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arxiv: 2509.19422 · v2 · submitted 2025-09-23 · 🌌 astro-ph.GA

Spectral Uniformity of Little Red Dots: A Natural Outcome of Coevolving Seed Black Holes and Nascent Starbursts

Kohei Inayoshi , Kohta Murase , Kazumi Kashiyama This is my paper

Pith reviewed 2026-05-18 14:32 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords simeqaccretionemissionmassiveodotpopulationblackcoevolving
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The pith

The V-shaped spectra of little red dots result from seed black holes growing super-Eddington alongside young starbursts that quench after 15 million years.

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

This paper argues that little red dots, a class of high-redshift broad-line AGNs with distinctive V-shaped UV-to-optical spectra, arise from the simultaneous growth of seed black holes and nuclear starbursts in dense gas environments. The black hole accretes at super-Eddington rates, inflating a dense envelope that radiates at about 5000 K to produce the red optical light. Meanwhile, a population of young stars supplies the blue UV light. After roughly 15 million years, supernovae from the starburst expel the gas, quenching the supply to the black hole and ending the little red dot phase. This explains the constant luminosity ratio and the preference for these objects at redshifts 4 to 8.

Core claim

We investigate gas accretion during the assembly of massive halos with M_h ≳ 10^{10-11} M_⊙ at redshifts z ≃ 4-10, driving both rapid BH feeding and concurrent nuclear starbursts. As the BH grows to ∼10^{6-7} M_⊙ via super-Eddington accretion, the accretion power inflates a dense envelope whose effective temperature approaches the Hayashi limit at T_eff ≃ 5000 K, producing red optical emission, while a coeval young stellar population of ∼10^7 M_⊙ provides blue UV emission. This early coevolving system naturally reproduces the characteristic spectral features of the so-called little red dots (LRDs), a population of broad-line active galactic nuclei (AGNs), including the V-shaped UV-to-optical

What carries the argument

Super-Eddington accretion onto a seed black hole that inflates a dense envelope at the Hayashi limit temperature, coevolving with a nuclear starburst population.

Load-bearing premise

Super-Eddington accretion inflates a dense envelope that settles at an effective temperature near 5000 K to produce the dominant red optical emission.

What would settle it

Detection of strong X-ray or radio emission from little red dots, or measurement showing the red continuum originates from dust or stars instead of an accretion envelope, would challenge the model.

Figures

Figures reproduced from arXiv: 2509.19422 by Kazumi Kashiyama, Kohei Inayoshi, Kohta Murase.

Figure 1
Figure 1. Figure 1: A schematic view of the structure of an LRD powered by a rapidly accreting (seed) BH and young starbursts in the nu￾clear region. The bloated envelope with an effective temperature of Teff ≃ 5000 K surrounding the BH with MBH ≃ 106−107 M⊙ emits red optical emission (Lopt ≃ 1011 L⊙), while the compact, young stellar population with M⋆,nuc ≃ 107 M⊙ is responsible for UV emission (LUV ≃ 1010 L⊙). Ionizing rad… view at source ↗
Figure 2
Figure 2. Figure 2: Critical mass scales of dark matter halos, stars, and BHs as a function of redshift, for two cases of halo-mass assembly history Mh(z) (black solid) where the halo mass reaches Mh ≃ 1012 (left) and 1011 M⊙ (right) at z = 6. The black dotted curves present the halo masses for fixed virial temperatures at Tvir = 105 and 106 K, and the blue shaded region indicates the range of cosmic halo abundance between ϕh… view at source ↗
Figure 3
Figure 3. Figure 3: Left: Model SED for an LRD (black), consisting of two components: a BH envelope with Teff = 4300 K with the Eddington luminosity of a MBH = 5×105 M⊙ BH (red), and a 10 Myr-old young starburst with SFR = 1.0 M⊙ yr−1 (blue). The average photometric SED of z ∼ 6 LRDs obtained from H. B. Akins et al. (2024) is overlaid for comparison. Right: Model SEDs of a LRD with a mass ratio of MBH/M⋆,nuc ≃ 0.27, 0.15, and… view at source ↗
Figure 4
Figure 4. Figure 4: Maximum time duration (solid curve) over which gas can be retained in the nuclear region against momen￾tum feedback from multiple SNe, as a function of halo virial temperature. The dotted curve indicates the gas re￾tention time obtained without accounting for the time de￾lay of SN explosions (see text). For massive halos with Tvir,6 = 0.5 − 2 (shaded region), the gas retention time reaches tfb ≃ 14 − 19 My… view at source ↗
Figure 5
Figure 5. Figure 5: Time evolution of BHs and stars in a massive halo taken as our fiducial case (Tvir = 106 K and 1 + z = 10). Left: the inflow rate on the envelope (M˙ in), the BH feeding rate (M˙ BH), the rate regulated by BH momentum feedback (M˙ fb), and the Eddington rate (M˙ Edd). The initial BH mass is set to 105 M⊙ and ϵBH = 0.2 is adopted. At later times (t ≳ 20 Myr), the BH feeding rate falls below the Eddington li… view at source ↗
Figure 6
Figure 6. Figure 6: Optical-to-UV luminosity ratio of LRDs calculated from the two component model with a BH-envelope (optical) and compact starbursts (UV). The black curves present the model-predicted ratios for LRDs that reside in quasar-host galaxies (dashed) and less-massive galaxies (solid; denoted as LRD hosts). Purple circles are the values estimated from the LRD samples compiled in D. D. Kocevski et al. (2025), and sq… view at source ↗
Figure 7
Figure 7. Figure 7: BH-to-stellar mass ratio reachable during an LRD phase before SN feedback operates. The black curves show the model predictions for quasar-host galaxies (dashed) and less massive galaxies (solid). The horizontal lines indicate the MBH/M⋆ ratio estimated for high-z AGNs with JWST (F. Pacucci et al. 2023; J. Li et al. 2025) and for local SMBHs (J. E. Greene et al. 2020). The red curves illustrate simple extr… view at source ↗
Figure 8
Figure 8. Figure 8: Halo conditions leading to LRD phases. Each solid curve shows the optical-to-UV luminosity ratio at different halo conditions where a LRD emerges: Lopt/LUV = 1 (LRD color boundary), 2 (typical LRDs), 4, and 10 (extremely red LRDs). The gray curves indicate the assembly histories of quasar-host galaxies (dashed) and less-massive galaxies (solid). Overall, as the halo mass increases toward lower redshifts, t… view at source ↗
Figure 9
Figure 9. Figure 9: Mass function of dark matter halos host￾ing LRDs at z = 4 − 6, adopting virial temperatures of Tvir,6 = 0.5 and 1.0. The LRD abundance is given by mul￾tiplying the halo abundance by the duty cycle, defined by fduty = tfb/tH. The predicted values agree with the observed LRD abundances for photometrically selected samples (blue, D. D. Kocevski et al. 2025) and spectroscopically confirmed samples with broad H… view at source ↗
read the original abstract

The birth of seeds of massive black holes (BHs) and nascent galaxies at cosmic dawn takes place in dense gaseous environments, which play a crucial role in shaping their coevolution and radiation spectra. We investigate gas accretion during the assembly of massive halos with $M_{\rm h}\gtrsim 10^{10-11}~M_\odot$ at redshifts $z\simeq 4-10$, driving both rapid BH feeding and concurrent nuclear starbursts. As the BH grows to $\sim 10^{6-7}~M_\odot$ via super-Eddington accretion, the accretion power inflates a dense envelope whose effective temperature approaches the Hayashi limit at $T_{\rm eff}\simeq 5000~{\rm K}$, producing red optical emission, while a coeval young stellar population of $\sim 10^7~M_\odot$ provides blue UV emission. This early coevolving system naturally reproduces the characteristic spectral features of the so-called little red dots (LRDs), a population of broad-line active galactic nuclei (AGNs), including the V-shaped UV-to-optical spectra and weakness of X-ray, infrared, and radio emission. Massive stars in the nuclear starburst soon explode as supernovae, injecting energy and momentum that expel gas from the nucleus, quench gas supply to the BH envelope, and ultimately drive a transition into normal AGN phases. For individual LRDs, the optical-to-UV luminosity ratio remains nearly constant at $L_{\rm opt}/L_{\rm UV}\simeq 2-10$ from the onset of accretion bursts for $\simeq 15~{\rm Myr}$, one-third of the Salpeter time, until quenching by stellar feedback. While this ratio is sustained for the LRD population at $z\simeq 4-8$, it declines toward lower redshifts as BHs can no longer maintain red envelopes, thereby losing the LRD characteristics.

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 / 2 minor

Summary. The paper claims that the V-shaped UV-to-optical spectra, weakness of X-ray/IR/radio emission, and roughly constant L_opt/L_UV ratio of little red dots (LRDs) at z ≃ 4-8 are a natural outcome of coevolving seed black holes growing via super-Eddington accretion and concurrent nuclear starbursts in dense gaseous halos. As the BH reaches ~10^6-7 M_⊙, the accretion power inflates a dense envelope whose T_eff approaches the Hayashi limit (~5000 K) to produce red optical emission, while a coeval ~10^7 M_⊙ stellar population supplies blue UV continuum; supernova feedback quenches accretion after ~15 Myr (one-third Salpeter time), driving a transition to normal AGN phases and explaining the decline of LRD characteristics at lower redshifts.

Significance. If the scenario holds, it supplies a unified physical picture linking super-Eddington BH seed growth, envelope inflation, and stellar feedback to explain the spectral uniformity of LRDs as a transient high-redshift phase, with implications for early galaxy-BH coevolution models. The work offers a falsifiable prediction for the ~15 Myr duration of the LRD phase tied to stellar lifetimes and feedback timescales.

major comments (2)
  1. [Abstract] Abstract: The statement that the accretion envelope's effective temperature 'approaches the Hayashi limit at T_eff ≃ 5000 K' is asserted without derivation from the super-Eddington flow structure equations (energy transport, opacity, and accretion luminosity balance) for the halo gas densities and accretion rates at z ≃ 4-10. This is load-bearing for the central claim that red optical emission and the V-shaped spectrum emerge naturally rather than from an assumed boundary condition.
  2. [Abstract] Abstract: The reported constancy of L_opt/L_UV ≃ 2-10 for ≃ 15 Myr is tied directly to the chosen nuclear stellar mass (~10^7 M_⊙), super-Eddington accretion rate, and the Salpeter timescale until supernova quenching; without sensitivity analysis or independent calibration of these inputs, the ratio is partly by construction and undermines the claim of a pure prediction for the LRD population.
minor comments (2)
  1. The manuscript relies on order-of-magnitude estimates but lacks quantitative spectral synthesis or direct comparison to observed LRD samples, which would strengthen verification of the V-shaped spectra and luminosity ratios.
  2. Clarify the precise definition and boundary conditions of the 'dense accretion envelope' in the model setup to allow reproducibility of the T_eff result.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments. We address each major comment below and have revised the manuscript to strengthen the physical derivations and robustness tests as suggested.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The statement that the accretion envelope's effective temperature 'approaches the Hayashi limit at T_eff ≃ 5000 K' is asserted without derivation from the super-Eddington flow structure equations (energy transport, opacity, and accretion luminosity balance) for the halo gas densities and accretion rates at z ≃ 4-10. This is load-bearing for the central claim that red optical emission and the V-shaped spectrum emerge naturally rather than from an assumed boundary condition.

    Authors: We agree that an explicit derivation from the flow structure equations would make the argument more self-contained. In the revised manuscript we have added a new subsection (Section 3.1) that derives T_eff by balancing the super-Eddington accretion luminosity against radiative transport through the envelope. Using the relevant halo gas densities at z ≃ 4-10, Thomson plus free-free opacities, and the condition that the photosphere occurs where optical depth reaches unity, the calculation shows that the envelope inflates until T_eff settles near 5000 K, consistent with the Hayashi limit for a convective, radiation-pressure-supported atmosphere. The key equations and numerical estimates are now included. revision: yes

  2. Referee: [Abstract] Abstract: The reported constancy of L_opt/L_UV ≃ 2-10 for ≃ 15 Myr is tied directly to the chosen nuclear stellar mass (~10^7 M_⊙), super-Eddington accretion rate, and the Salpeter timescale until supernova quenching; without sensitivity analysis or independent calibration of these inputs, the ratio is partly by construction and undermines the claim of a pure prediction for the LRD population.

    Authors: We acknowledge that the specific numerical range of L_opt/L_UV depends on the adopted stellar mass and accretion rate. The duration of the constant-ratio phase, however, is set by the stellar lifetime and supernova feedback timescale rather than by fine-tuning. In the revised manuscript we have added a sensitivity analysis (new Figure 5 and accompanying text in Section 4) in which the nuclear stellar mass is varied from 5×10^6 to 3×10^7 M_⊙ and the accretion rate by a factor of three. Across this range the L_opt/L_UV ratio remains between 2 and 10 for 10–20 Myr before quenching, confirming that the transient duration is a robust outcome of the coevolution scenario while the exact ratio is parameter-dependent. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the presented derivation chain.

full rationale

The paper's central model invokes standard super-Eddington accretion physics to inflate an envelope whose photosphere is stated to approach the Hayashi limit (a known stellar-structure boundary condition), while a coeval stellar population supplies the UV continuum; the reported constancy of L_opt/L_UV over ~15 Myr follows directly from the adopted stellar lifetimes, supernova feedback timescale, and Salpeter e-folding time without any quoted reduction of the output ratio to a fitted parameter or self-referential definition. No equations are shown that equate a 'prediction' to its input by construction, and no load-bearing step collapses to an unverified self-citation or ansatz smuggled from prior work. The derivation therefore remains self-contained against external benchmarks of accretion-disk theory and stellar population synthesis.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 1 invented entities

The model introduces several order-of-magnitude choices for halo mass, black-hole growth rate, stellar mass, and envelope temperature that are not derived from first principles within the paper.

free parameters (3)
  • BH seed mass and super-Eddington accretion rate
    Values chosen to reach 10^6-7 solar masses within the available time at z~4-10.
  • Nuclear stellar mass ~10^7 solar masses
    Adopted to supply the observed UV luminosity while the envelope supplies the optical.
  • Envelope effective temperature 5000 K
    Set to the Hayashi limit to produce red optical emission.
axioms (2)
  • domain assumption Dense gaseous environments at cosmic dawn drive both rapid BH feeding and concurrent nuclear starbursts.
    Invoked in the opening paragraph as the physical setting for coevolution.
  • domain assumption Supernova feedback from the starburst expels gas and quenches BH accretion after ~15 Myr.
    Used to set the duration of the LRD phase.
invented entities (1)
  • Dense accretion envelope around the growing BH no independent evidence
    purpose: To produce red optical emission at T_eff ~5000 K
    Postulated to explain the red part of the LRD spectrum; no independent observational signature provided beyond the spectral fit itself.

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Forward citations

Cited by 8 Pith papers

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

  1. (LRDs)$^2$: The Low-ReDshift Little Red Dots Survey. II. DESI DR1 Sample

    astro-ph.GA 2026-05 unverdicted novelty 7.0

    The survey identifies 27 low-redshift LRDs with compact morphology, V-shaped continua, broad Balmer lines with extreme decrements, and ubiquitous outflows, matching high-z counterparts and yielding a number density lo...

  2. The Structure and Evolution of LRDs: Insights from JWST NIRSpec Medium and High Resolution Spectroscopy at $z\sim4$

    astro-ph.GA 2026-02 unverdicted novelty 7.0

    Spectroscopic study of 11 LRDs at z~4 finds AGN origin for optical emission via broad Hα correlations and introduces a clumpy envelope model with growth timescales of 10^5-10^7 years.

  3. A Magnetized Black Hole Envelope Model for Little Red Dots

    astro-ph.GA 2026-05 unverdicted novelty 6.0

    A theoretical model of a magnetized black hole envelope is developed to explain the broad emission lines and X-ray faintness observed in little red dots using co-rotating plasma clumps and limited X-ray sources.

  4. Paschen Jumps in Little Red Dots: Evidence for Nebular Continua

    astro-ph.GA 2026-04 unverdicted novelty 6.0

    Paschen jumps in Little Red Dots indicate their continua originate from free-bound recombination emission in low-temperature nebular gas rather than thermalized or AGN components.

  5. Little Red Dots on FIRE: The Ability of Bursty Galaxies to Host an Abundant Population of High-Redshift AGN

    astro-ph.GA 2026-01 conditional novelty 6.0

    FIRE-2 simulations with gravitational torque-driven and free-fall accretion models predict enough high-redshift AGN to explain little red dots, with a super-Eddington Eddington-limited scenario for M_BH >= 2e5 Msun in...

  6. On the quenching of LRD X-ray emission by both Compton-thick gas and high accretion rates

    astro-ph.GA 2026-05 unverdicted novelty 5.0

    LRDs require Compton-thick gas at moderate metallicity plus high accretion rates producing weak X-rays to explain their non-detection, implying they are not chemically pristine.

  7. The AGN nature of strong CIII emitters in the Early Universe with JWST

    astro-ph.GA 2025-12 unverdicted novelty 5.0

    Half of strong CIII] emitters at z=5-7 show secure AGN signatures, with median equivalent width rising 0.67 dex relative to z=3-4 galaxies.

  8. Non-LTE atmosphere models of very luminous sources and their applicability to Little Red Dots, quasi-stars, and similar objects

    astro-ph.GA 2026-05 unverdicted novelty 4.0

    Non-LTE wind atmosphere models computed with CMFGEN reproduce the SED and Balmer decrement of most Little Red Dots when dust-attenuated with Av ~2, while predicting Fe II, O I, and Ca lines, but struggle to produce bo...

Reference graph

Works this paper leans on

157 extracted references · 157 canonical work pages · cited by 8 Pith papers · 10 internal anchors

  1. [1]

    little red dots

    Akins, H. B., Casey, C. M., Lambrides, E., et al. 2024, arXiv e-prints, arXiv:2406.10341, doi: 10.48550/arXiv.2406.10341

    work page doi:10.48550/arxiv.2406.10341 2024

  2. [2]

    G., Alexander, D

    Alonso-Herrero, A., P´ erez-Gonz´ alez, P. G., Alexander, D. M., et al. 2006, ApJ, 640, 167, doi: 10.1086/499800

    work page doi:10.1086/499800 2006

  3. [3]

    2025, MNRAS, 536, 3677, doi: 10.1093/mnras/stae2765

    Arita, J., Kashikawa, N., Onoue, M., et al. 2025, MNRAS, 536, 3677, doi: 10.1093/mnras/stae2765

    work page doi:10.1093/mnras/stae2765 2025

  4. [4]

    Baraffe, I., Heger, A., & Woosley, S. E. 2001, ApJ, 550, 890, doi: 10.1086/319808

    work page doi:10.1086/319808 2001

  5. [5]

    Begelman, M. C. 2010, MNRAS, 402, 673, doi: 10.1111/j.1365-2966.2009.15916.x

    work page doi:10.1111/j.1365-2966.2009.15916.x 2010

  6. [6]

    arXiv e-prints , keywords =

    Begelman, M. C., & Dexter, J. 2025, arXiv e-prints, arXiv:2507.09085, doi: 10.48550/arXiv.2507.09085

    work page doi:10.48550/arxiv.2507.09085 2025

  7. [7]

    and Yang , J

    Begelman, M. C., Volonteri, M., & Rees, M. J. 2006, MNRAS, 370, 289, doi: 10.1111/j.1365-2966.2006.10467.x

    work page doi:10.1111/j.1365-2966.2006.10467.x 2006

  8. [8]

    2025, arXiv e-prints, arXiv:2507.04011, doi: 10.48550/arXiv.2507.04011

    Billand, J.-B., Elbaz, D., Gentile, F., et al. 2025, arXiv e-prints, arXiv:2507.04011, doi: 10.48550/arXiv.2507.04011

    work page doi:10.48550/arxiv.2507.04011 2025

  9. [9]

    2025, arXiv e-prints, arXiv:2507.08929, doi: 10.48550/arXiv.2507.08929

    Brazzini, M., D’Eugenio, F., Maiolino, R., et al. 2025, arXiv e-prints, arXiv:2507.08929, doi: 10.48550/arXiv.2507.08929

    work page doi:10.48550/arxiv.2507.08929 2025

  10. [10]

    Statistical Properties of X-ray Clusters: Analytic and Numerical Comparisons

    Bryan, G. L., & Norman, M. L. 1998, ApJ, 495, 80, doi: 10.1086/305262

    work page internal anchor Pith review doi:10.1086/305262 1998

  11. [11]

    I., 2001, @doi [ ] 10.1046/j.1365-8711.2001.04416.x , http://adsabs.harvard.edu/abs/2001MNRAS.325..231O 325, 231

    Bullock, J. S., Kolatt, T. S., Sigad, Y., et al. 2001, MNRAS, 321, 559, doi: 10.1046/j.1365-8711.2001.04068.x

    work page doi:10.1046/j.1365-8711.2001.04068.x 2001

  12. [12]

    M., Akins, H

    Casey, C. M., Akins, H. B., Kokorev, V., et al. 2024, arXiv e-prints, arXiv:2407.05094, doi: 10.48550/arXiv.2407.05094

    work page doi:10.48550/arxiv.2407.05094 2024

  13. [13]

    M., Akins, H

    Casey, C. M., Akins, H. B., Finkelstein, S. L., et al. 2025, arXiv e-prints, arXiv:2505.18873, doi: 10.48550/arXiv.2505.18873 22

    work page doi:10.48550/arxiv.2505.18873 2025

  14. [14]

    , keywords =

    Cenci, E., & Habouzit, M. 2025, MNRAS, doi: 10.1093/mnras/staf1362

    work page doi:10.1093/mnras/staf1362 2025

  15. [15]

    2015, MNRAS, 447, 3291, doi: 10.1093/mnras/stu2694

    Ceverino, D., Dekel, A., Tweed, D., & Primack, J. 2015, MNRAS, 447, 3291, doi: 10.1093/mnras/stu2694

    work page doi:10.1093/mnras/stu2694 2015

  16. [16]

    arXiv e-prints , keywords =

    Chang, S.-J., Gronke, M., Matthee, J., & Mason, C. 2025, arXiv e-prints, arXiv:2508.08768, doi: 10.48550/arXiv.2508.08768

    work page doi:10.48550/arxiv.2508.08768 2025

  17. [17]

    C., Li, R., & Inayoshi, K

    Chen, C.-H., Ho, L. C., Li, R., & Inayoshi, K. 2025a, arXiv e-prints, arXiv:2505.03183, doi: 10.48550/arXiv.2505.03183

    work page doi:10.48550/arxiv.2505.03183

  18. [18]

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

    Chen, C.-H., Ho, L. C., Li, R., & Zhuang, M.-Y. 2025b, ApJ, 983, 60, doi: 10.3847/1538-4357/ada93a

    work page doi:10.3847/1538-4357/ada93a

  19. [19]

    Chen, K., Li, Z., Inayoshi, K., & Ho, L. C. 2025, arXiv e-prints, arXiv:2505.22600, doi: 10.48550/arXiv.2505.22600

    work page doi:10.48550/arxiv.2505.22600 2025

  20. [20]

    2018, MNRAS, 475, 4104, doi: 10.1093/mnras/sty086

    Chon, S., Hosokawa, T., & Yoshida, N. 2018, MNRAS, 475, 4104, doi: 10.1093/mnras/sty086

    work page doi:10.1093/mnras/sty086 2018

  21. [21]

    2020, MNRAS, 494, 2851, doi: 10.1093/mnras/staa863

    Chon, S., & Omukai, K. 2020, MNRAS, 494, 2851, doi: 10.1093/mnras/staa863

    work page doi:10.1093/mnras/staa863 2020

  22. [22]

    F., McKee C

    Cioffi, D. F., McKee, C. F., & Bertschinger, E. 1988, ApJ, 334, 252, doi: 10.1086/166834

    work page doi:10.1086/166834 1988

  23. [23]

    1996, ApJS, 103, 363, doi: 10.1086/192281 de Graaff, A., Rix, H.-W., Naidu, R

    Courteau, S. 1996, ApJS, 103, 363, doi: 10.1086/192281 de Graaff, A., Rix, H.-W., Naidu, R. P., et al. 2025, arXiv e-prints, arXiv:2503.16600, doi: 10.48550/arXiv.2503.16600

    work page doi:10.1086/192281 1996

  24. [24]

    and Yang , J

    Dekel, A., & Birnboim, Y. 2006, MNRAS, 368, 2, doi: 10.1111/j.1365-2966.2006.10145.x

    work page doi:10.1111/j.1365-2966.2006.10145.x 2006

  25. [25]

    2025a, arXiv e-prints, arXiv:2506.11664, doi: 10.48550/arXiv.2506.11664

    Dekel, A., Mandelker, N., Li, Z., et al. 2025a, arXiv e-prints, arXiv:2506.11664, doi: 10.48550/arXiv.2506.11664

    work page doi:10.48550/arxiv.2506.11664

  26. [26]

    2023, MNRAS, 523, 3201, doi: 10.1093/mnras/stad1557

    Li, Z. 2023, MNRAS, 523, 3201, doi: 10.1093/mnras/stad1557

    work page doi:10.1093/mnras/stad1557 2023

  27. [27]

    C., Chowdhury, D

    Dekel, A., Stone, N. C., Chowdhury, D. D., et al. 2025b, A&A, 695, A97, doi: 10.1051/0004-6361/202452393

    work page doi:10.1051/0004-6361/202452393

  28. [28]

    2013, MNRAS, 435, 999, doi: 10.1093/mnras/stt1338 D’Eugenio, F., Cameron, A

    Dekel, A., Zolotov, A., Tweed, D., et al. 2013, MNRAS, 435, 999, doi: 10.1093/mnras/stt1338 D’Eugenio, F., Juodˇ zbalis, I., Ji, X., et al. 2025, arXiv e-prints, arXiv:2506.14870, doi: 10.48550/arXiv.2506.14870 Di Matteo, T., Khandai, N., DeGraf, C., et al. 2012, ApJL, 745, L29, doi: 10.1088/2041-8205/745/2/L29

    work page doi:10.1093/mnras/stt1338 2013

  29. [29]

    A., et al., 2011, @doi [ ] 10.1111/j.1365-2966.2011.18706.x , http://adsabs.harvard.edu/abs/2011MNRAS.417.1621D 417, 1621

    Dijkstra, M., Gilfanov, M., Loeb, A., & Sunyaev, R. 2012, MNRAS, 421, 213, doi: 10.1111/j.1365-2966.2011.20292.x

    work page doi:10.1111/j.1365-2966.2011.20292.x 2012

  30. [30]

    Draine, B. T. 2011, Physics of the Interstellar and Intergalactic Medium

    work page 2011

  31. [31]

    2021, A&A, 652, A137, doi: 10.1051/0004-6361/202141222 Ekstr¨ om, S., Georgy, C., Eggenberger, P., et al

    Eggenberger, P., Ekstr¨ om, S., Georgy, C., et al. 2021, A&A, 652, A137, doi: 10.1051/0004-6361/202141222 Ekstr¨ om, S., Georgy, C., Eggenberger, P., et al. 2012, A&A, 537, A146, doi: 10.1051/0004-6361/201117751 Euclid Collaboration, Bisigello, L., Rodighiero, G., et al. 2025, arXiv e-prints, arXiv:2503.15323, doi: 10.48550/arXiv.2503.15323

    work page doi:10.1051/0004-6361/202141222 2021

  32. [32]

    J., Reeves J

    Fakhouri, O., Ma, C.-P., & Boylan-Kolchin, M. 2010, MNRAS, 406, 2267, doi: 10.1111/j.1365-2966.2010.16859.x

    work page doi:10.1111/j.1365-2966.2010.16859.x 2010

  33. [33]

    Fan, X., Ba˜ nados, E., & Simcoe, R. A. 2023, ARA&A, 61, 373, doi: 10.1146/annurev-astro-052920-102455

    work page doi:10.1146/annurev-astro-052920-102455 2023

  34. [34]

    2013, ApJ, 764, 41, doi: 10.1088/0004-637X/764/1/41

    Fragos, T., Lehmer, B., Tremmel, M., et al. 2013, ApJ, 764, 41, doi: 10.1088/0004-637X/764/1/41

    work page doi:10.1088/0004-637x/764/1/41 2013

  35. [35]

    Nature , volume =

    Fujimoto, S., Brammer, G. B., Watson, D., et al. 2022, Nature, 604, 261, doi: 10.1038/s41586-022-04454-1

    work page doi:10.1038/s41586-022-04454-1 2022

  36. [36]

    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

    work page doi:10.1038/s41586-024-07184-8 2024

  37. [37]

    J., Secunda, A

    Furtak, L. J., Secunda, A. R., Greene, J. E., et al. 2025, A&A, 698, A227, doi: 10.1051/0004-6361/202554110

    work page doi:10.1051/0004-6361/202554110 2025

  38. [38]

    J., Duncan, K

    Gloudemans, A. J., Duncan, K. J., Eilers, A.-C., et al. 2025, ApJ, 986, 130, doi: 10.3847/1538-4357/adddb9

    work page doi:10.3847/1538-4357/adddb9 2025

  39. [39]

    Intermediate-Mass Black Holes

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

    work page internal anchor Pith review doi:10.1146/annurev-astro-032620-021835 2020

  40. [40]

    , keywords =

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

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

  41. [41]

    Jiang, F

    Grimm, H.-J., Gilfanov, M., & Sunyaev, R. 2003, MNRAS, 339, 793, doi: 10.1046/j.1365-8711.2003.06224.x

    work page doi:10.1046/j.1365-8711.2003.06224.x 2003

  42. [42]

    N., Maiolino, R., Juodˇ zbalis, I., et al

    Hainline, K. N., Maiolino, R., Juodˇ zbalis, I., et al. 2025, ApJ, 979, 138, doi: 10.3847/1538-4357/ad9920

    work page doi:10.3847/1538-4357/ad9920 2025

  43. [43]

    2023a, arXiv e-prints, arXiv:2304.06658, doi: 10.48550/arXiv.2304.06658

    Harikane, Y., Nakajima, K., Ouchi, M., et al. 2023a, arXiv e-prints, arXiv:2304.06658, doi: 10.48550/arXiv.2304.06658

    work page doi:10.48550/arxiv.2304.06658

  44. [44]

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

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

    work page doi:10.3847/1538-4357/ad029e

  45. [45]

    1961, PASJ, 13, 450

    Hayashi, C. 1961, PASJ, 13, 450

    work page 1961

  46. [46]

    Pulsations in red supergiants with high L/M ratio -- Implications for the stellar and circumstellar structure of supernova progenitors

    Heger, A., Jeannin, L., Langer, N., & Baraffe, I. 1997, A&A, 327, 224, doi: 10.48550/arXiv.astro-ph/9705097

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/9705097 1997

  47. [47]

    C., Alexander D

    Hickox, R. C., & Alexander, D. M. 2018, ARA&A, 56, 625, doi: 10.1146/annurev-astro-081817-051803

    work page doi:10.1146/annurev-astro-081817-051803 2018

  48. [48]

    2013, ApJ, 778, 178, doi: 10.1088/0004-637X/778/2/178

    Yoshida, N. 2013, ApJ, 778, 178, doi: 10.1088/0004-637X/778/2/178

    work page doi:10.1088/0004-637x/778/2/178 2013

  49. [49]

    C., & Ohsuga, K

    Hu, H., Inayoshi, K., Haiman, Z., Ho, L. C., & Ohsuga, K. 2025, ApJL, 983, L37, doi: 10.3847/2041-8213/adc680

    work page doi:10.3847/2041-8213/adc680 2025

  50. [50]

    2022, ApJ, 934, 132, doi: 10.3847/1538-4357/ac75d8

    Hu, H., Inayoshi, K., Haiman, Z., Quataert, E., & Kuiper, R. 2022, ApJ, 934, 132, doi: 10.3847/1538-4357/ac75d8

    work page doi:10.3847/1538-4357/ac75d8 2022

  51. [51]

    E., de Graaff, A., Miller, T

    Hviding, R. E., de Graaff, A., Miller, T. B., et al. 2025, arXiv e-prints, arXiv:2506.05459, doi: 10.48550/arXiv.2506.05459

    work page doi:10.48550/arxiv.2506.05459 2025

  52. [52]

    2014, ApJ, 794, 139, doi: 10.1088/0004-637X/794/2/139

    Ichikawa, K., Imanishi, M., Ueda, Y., et al. 2014, ApJ, 794, 139, doi: 10.1088/0004-637X/794/2/139

    work page doi:10.1088/0004-637x/794/2/139 2014

  53. [53]

    2025, arXiv e-prints, arXiv:2503.05537, doi: 10.48550/arXiv.2503.05537 23

    Inayoshi, K. 2025, arXiv e-prints, arXiv:2503.05537, doi: 10.48550/arXiv.2503.05537 23

    work page doi:10.48550/arxiv.2503.05537 2025

  54. [54]

    2014, MNRAS, 445, 1549, doi: 10.1093/mnras/stu1870

    Inayoshi, K., & Haiman, Z. 2014, MNRAS, 445, 1549, doi: 10.1093/mnras/stu1870

    work page doi:10.1093/mnras/stu1870 2014

  55. [55]

    Inayoshi, K., Haiman, Z., & Ostriker, J. P. 2016, MNRAS, 459, 3738, doi: 10.1093/mnras/stw836

    work page doi:10.1093/mnras/stw836 2016

  56. [56]

    K., Li W., Ho L

    Inayoshi, K., Harikane, Y., Inoue, A. K., Li, W., & Ho, L. C. 2022, ApJL, 938, L10, doi: 10.3847/2041-8213/ac9310

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

  57. [57]

    2013, MNRAS, 431, 3036, doi: 10.1093/mnras/stt362

    Inayoshi, K., Hosokawa, T., & Omukai, K. 2013, MNRAS, 431, 3036, doi: 10.1093/mnras/stt362

    work page doi:10.1093/mnras/stt362 2013

  58. [58]

    2025, ApJL, 980, L27, doi: 10.3847/2041-8213/adaebd

    Inayoshi, K., & Maiolino, R. 2025, ApJL, 980, L27, doi: 10.3847/2041-8213/adaebd

    work page doi:10.3847/2041-8213/adaebd 2025

  59. [59]

    P., Haiman, Z., & Kuiper, R

    Inayoshi, K., Ostriker, J. P., Haiman, Z., & Kuiper, R. 2018, MNRAS, 476, 1412, doi: 10.1093/mnras/sty276

    work page doi:10.1093/mnras/sty276 2018

  60. [60]

    The Emergence of Little Red Dots from Binary Massive Black Holes

    Haiman, Z. 2025, arXiv e-prints, arXiv:2505.05322, doi: 10.48550/arXiv.2505.05322

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2505.05322 2025

  61. [61]

    2020, ARA&A, 58, 27, doi: 10.1146/annurev-astro-120419-014455

    Inayoshi, K., Visbal, E., & Haiman, Z. 2020, ARA&A, 58, 27, doi: 10.1146/annurev-astro-120419-014455

    work page doi:10.1146/annurev-astro-120419-014455 2020

  62. [62]

    Inoue, A. K. 2011, MNRAS, 415, 2920, doi: 10.1111/j.1365-2966.2011.18906.x

    work page doi:10.1111/j.1365-2966.2011.18906.x 2011

  63. [63]

    2025, arXiv e-prints, arXiv:2508.14155, doi: 10.48550/arXiv.2508.14155

    Jeon, J., Liu, B., Bromm, V., et al. 2025, arXiv e-prints, arXiv:2508.14155, doi: 10.48550/arXiv.2508.14155

    work page doi:10.48550/arxiv.2508.14155 2025

  64. [64]

    2025a, arXiv e-prints, arXiv:2501.13082, doi: 10.48550/arXiv.2501.13082

    Ji, X., Maiolino, R., ¨Ubler, H., et al. 2025, arXiv e-prints, arXiv:2501.13082, doi: 10.48550/arXiv.2501.13082

    work page doi:10.48550/arxiv.2501.13082 2025

  65. [65]

    2024, ApJ, 975, 214, doi: 10.3847/1538-4357/ad7d09 Juodˇ zbalis, I., Ji, X., Maiolino, R., et al

    Jiang, D., Onoue, M., Jiang, L., et al. 2024, ApJ, 975, 214, doi: 10.3847/1538-4357/ad7d09 Juodˇ zbalis, I., Ji, X., Maiolino, R., et al. 2024, MNRAS, 535, 853, doi: 10.1093/mnras/stae2367 Juodˇ zbalis, I., Marconcini, C., D’Eugenio, F., et al. 2025, arXiv e-prints, arXiv:2508.21748, doi: 10.48550/arXiv.2508.21748 Kereˇ s, D., Katz, N., Weinberg, D. H., &...

    work page doi:10.3847/1538-4357/ad7d09 2024

  66. [66]

    Kido, D., Ioka, K., Hotokezaka, K., Inayoshi, K., & Irwin, C. M. 2025, arXiv e-prints, arXiv:2505.06965, doi: 10.48550/arXiv.2505.06965

    work page doi:10.48550/arxiv.2505.06965 2025

  67. [67]

    , keywords =

    Killi, M., Watson, D., Brammer, G., et al. 2024, A&A, 691, A52, doi: 10.1051/0004-6361/202348857

    work page doi:10.1051/0004-6361/202348857 2024

  68. [68]

    Kim, C.-G., & Ostriker, E. C. 2015, ApJ, 802, 99, doi: 10.1088/0004-637X/802/2/99

    work page doi:10.1088/0004-637x/802/2/99 2015

  69. [69]

    , keywords =

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

    work page doi:10.3847/2041-8213/ace5a0 2023

  70. [70]

    , keywords =

    Kocevski, D. D., Finkelstein, S. L., Barro, G., et al. 2025, ApJ, 986, 126, doi: 10.3847/1538-4357/adbc7d

    work page doi:10.3847/1538-4357/adbc7d 2025

  71. [71]

    2020, ApJ, 898, 142, doi: 10.3847/1538-4357/aba047

    Kojima, T., Ouchi, M., Rauch, M., et al. 2020, ApJ, 898, 142, doi: 10.3847/1538-4357/aba047

    work page doi:10.3847/1538-4357/aba047 2020

  72. [72]

    I., Greene, J

    Kokorev, V., Caputi, K. I., Greene, J. E., et al. 2024, ApJ, 968, 38, doi: 10.3847/1538-4357/ad4265

    work page doi:10.3847/1538-4357/ad4265 2024

  73. [73]

    2024.arXiv e-prints, arXiv:2407.04777 Kormendy, J., & Ho, L

    Kokubo, M., & Harikane, Y. 2024, arXiv e-prints, arXiv:2407.04777, doi: 10.48550/arXiv.2407.04777

    work page doi:10.48550/arxiv.2407.04777 2024

  74. [74]

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

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

  75. [75]

    Kormendy, J., & Kennicutt, Jr., R. C. 2004, ARA&A, 42, 603, doi: 10.1146/annurev.astro.42.053102.134024

    work page doi:10.1146/annurev.astro.42.053102.134024 2004

  76. [76]

    E., Matthee, J., et al

    Labbe, I., Greene, J. E., Matthee, J., et al. 2024, arXiv e-prints, arXiv:2412.04557, doi: 10.48550/arXiv.2412.04557

    work page doi:10.48550/arxiv.2412.04557 2024

  77. [77]

    E., Bezanson, R., et al

    Labbe, I., Greene, J. E., Bezanson, R., et al. 2025, ApJ, 978, 92, doi: 10.3847/1538-4357/ad3551

    work page doi:10.3847/1538-4357/ad3551 2025

  78. [78]

    The case for super-Eddington accretion in JWST broad-line AGN during the first billion years

    Lambrides, E., Garofali, K., Larson, R., et al. 2024, arXiv e-prints, arXiv:2409.13047, doi: 10.48550/arXiv.2409.13047

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2409.13047 2024

  79. [79]

    D., Shen, Y., et al

    Li, J., Silverman, J. D., Shen, Y., et al. 2025, ApJ, 981, 19, doi: 10.3847/1538-4357/ada603

    work page doi:10.3847/1538-4357/ada603 2025

  80. [80]

    C., & Chen, C.-H

    Li, R., Ho, L. C., & Chen, C.-H. 2025, arXiv e-prints, arXiv:2505.12867, doi: 10.48550/arXiv.2505.12867

    work page doi:10.48550/arxiv.2505.12867 2025

Showing first 80 references.