/1538-4357/837/1/97 2017

  58. [58]

    A.\ 2015, , 573, A42

    Luridiana, V., Morisset, C., & Shaw, R. A.\ 2015, , 573, A42. doi:10.1051/0004-6361/201323152

    work page doi:10.1051/0004-6361/201323152 2015

  59. [59]

    doi:10.3847/1538-4357/ad7b32

    Ma, Z., Sun, B., Cheng, C., et al.\ 2024, , 975, 1, 87. doi:10.3847/1538-4357/ad7b32

    work page doi:10.3847/1538-4357/ad7b32 2024

  60. [60]

    , keywords =

    Maiolino, R., Gallerani, S., Neri, R., et al.\ 2012, , 425, 1, L66. doi:10.1111/j.1745-3933.2012.01303.x

    work page doi:10.1111/j.1745-3933.2012.01303.x 2012

  61. [61]

    doi:10.1093/mnrasl/slv070

    Mancini, M., Schneider, R., Graziani, L., et al.\ 2015, , 451, L70. doi:10.1093/mnrasl/slv070

    work page doi:10.1093/mnrasl/slv070 2015

  62. [62]

    A., Walter, F., Di Mascia, F., et al.\ 2025, , 695, L18

    Meyer, R. A., Walter, F., Di Mascia, F., et al.\ 2025, , 695, L18. doi:10.1051/0004-6361/202453279

    work page doi:10.1051/0004-6361/202453279 2025

  63. [63]

    doi:10.1017/S1743921319002424

    Moriwaki, K.\ 2020, Panchromatic Modelling with Next Generation Facilities, 341, 249. doi:10.1017/S1743921319002424

    work page doi:10.1017/s1743921319002424 2020

  64. [64]

    doi:10.3847/1538-4365/ac7710

    Nakajima, K., Ouchi, M., Xu, Y., et al.\ 2022, , 262, 1, 3. doi:10.3847/1538-4365/ac7710

    work page doi:10.3847/1538-4365/ac7710 2022

  65. [65]

    doi:10.3847/1538-4365/acd556

    Nakajima, K., Ouchi, M., Isobe, Y., et al.\ 2023, , 269, 2, 33. doi:10.3847/1538-4365/acd556

    work page doi:10.3847/1538-4365/acd556 2023

  66. [66]

    doi:10.48550/arXiv.2506.11846

    Nakajima, K., Ouchi, M., Harikane, Y., et al.\ 2025, , arXiv:2506.11846. doi:10.48550/arXiv.2506.11846

    work page doi:10.48550/arxiv.2506.11846 2025

  67. [67]

    doi:10.3847/1538-4357/ace25a

    Nakazato, Y., Yoshida, N., & Ceverino, D.\ 2023, , 953, 2, 140. doi:10.3847/1538-4357/ace25a

    work page doi:10.3847/1538-4357/ace25a 2023

  68. [68]

    Osterbrock, D. E. & Mathews, W. G.\ 1986, , 24, 171. doi:10.1146/annurev.aa.24.090186.001131

    work page doi:10.1146/annurev.aa.24.090186.001131 1986

  69. [69]

    Osterbrock, D. E. & Ferland, G. J.\ 2006,

    2006

  70. [70]

    Pagel, B. E. J., Simonson, E. A., Terlevich, R. J., et al.\ 1992, , 255, 325. doi:10.1093/mnras/255.2.325

    work page doi:10.1093/mnras/255.2.325 1992

  71. [71]

    doi:10.1093/mnras/stae160

    Palla, M., De Looze, I., Rela \ n o, M., et al.\ 2024, , 528, 2, 2407. doi:10.1093/mnras/stae160

    work page doi:10.1093/mnras/stae160 2024

  72. [72]

    , keywords =

    P \'e roux, C. & Howk, J. C.\ 2020, , 58, 363. doi:10.1146/annurev-astro-021820-120014

    work page doi:10.1146/annurev-astro-021820-120014 2020

  73. [73]

    Aghanim, et al

    Planck Collaboration, Aghanim, N., Akrami, Y., et al.\ 2020, , 641, A6. doi:10.1051/0004-6361/201833910

    work page doi:10.1051/0004-6361/201833910 2020

  74. [74]

    S., & Galametz, M.\ 2017, , 471, 3, 3152

    Popping, G., Somerville, R. S., & Galametz, M.\ 2017, , 471, 3, 3152. doi:10.1093/mnras/stx1545

    work page doi:10.1093/mnras/stx1545 2017

  75. [75]

    W., Fudamoto, Y., Inoue, A

    Ren, Y. W., Fudamoto, Y., Inoue, A. K., et al.\ 2023, , 945, 1, 69. doi:10.3847/1538-4357/acb8ab

    work page doi:10.3847/1538-4357/acb8ab 2023

  76. [76]

    T., Lacy, M., Storrie-Lombardi, L

    Richards, G. T., Lacy, M., Storrie-Lombardi, L. J., et al.\ 2006, , 166, 2, 470. doi:10.1086/506525

    work page internal anchor Pith review doi:10.1086/506525 2006

  77. [77]

    R., Vieira, J

    Rigby, J. R., Vieira, J. D., Phadke, K. A., et al.\ 2025, , 978, 1, 108. doi:10.3847/1538-4357/ad7501

    work page doi:10.3847/1538-4357/ad7501 2025

  78. [78]

    doi:10.1051/0004-6361/202347444

    Rihtar s i c , G., Biffi, V., Fabjan, D., et al.\ 2024, , 683, A57. doi:10.1051/0004-6361/202347444

    work page doi:10.1051/0004-6361/202347444 2024

  79. [79]

    doi:10.48550/arXiv.2601.06255

    Rodr \' guez Del Pino, B., Arribas, S., Perna, M., et al.\ 2026, arXiv:2601.06255. doi:10.48550/arXiv.2601.06255

    work page doi:10.48550/arxiv.2601.06255 2026

  80. [80]

    S., Rieke, G

    Rujopakarn, W., Dunlop, J. S., Rieke, G. H., et al.\ 2016, , 833, 1, 12. doi:10.3847/0004-637X/833/1/12

    work page doi:10.3847/0004-637x/833/1/12 2016

Showing first 80 references.