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Discovery of Local Analogs to JWST's Little Red Dots

T0 review · 3 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read Seven low-redshift Green Pea galaxies with broad-line active nuclei reproduce the V-shaped ultraviolet-to-optical spectral energy distributions of JWST's Little Red Dots, making them local analogs for studying these high-redshift objects.

desk verdict A timely, honest proposal that low-z broad-line green peas are local LRD analogs, but the V-shaped selection is too noisy to pin down seven secure analogs. read the letter →

arxiv 2412.08396 v1 pith:A5F3JODT submitted 2024-12-11 astro-ph.GA

Ruqiu Lin , Zhen-Ya Zheng , Chunyan Jiang , Fang-Ting Yuan , Luis C. Ho , Junxian Wang , Linhua Jiang , James E. Rhoads
show 7 more authors
Sangeeta Malhotra L. Felipe Barrientos Isak Wold Leopoldo Infante Shuairu Zhu Xiang Ji Xiaodan Fu
This is my paper · ORCID
classification astro-ph.GA
keywords LittleRedDotsGreenpeagalaxiesbroad-lineAGNV-shapedSEDover-massiveblackholeslocalanalogsgalaxyevolutionactivegalacticnuclei
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper argues that a subset of low-redshift Green Pea galaxies that host broad-line active galactic nuclei (BLGPs) reproduce the defining photometric signature of JWST's high-redshift Little Red Dots: a V-shaped spectral energy distribution, blue in the rest-frame ultraviolet and red in the rest-frame optical. Seven of 19 BLGPs satisfy this V-shape criterion, and they match Little Red Dots in faint ultraviolet absolute magnitude, sub-Eddington accretion rates, and, for three objects, narrow-line ratios that imply similar ionization conditions and gas-phase metallicities. If the analogy holds, these nearby dwarf galaxies become local test beds for questions about Little Red Dots that JWST cannot yet answer, especially what produces the blue ultraviolet light. The paper also reports that 16 of the 19 BLGPs host black holes more massive than the local scaling relation predicts, constituting the first over-massive black hole sample found at $z<0.4$.

What carries the argument

The load-bearing selection device is the V-shaped SED criterion, defined through continuum slopes $\beta$ (with $f_\lambda=\lambda^\beta$): a blue ultraviolet slope $\beta_{\rm UV}\lesssim-0.37$ measured from GALEX NUV and SDSS $u$-band photometry, and a red optical slope $\beta_{\rm opt}\gtrsim0$ measured from SDSS $i$- and $z$-band magnitudes after subtracting strong emission lines. Applied to a parent sample of 19 Green Pea galaxies with broad H$\alpha$ (FWHM $>1000$ km s$^{-1}$), this criterion selects the 7 V-shaped BLGPs that the paper identifies as local analogs. Supporting machinery includes virial black hole masses from broad H$\alpha$ using a scale factor $f=4.47$, BPT narrow-line diagnostics, WISE mid-infrared AGN classification, and a comparison of the V-shape break wavelength with black hole mass that shows a likely anti-correlation.

What would settle it

Take deep, line-free rest-frame ultraviolet and optical spectra of the seven candidate V-shaped BLGPs; if more than two of them lose their V-shape once the continuum is measured directly rather than inferred from line-subtracted photometry, or if their Eddington ratios become super-Eddington under re-derived bolometric corrections, the claimed local-analog status would not survive.

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Extended reading notes

Core claim

The central claim is that V-shaped BLGPs should be regarded as local analogs of Little Red Dots. Seven of the 19 broad-line Green Pea galaxies show rest-frame ultraviolet-to-optical SEDs with $\beta_{\rm UV}\lesssim-0.37$ and $\beta_{\rm opt}\gtrsim0$, the same V-shape criterion used for high-redshift Little Red Dots, together with broad H$\alpha$ lines wider than $1000$ km s$^{-1}$. These seven objects have ultraviolet absolute magnitudes around $-19$ mag, Eddington ratios near $0.1$, and, in three cases, BPT line ratios coincident with those of the Little Red Dot JADES 10013704, leading the authors to conclude that V-shaped BLGPs are the same kind of object as Little Red Dots observed at different cosmic epochs. In addition, 16 of the 19 BLGPs lie above the local $M_{\rm BH}$--$M_*$ relation by more than $1\sigma$, so the paper claims the over-massive black hole phenomenon seen in high-redshift JWST sources also exists locally, with the black holes often ten times more massive than expected for their host stellar masses.

Load-bearing premise

The identification of the V-shape rests on continuum slopes measured from broad-band photometry after subtracting strong emission lines, assuming the high-redshift Little Red Dot V-shape criterion transfers to low-redshift Green Pea galaxies and that virial black hole masses with a fixed scale factor are reliable in dwarf hosts.

Editorial extensions

If this is right

  • Because V-shaped BLGPs lie at $z<0.4$, their ultraviolet emission can be observed with high sensitivity and spatial resolution, so deep ultraviolet spectroscopy and imaging can settle whether Little Red Dot ultraviolet light is scattered AGN light or young stellar emission.
  • The apparent correlation between V-shape break wavelength and black hole mass becomes a local constraint on the AGN-galaxy hybrid SED models proposed for Little Red Dots.
  • A sample of 16 over-massive black holes at $z<0.4$ provides a local benchmark that seeding and growth models for early black holes must reproduce.
  • Three V-shaped BLGPs occupy the same BPT region as Little Red Dots, implying that the ionization conditions and gas-phase metallicities of these high-redshift objects can be studied in detail in nearby galaxies.
  • If the analogy holds, Green Pea galaxies offer a statistically accessible local population for studying the co-evolution of compact galaxies and their central black holes across cosmic time.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A testable extension the authors do not pursue: monitor the seven V-shaped BLGPs for ultraviolet and optical variability; if they are true Little Red Dot analogs, they should show AGN-driven flickering on timescale scales comparable to the months-to-years variability reported in Little Red Dots.
  • The over-massive black hole result implies a local population of possible 'leftover seeds' that have avoided significant merging or growth; an untested consequence is that their host galaxies should show suppressed star formation or disturbed morphologies, which deep imaging could check.
  • The 7 of 19 fraction is likely a lower bound rather than a physical dichotomy, because GALEX coverage and emission-line contamination differ at low redshift; some non-V-shaped BLGPs might be analogs whose V-shape is washed out by selection effects.
  • If the break-wavelength versus black-hole-mass anti-correlation is confirmed in a larger sample, it would suggest the V-shape is a phase in AGN-galaxy evolution rather than a separate population, tying the Little Red Dot phenomenon to the growth state of the central black hole.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The manuscript reports the discovery of seven Green Pea galaxies with broad H-alpha lines (BLGPs) at z<0.4 that show V-shaped rest-frame UV-to-optical SEDs, selected from 19 BLGPs using the same beta_UV and beta_opt thresholds used for high-redshift little red dots (LRDs). The authors argue these are local analogs of LRDs based on similar SED shapes, faint UV absolute magnitudes, BPT line ratios (for three of seven), sub-Eddington accretion, and over-massive BHs. They also report that 16/19 BLGPs lie above the local M_BH-M_* relation, which they claim is the first such sample at z<0.4.

Significance. If the analog identification holds, the sample provides a rare low-z laboratory for studying the physical origin of LRD UV emission and the growth of over-massive BHs in dwarf hosts. The paper benefits from using a well-defined parent sample, explicit line-subtracted broad-band photometry, and side-by-side SED and spectral comparisons with a JWST LRD. However, the central claims rest on small numbers and on selection and virial-calibration assumptions that need quantitative treatment before the conclusions are fully supported.

major comments (3)
  1. [Section 2.2, Table 1] The V-shaped classification is not statistically secure for at least three of the seven selected sources: J092359+415736 (beta_UV = -0.54 +/- 0.66), J092834+292136 (beta_UV = -0.39 +/- 0.42), and J115438+065025 (beta_UV = -0.45 +/- 0.44) all lie within 1-sigma of the beta_UV <= -0.37 threshold, and J092834+292136 also has beta_opt = 0.21 +/- 0.31, only ~0.7-sigma above zero. Because the seven V-shaped BLGPs are the empirical basis for the analog claim, the authors should propagate the photometric errors into the classification (e.g., report a membership probability per source) or repeat the comparison using only the securely classified subsample, and state whether the conclusions survive.
  2. [Section 2.2, Figure 1] The V-shaped selection uses the same beta_UV and beta_opt thresholds that define LRDs, so the SED-shape similarity between the selected BLGPs and LRDs is partly by construction. The paper should state this explicitly and present the independent checks (M_UV, BPT location, Eddington ratio, M_BH-M_*) as the actual tests of the analog hypothesis. The current presentation, especially the claim in Section 5 that 'V-shaped BLGPs and LRDs are similar populations at different redshifts,' would be strengthened by a more guarded wording and by a quantitative discussion of how many of the seven pass each independent test.
  3. [Section 4.2, Table 1 and Figure 4] The claim that 16/19 BLGPs host over-massive BHs above the local M_BH-M_* relation by more than 1-sigma relies on virial BH masses with an adopted f = 4.47 and a stated ~0.4 dex systematic uncertainty, while the local relation itself has intrinsic scatter. The authors should quantify the expected number of galaxies that would lie above the relation given the measurement errors and the intrinsic scatter (e.g., via Monte Carlo), and should also discuss selection effects in the BLGP sample, before asserting that this is a rare and physically significant population.
minor comments (4)
  1. [Throughout] Please fix typographical errors: 'euqation' in Section 2.2, 'obsolute' in Section 3.2, 'Edington' and 'sub-Eddinton' for Eddington in Section 3.2 and Section 5, and 'classificaition' in the Table 2 footnote.
  2. [Section 3.1] The reported 'likely inverse correlation between the break wavelength of the V-shaped SED and the BH mass' is based on only seven points and visual inspection; please provide a correlation coefficient and significance, or soften the claim.
  3. [Section 2.3] In the discussion of J122245+360218, 'this 330-day time lag' should be 'time interval,' and the sentence describing which band matches the photometric magnitude should identify the band explicitly.
  4. [Figure 2] The comparison SED is a single LRD (JADES 10013704); please state whether this object is representative of the LRD population or an unusually clear example, since the visual match of the analogs to this single object is used to motivate retaining J122245+360218.

Circularity Check

2 steps flagged · score 5.0 of 10

The V-shaped-SED and broad-line-width similarities are partly by construction, because the sample is selected with the same beta_UV/beta_opt thresholds and FWHM cut used for LRDs, while the other analog properties are independently measured.

  1. self definitional [Section 2.2 (selection criteria), Section 3.1 (identification), Section 3.2 (claimed similarity)]
    "Finally, following the methodology in Kocevski et al. (2024), we utilize the continuum slopes β ... The criteria used here are βUV ≲ −0.37 for the blue UV continuum slope and βopt ≳ 0 for the red optical continuum slope ... Based on the broad Hα line width and the continuum slope criteria, we identify 7 V-shaped BLGPs as local analogs to LRDs from a sample of 19 BLGPs."

    The 'V-shaped BLGPs' are defined by imposing the same β_UV ≤ -0.37 and β_opt ≥ 0 thresholds that define the LRD V-shape. Therefore the later claim in Section 3.2 that V-shaped BLGPs resemble LRDs 'in terms of ... rest-frame UV-to-optical SEDs' is true by construction: the SED-shape similarity is the selection rule, not an independent empirical finding. The independent content of the analog claim must come from the other properties, which are not part of this selection.

  2. self definitional [Section 2.2 (FWHM cut), Section 3.2 (claimed broad-line similarity)]
    "First, we require a line width cut of the broad Hα line as FWHMHα, broad > 1000 km s−1, which is the selection criterion for high-z faint broad-line AGNs in Matthee et al. (2023). ... V-shaped BLGPs exhibit similar properties to LRDs, not only in terms of broad-line widths and rest-frame UV-to-optical SEDs but also regarding rest-frame UV absolute magnitudes, the relation of optical slopes and BH masses, narrow-line diagnostics, and Eddington ratios."

    The sample is explicitly restricted to objects with FWHM(Hα) > 1000 km/s, the same cut used for the high-z broad-line AGN comparison sample. Consequently, the statement that V-shaped BLGPs share 'broad-line widths' with LRDs is entailed by the sample definition rather than being a measured similarity. This is a second place where a selection criterion is later presented as a discovered shared property.

full rationale

The paper's central 'local analog' claim has two components. The rest-frame UV-to-optical SED shape and the broad-line width are imposed by the selection: Section 2.2 applies the Kocevski et al. (2024) β_UV ≤ -0.37 and β_opt ≥ 0 thresholds and the Matthee et al. (2023) FWHM(Hα) > 1000 km/s cut, so the later statements in Section 3.2 that V-shaped BLGPs share these properties with LRDs restate the selection criteria. The other similarities—faint M_UV, sub-Eddington λ_Edd, BPT narrow-line ratios, and location above the local M_BH-M_* relation—are not encoded in the selection and provide independent empirical content; the over-massive-BH claim (16/19 BLGPs) does not depend on the V-shape cut. The marginal β_UV values flagged in Table 1 are a statistical robustness concern, not a circularity. Overall, the paper is partially circular in presenting its own selection cuts as discovered similarities, but the analog conclusion is not forced by definition alone.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

No new physical entities are introduced; the analysis reclassifies existing objects using criteria from LRD studies.

free parameters (4)
  • UV slope threshold beta_UV = -0.37
    Adopted from Kocevski et al. (2024) LRD selection; chosen by hand, directly determines which objects are V-shaped.
  • Optical slope threshold beta_opt = 0
    Adopted from Kocevski et al. (2024); together with beta_UV defines the V-shape.
  • Virial factor f = 4.47
    Adopted from Woo et al. (2015) for Halpha; scales all BH masses and underpins the over-massive BH claim.
  • Bolometric correction L_bol/L_5100 = 9.8
    Adopted from McLure & Dunlop (2004) to estimate Eddington ratios for comparison with LRDs.
assumptions (4)
  • domain assumption Continuum slopes from line-subtracted broadband photometry trace the true AGN+host SED
    Section 2.2-2.3; optical slope computed from i,z magnitudes after Halpha subtraction, but emission-line variability and continuum faintness introduce unquantified bias.
  • domain assumption The V-shape criterion for LRDs is transferable to z<0.4
    Section 2.2; the beta_UV and beta_opt thresholds are taken from high-z LRD studies, assuming the same rest-frame features select the same physical population.
  • domain assumption Virial BH masses with f=4.47 apply to low-mass dwarf galaxies
    Section 2.1; BH masses are derived from broad Halpha via relations calibrated on AGN samples, with 0.4 dex uncertainty; whether they hold for compact dwarf hosts is untested.
  • domain assumption GPs are local analogs of high-z star-forming galaxies
    Section 1; this motivates the search but is not proven for the AGN subset.

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Cite this review

Pith. "Pith review of Discovery of Local Analogs to JWST's Little Red Dots." pith.science (2026). https://pith.science/paper/A5F3JODT

@misc{pith2026241208396,
  author       = {Pith},
  title        = {Pith review of: Discovery of Local Analogs to JWST's Little Red Dots},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/A5F3JODT}},
  note         = {Machine review of arXiv:2412.08396}
}
abstract

Recently, the James Webb Space Telescope (JWST) has revealed a new class of high redshift (high-$z$, $z>4$) compact galaxies which are red in the rest-frame optical and blue in the rest-frame UV as V-shaped spectral energy distributions (SEDs), referred to as "Little Red Dots" (LRDs). It is very likely that LRDs host obscured broad-line active galactic nuclei (AGNs). In the meanwhile, Green pea galaxies (GPs), which are compact dwarf galaxies at low redshift, share various similar properties with high redshift star-forming galaxies. Here we aim to find the connection between the LRDs and GPs hosting broad-line AGNs (BLGPs). With a sample of 19 BLGPs obtained from our previous work, we further identify 7 GPs with V-shaped rest-frame UV-to-optical SEDs that are likely local analogs to LRDs. These V-shaped BLGPs exhibit faint UV absolute magnitudes and sub-Eddington rates similar to those of LRDs. Three of them occupy a similar region as LRDs in the BPT diagram, suggesting they have similar ionization conditions and gas-phase metallicities to LRDs. These similarities suggest that V-shaped BLGPs can be taken as local analogs of high-redshift LRDs. In addition, most (16/19) BLGPs, including 6 V-shaped BLGPs, host over-massive black holes above the local $M_{\rm BH}$-$M_{*}$ relation, making it the first sample of galaxies hosting over-massive black holes at $z<0.4$. These findings will help us learn more about the formation and co-evolution of early galaxies and black holes.

Figures

Figures reproduced from arXiv: 2412.08396 by the authors.

Figure 1
Figure 1. Optical continuum slope βopt vs. UV continuum slope βUV for the GPs hosting broad-line AGNs (stars). The shaded area presents the LRDs selection criteria (Kocevski et al. 2024) with the V-shaped UV-to-optical SEDs. The V-shaped BLGPs are marked on blue squares. The color bar shows the fraction of broad to total Hα flux for our BLGP sample. For comparison, we illustrate high-z broad￾line AGNs including LRDs reported … view at source ↗
Figure 2
Figure 2. Left column: Comparison of rest-frame UV-to-optical SEDs between the V-shaped BLGPs at z ∼ 0.3 (green dots) and a LRD (JADES 10013704) at z = 5.9 reported in Maiolino et al. (2023) (red dots). The green circles represent the continuum flux after subtracting emission lines. The background red line and the image in the upper left are the NIRSpec/PRISM spectrum and the NIRCam F115W-F200W-F444W color cutout of JADES 100… view at source ↗
Figure 3
Figure 3. Panel a: Optical continuum slope vs. BH mass for BLGPs (stars). For comparison, we illustrate high-z broad-line AGNs including LRDs reported in Maiolino et al. (2023), Matthee et al. (2023), Greene et al. (2024), and Harikane et al. (2023), if available. Panel b: BPT diagram. The classification lines follow Kewley et al. (2001) (solid line) and Kauffmann et al. (2003) (dashed line), also seen in Kewley et al. (2006)… view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: MBH vs. M∗ diagram. For comparison, we il￾lustrate high-z broad-line AGNs including LRDs reported in Maiolino et al. (2023), Kocevski et al. (2023), and Harikane et al. (2023). Six LRDs with stellar mass measurements derived by Chen et al. (2024) are also plotted. The …

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Forward citations

Cited by 3 Pith papers

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

  1. Two Peas in a Pod: The First Confirmed Dual Active Galactic Nucleus within a Green Pea Galaxy System

    astro-ph.GA 2026-07 conditional novelty 7.0 of 10

    A compact Green Pea galaxy system hosts two resolved, simultaneously accreting supermassive black holes — the first confirmed dual AGN in such a galaxy.

  2. Where did all the Little Red Dots go? The abundance of LRD analogues among objects with broad lines at $z < 0.35$

    astro-ph.GA 2026-08 conditional novelty 6.0 of 10

    Only 0.08% of low-redshift broad-line objects have SEDs resembling high-redshift Little Red Dots, yielding nine candidates, one of which is the known analogue 'The Egg'.

  3. ATLAS. II. Extremely High Incidence of Balmer Line Absorption with Predominant Blueshifts in LRDs: Statistical Insights through Comparison with Type 1 AGNs

    astro-ph.GA 2026-07 conditional novelty 6.0 of 10

    Balmer-line absorption occurs in ~35% (14/40) of JWST little-red-dot AGNs, roughly 850x the rate in SDSS type-1 AGNs, with mostly slow blueshifted absorber velocities.

Reference graph

Works this paper leans on

63 extracted references · 1 canonical work pages · cited by 3 Pith papers

  1. [1]

    B., Casey, C

    Akins, H. B., Casey, C. M., Allen, N., et al. 2023, ApJ, 956, 61, doi: 10.3847/1538-4357/acef21 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f

    doi:10.3847/1538-4357/acef21 2023

  2. [2]

    A., Phillips, M

    Baldwin, J. A., Phillips, M. M., & Terlevich, R. 1981, PASP, 93, 5, doi: 10.1086/130766

    doi:10.1086/130766 1981

  3. [3]

    G., Kocevski, D

    Barro, G., P´ erez-Gonz´ alez, P. G., Kocevski, D. D., et al. 2024, ApJ, 963, 128, doi: 10.3847/1538-4357/ad167e

    doi:10.3847/1538-4357/ad167e 2024

  4. [4]

    2019, A&A, 622, A103, doi: 10.1051/0004-6361/201834156

    Boquien, M., Burgarella, D., Roehlly, Y., et al. 2019, A&A, 622, A103, doi: 10.1051/0004-6361/201834156

    doi:10.1051/0004-6361/201834156 2019

  5. [5]

    M., Leitherer, C., & Overzier, R

    Borthakur, S., Heckman, T. M., Leitherer, C., & Overzier, R. A. 2014, Science, 346, 216, doi: 10.1126/science.1254214

    doi:10.1126/science.1254214 2014

  6. [6]

    2023, MNRAS, 525, 2087, doi: 10.1093/mnras/stad1704

    Brinchmann, J. 2023, MNRAS, 525, 2087, doi: 10.1093/mnras/stad1704

    doi:10.1093/mnras/stad1704 2023

  7. [7]

    2005, MNRAS, 360, 1413, doi: 10.1111/j.1365-2966.2005.09131.x

    Burgarella, D., Buat, V., & Iglesias-P´ aramo, J. 2005, MNRAS, 360, 1413, doi: 10.1111/j.1365-2966.2005.09131.x

    arXiv 2005

  8. [8]

    2009, MNRAS, 399, 1191, doi: 10.1111/j.1365-2966.2009.15383.x

    Cardamone, C., Schawinski, K., Sarzi, M., et al. 2009, MNRAS, 399, 1191, doi: 10.1111/j.1365-2966.2009.15383.x

    arXiv 2009

Show all 63 references
  1. [9]

    C., Li, R., & Zhuang, M.-Y

    Chen, C.-H., Ho, L. C., Li, R., & Zhuang, M.-Y. 2024, arXiv e-prints, arXiv:2411.04446, doi: 10.48550/arXiv.2411.04446 10

    2024 doi arXiv

  2. [10]

    R., Jaskot, A

    Flury, S. R., Jaskot, A. E., Ferguson, H. C., et al. 2022, ApJS, 260, 1, doi: 10.3847/1538-4365/ac5331

    2022 doi

  3. [11]

    J., Labb´ e, I., Zitrin, A., et al

    Furtak, L. J., Labb´ e, I., Zitrin, A., et al. 2024, Nature, 628, 57, doi: 10.1038/s41586-024-07184-8

    2024 doi

  4. [12]

    E., & Ho, L

    Greene, J. E., & Ho, L. C. 2005, ApJ, 630, 122, doi: 10.1086/431897 —. 2007, ApJ, 667, 131, doi: 10.1086/520497

    2005 doi

  5. [13]

    E., Strader, J., & Ho, L

    Greene, J. E., Strader, J., & Ho, L. C. 2020, ARA&A, 58, 257, doi: 10.1146/annurev-astro-032620-021835

    2020 doi

  6. [14]

    E., Labbe, I., Goulding, A

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

    2024 doi

  7. [15]

    2023, ApJ, 959, 39, doi: 10.3847/1538-4357/ad029e

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

    2023 doi

  8. [16]

    L., & Erb, D

    Henry, A., Scarlata, C., Martin, C. L., & Erb, D. 2015, ApJ, 809, 19, doi: 10.1088/0004-637X/809/1/19

    2015 doi

  9. [17]

    C., & Kim, M

    Ho, L. C., & Kim, M. 2015, ApJ, 809, 123, doi: 10.1088/0004-637X/809/2/123

    2015 doi

  10. [18]

    I., et al

    Iani, E., Rinaldi, P., Caputi, K. I., et al. 2024, arXiv e-prints, arXiv:2406.18207, doi: 10.48550/arXiv.2406.18207

    2024 doi arXiv

  11. [19]

    I., Guseva, N

    Izotov, Y. I., Guseva, N. G., Fricke, K. J., & Henkel, C. 2015, MNRAS, 451, 2251, doi: 10.1093/mnras/stv1115

    2015 doi

  12. [20]

    I., Guseva, N

    Izotov, Y. I., Guseva, N. G., Fricke, K. J., et al. 2021a, A&A, 646, A138, doi: 10.1051/0004-6361/202039772

    doi

  13. [21]

    I., Guseva, N

    Izotov, Y. I., Guseva, N. G., & Thuan, T. X. 2011, ApJ, 728, 161, doi: 10.1088/0004-637X/728/2/161

    2011 doi

  14. [22]

    I., Orlitov´ a, I., Schaerer, D., et al

    Izotov, Y. I., Orlitov´ a, I., Schaerer, D., et al. 2016a, Nature, 529, 178, doi: 10.1038/nature16456

    doi

  15. [23]

    I., Schaerer, D., Thuan, T

    Izotov, Y. I., Schaerer, D., Thuan, T. X., et al. 2016b, MNRAS, 461, 3683, doi: 10.1093/mnras/stw1205

    doi

  16. [24]

    I., Schaerer, D., Worseck, G., et al

    Izotov, Y. I., Schaerer, D., Worseck, G., et al. 2018, MNRAS, 474, 4514, doi: 10.1093/mnras/stx3115

    2018 doi

  17. [25]

    I., Thuan, T

    Izotov, Y. I., Thuan, T. X., Guseva, N. G., et al. 2024, MNRAS, 527, 281, doi: 10.1093/mnras/stad3151

    2024 doi

  18. [26]

    I., Worseck, G., Schaerer, D., et al

    Izotov, Y. I., Worseck, G., Schaerer, D., et al. 2021b, MNRAS, 503, 1734, doi: 10.1093/mnras/stab612

    doi

  19. [27]

    H., Cohen, M., Masci, F., et al

    Jarrett, T. H., Cohen, M., Masci, F., et al. 2011, ApJ, 735, 112, doi: 10.1088/0004-637X/735/2/112

    2011 doi

  20. [28]

    2019, ApJ, 885, 96, doi: 10.3847/1538-4357/ab3d3b

    McKinney, J. 2019, ApJ, 885, 96, doi: 10.3847/1538-4357/ab3d3b

    2019 doi

  21. [29]

    M., Tremonti, C., et al

    Kauffmann, G., Heckman, T. M., Tremonti, C., et al. 2003, MNRAS, 346, 1055, doi: 10.1111/j.1365-2966.2003.07154.x

    2003

  22. [30]

    J., Dopita, M

    Kewley, L. J., Dopita, M. A., Sutherland, R. S., Heisler, C. A., & Trevena, J. 2001, ApJ, 556, 121, doi: 10.1086/321545

    2001 doi

  23. [31]

    J., Groves, B., Kauffmann, G., & Heckman, T

    Kewley, L. J., Groves, B., Kauffmann, G., & Heckman, T. 2006, MNRAS, 372, 961, doi: 10.1111/j.1365-2966.2006.10859.x

    2006

  24. [32]

    2020, ApJ, 893, 134, doi: 10.3847/1538-4357/ab7895

    Yang, H. 2020, ApJ, 893, 134, doi: 10.3847/1538-4357/ab7895

    2020 doi

  25. [33]

    D., Onoue, M., Inayoshi, K., et al

    Kocevski, D. D., Onoue, M., Inayoshi, K., et al. 2023, ApJL, 954, L4, doi: 10.3847/2041-8213/ace5a0

    2023 doi

  26. [34]

    D., Finkelstein, S

    Kocevski, D. D., Finkelstein, S. L., Barro, G., et al. 2024, arXiv e-prints, arXiv:2404.03576, doi: 10.48550/arXiv.2404.03576

    2024 doi arXiv

  27. [35]

    2023, ApJL, 957, L7, doi: 10.3847/2041-8213/ad037a

    Kokorev, V., Fujimoto, S., Labbe, I., et al. 2023, ApJL, 957, L7, doi: 10.3847/2041-8213/ad037a

    2023 doi

  28. [36]

    E., Bezanson, R., et al

    Labbe, I., Greene, J. E., Bezanson, R., et al. 2023, arXiv e-prints, arXiv:2306.07320, doi: 10.48550/arXiv.2306.07320

    2023 doi arXiv

  29. [37]

    2013, A&A, 553, A106, doi: 10.1051/0004-6361/201118370

    Leitet, E., Bergvall, N., Hayes, M., Linn´ e, S., & Zackrisson, E. 2013, A&A, 553, A106, doi: 10.1051/0004-6361/201118370

    2013 doi

  30. [38]

    C., & Oey, M

    Leitherer, C., Hernandez, S., Lee, J. C., & Oey, M. S. 2016, ApJ, 823, 64, doi: 10.3847/0004-637X/823/1/64

    2016 doi

  31. [39]

    2022, ApJ, 940, 35, doi: 10.3847/1538-4357/ac9232

    Lin, R., Zheng, Z.-Y., Hu, W., et al. 2022, ApJ, 940, 35, doi: 10.3847/1538-4357/ac9232

    2022 doi

  32. [40]

    2024, SCIENCE CHINA Physics, Mechanics & Astronomy, 67, 109811, doi: 10.1007/s11433-024-2412-3

    Lin, R., Zheng, Z.-Y., Yuan, F., et al. 2024, SCIENCE CHINA Physics, Mechanics & Astronomy, 67, 109811, doi: 10.1007/s11433-024-2412-3

    2024 doi

  33. [41]

    2023, arXiv e-prints, arXiv:2308.01230, doi: 10.48550/arXiv.2308.01230

    Maiolino, R., Scholtz, J., Curtis-Lake, E., et al. 2023, arXiv e-prints, arXiv:2308.01230, doi: 10.48550/arXiv.2308.01230

    2023 doi arXiv

  34. [42]

    2024, Nature, 627, 59, doi: 10.1038/s41586-024-07052-5

    Maiolino, R., Scholtz, J., Witstok, J., et al. 2024, Nature, 627, 59, doi: 10.1038/s41586-024-07052-5

    2024 doi

  35. [43]

    A., et al

    Matthee, J., Mackenzie, R., Simcoe, R. A., et al. 2023, ApJ, 950, 67, doi: 10.3847/1538-4357/acc846

    2023 doi

  36. [44]

    P., Brammer, G., et al

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

    2024 doi

  37. [45]

    J., & Dunlop, J

    McLure, R. J., & Dunlop, J. S. 2004, MNRAS, 352, 1390, doi: 10.1111/j.1365-2966.2004.08034.x

    2004

  38. [46]

    2017, International Journal of Modern Physics D, 26, 1730021, doi: 10.1142/S021827181730021X

    Mezcua, M. 2017, International Journal of Modern Physics D, 26, 1730021, doi: 10.1142/S021827181730021X

    2017 doi

  39. [47]

    2024, ApJL, 966, L30, doi: 10.3847/2041-8213/ad3c2a

    Mezcua, M., Pacucci, F., Suh, H., Siudek, M., & Natarajan, P. 2024, ApJL, 966, L30, doi: 10.3847/2041-8213/ad3c2a

    2024 doi

  40. [48]

    2023, ApJL, 943, L5, doi: 10.3847/2041-8213/acae25

    Mezcua, M., Siudek, M., Suh, H., et al. 2023, ApJL, 943, L5, doi: 10.3847/2041-8213/acae25

    2023 doi

  41. [49]

    2009, A&A, 507, 1793, doi: 10.1051/0004-6361/200912497

    Noll, S., Burgarella, D., Giovannoli, E., et al. 2009, A&A, 507, 1793, doi: 10.1051/0004-6361/200912497

    2009 doi

  42. [50]

    2023, ApJL, 957, L3, doi: 10.3847/2041-8213/ad0158

    Pacucci, F., Nguyen, B., Carniani, S., Maiolino, R., & Fan, X. 2023, ApJL, 957, L3, doi: 10.3847/2041-8213/ad0158

    2023 doi

  43. [51]

    E., Wold, I

    Rhoads, J. E., Wold, I. G. B., Harish, S., et al. 2023, ApJL, 942, L14, doi: 10.3847/2041-8213/acaaaf

    2023 doi

  44. [52]

    2022, A&A, 665, L4, doi: 10.1051/0004-6361/202244556

    Schaerer, D., Marques-Chaves, R., Barrufet, L., et al. 2022, A&A, 665, L4, doi: 10.1051/0004-6361/202244556

    2022 doi

  45. [53]

    A., Lyu, J., Rieke, G

    Stone, M. A., Lyu, J., Rieke, G. H., & Alberts, S. 2023, ApJ, 953, 180, doi: 10.3847/1538-4357/acebe0 11

    2023 doi

  46. [54]

    2023, ApJ, 953, 53, doi: 10.3847/1538-4357/acd53c ¨Ubler, H., Maiolino, R., Curtis-Lake, E., et al

    Sun, F., Egami, E., Pirzkal, N., et al. 2023, ApJ, 953, 53, doi: 10.3847/1538-4357/acd53c ¨Ubler, H., Maiolino, R., Curtis-Lake, E., et al. 2023, A&A, 677, A145, doi: 10.1051/0004-6361/202346137

    2023 doi

  47. [55]

    M., Leitherer, C., et al

    Wang, B., Heckman, T. M., Leitherer, C., et al. 2019, ApJ, 885, 57, doi: 10.3847/1538-4357/ab418f

    2019 doi

  48. [56]

    2024, Nature Astronomy, 8, 504, doi: 10.1038/s41550-024-02197-9

    Wang, L., Hu, M., Wang, L., et al. 2024, Nature Astronomy, 8, 504, doi: 10.1038/s41550-024-02197-9

    2024 doi

  49. [57]

    2023, ApJL, 958, L14, doi: 10.3847/2041-8213/ad01c0

    Withers, S., Muzzin, A., Ravindranath, S., et al. 2023, ApJL, 958, L14, doi: 10.3847/2041-8213/ad01c0

    2023 doi

  50. [58]

    Woo, J.-H., Yoon, Y., Park, S., Park, D., & Kim, S. C. 2015, ApJ, 801, 38, doi: 10.1088/0004-637X/801/1/38

    2015 doi

  51. [59]

    2016, ApJ, 820, 130, doi: 10.3847/0004-637X/820/2/130

    Yang, H., Malhotra, S., Gronke, M., et al. 2016, ApJ, 820, 130, doi: 10.3847/0004-637X/820/2/130

    2016 doi

  52. [60]

    2023, MNRAS, 519, 1618, doi: 10.1093/mnras/stac3477

    Yang, Y., Baade, D., Hoeflich, P., et al. 2023, MNRAS, 519, 1618, doi: 10.1093/mnras/stac3477

    2023 doi

  53. [61]

    A., et al

    Yue, M., Eilers, A.-C., Simcoe, R. A., et al. 2024, ApJ, 966, 176, doi: 10.3847/1538-4357/ad3914

    2024 doi

  54. [62]

    Zhang, Z., Jiang, L., Liu, W., & Ho, L. C. 2024, arXiv e-prints, arXiv:2411.02729, doi: 10.48550/arXiv.2411.02729

    2024 doi arXiv

  55. [63]

    Zhuang, M.-Y., & Ho, L. C. 2023, Nature Astronomy, 7, 1376, doi: 10.1038/s41550-023-02051-4

    2023 doi

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