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REVIEW 3 major objections 6 minor 285 references

Super-Eddington quasar feedback drives blow-outs that reshape the circumgalactic medium and produce extended Hα nebulae at z~6.

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2026-08-01 06:52 UTC pith:JUTX3TAA

load-bearing objection A solid, visually compelling simulation study linking extreme early black-hole growth to clumpy CGM and extended Hα nebulae at z~6, but the title's 'super-Eddington' driver is not actually isolated by the run design. the 3 major comments →

arxiv 2607.21719 v1 pith:JUTX3TAA submitted 2026-07-23 astro-ph.GA

Outflows in super-Eddington quasars drive clumpy circumgalactic medium and extended Hα nebulae at z gtrsim 6

Lucas Tortora , Tiago Costa , Debora Sijacki , Jake S. Bennett This is my paper
classification astro-ph.GA
keywords quasarssuper-Eddington accretionAGN feedbackcircumgalactic mediumH-alpha nebulaeradiative transferdamped Lyman-alpha systemshigh-redshift galaxies
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper argues that a super-Eddington accreting black hole at z~6, growing to over 10^10 solar masses, drives powerful outflows that fundamentally reshape the circumgalactic medium (CGM). The feedback clears escape channels, leaving the quasar unobscured, and ejects cold, fast, metal-enriched clumps that greatly increase the covering fraction of neutral hydrogen. Radiative transfer shows these clumps and filaments glow in Hα, forming extended nebulae whose size and brightness track feedback strength and drop when the nucleus is obscured. If true, Hα nebulae and HI absorption across the CGM become direct tracers of early black hole growth.

Core claim

The central claim is that sufficiently strong quasar feedback, produced by mildly super-Eddington accretion, triggers a 'blow-out' episode that transforms the host halo. The simulations show that repeated feedback cycles expel gas, leaving the central engine Compton-thin, while metal-enriched outflows cool and fragment into a population of cold, dense, neutral clumps that populate the halo out to and beyond the virial radius. As a result, the DLA covering fraction within 50 kpc rises by up to ~64 percent relative to the no-AGN case. Post-processing radiative transfer with a new Voronoi ray-tracing code shows that the same feedback imprints the CGM in Hα: when the quasar is unobscured, ionizi

What carries the argument

The arguments rest on three zoom-in cosmological simulations of the same massive protocluster halo: a no-AGN run, the fiducial FABLE model, and FABLE-sE, which seeds black holes in smaller haloes, allows accretion up to f_Edd=2, and reduces feedback coupling to 0.05 to assemble a 1.3e10 Msun black hole. The central diagnostic is the 'blow-out' episode, a ~200 Myr period during which cumulative AGN feedback expels gas from the nucleus and drives fast (v > 1000 km/s) cold outflows. The CGM's clumpy, outflowing neutral gas is quantified by the DLA covering fraction, and the radiative response is computed with VoroLite, a ray-tracing code that propagates quasar ionizing photons through the Voron

Load-bearing premise

The fable-sE run is a deliberately hand-tuned growth channel (earlier seeding, accretion cap f_Edd=2, feedback coupling 0.05) chosen to produce a 1.3e10 Msun black hole; if real billion-solar-mass black holes assemble by a different route, the predicted CGM transformation and nebular signatures may not apply.

What would settle it

A high-resolution re-simulation of the same halo (or any z~6 massive halo) that resolves sub-kpc multiphase gas and still shows no significant DLA covering enhancement or cold clump population after a super-Eddington phase would falsify the clump mechanism; observationally, an unobscured z~6 quasar with no extended Hα nebula beyond ~10 kpc despite a sustained ~1 Myr bright phase would contradict the predicted link between unobscuration and extended nebular emission.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Many z>6 quasars may be heavily obscured for most of their growth; unobscured blue quasars likely represent a brief post-blow-out phase, so their demographics can constrain AGN feedback strength.
  • The DLA covering fraction in quasar haloes is a transient, feedback-driven quantity: it can rise by ~64% during blow-out and then decline, so observations probing HI around quasars should see strong environmental evolution.
  • Hα nebular emission is a direct tracer of both obscuration stage and integrated feedback energy: extended nebulae (out to ~30 kpc) appear only after the central engine is unobscured.
  • Simulated Hα surface brightness radial profiles are consistent with current JWST NIRSpec observations of z~6 quasars (BEES sample), supporting the idea that observed quasars have undergone significant feedback.
  • The energy injection rate and outflow kinetic power decouple: outflows are set by cumulative energy injection over long times, not instantaneous quasar luminosity, so short-lived or variable quasars can still launch powerful outflows.

Where Pith is reading between the lines

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

  • If correct, Hα nebulae could be used as a 'fossil' record of past quasar activity: an extended nebula without an obvious central source might flag a recently unobscured quasar, linking nebular surveys to black hole growth histories.
  • The same blow-out mechanism implies that the escape of ionizing radiation (and hence quasar proximity zones and contribution to reionization) is regulated by feedback, not just gas supply; this may connect quasar lifetime estimates from proximity zones to feedback histories.
  • The prediction that cold neutral clumps are ejected to ~100 kpc suggests that some high-redshift DLA absorbers in quasar fields may be physically associated with outflows rather than cold accretion streams; future spectroscopy of DLA metallicities and kinematics could test this.
  • A testable extension: compare the Hα nebula morphology (clumpy vs smooth) between unobscured and obscured quasars at fixed luminosity; the model predicts that clumpiness arises specifically from the blow-out phase.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. This paper presents an analysis of three zoom-in cosmological simulations of a massive z~6 halo: NoAGN, fable (fiducial feedback), and fable-sE (modified BH seeding, mildly super-Eddington accretion cap f_Edd=2, and reduced feedback coupling ε_f=0.05). The central result is that fable-sE, which grows a 1.3×10^10 M_sun black hole, undergoes a strong 'blow-out' episode that drives metal-enriched, cold, fast neutral clumps into the CGM, enhancing the DLA covering fraction by up to ~64% relative to NoAGN. Using a new ray-tracing code VoroLite, the authors post-process the simulations with quasar radiation and predict Hα nebulae whose spatial extent and surface brightness increase as the central engine becomes unobscured, and compare these predictions to recent JWST observations of z~6 quasars.

Significance. If the causal chain posited in the title and abstract is correct, the paper provides a valuable theoretical framework for interpreting JWST observations of z>6 quasar environments: obscuration stages are tied to feedback-induced CGM transformations and to extended Hα nebulae. The paper's strengths include a detailed description of the ray-tracing methodology on a Voronoi mesh, explicit checks against different projection axes, and a transparent enumeration of caveats in Section 4.4. The authors also make falsifiable predictions for DLA covering fractions and Hα surface brightness profiles. However, the headline attribution of the effect specifically to super-Eddington accretion is not isolated in the run design, and several acknowledged simplifications are load-bearing for the quantitative observational claims.

major comments (3)
  1. [§2.1; Title/Abstract] The fable-sE run modifies three parameters simultaneously: seeding halo mass threshold (M_vir>10^9 h^-1 M_sun), Eddington cap (f_Edd=2), and feedback coupling (ε_f=0.05). The paper's title and abstract claim that 'super-Eddington quasars' drive the CGM transformation, but no run varies f_Edd while holding seeding and ε_f fixed. The observed blow-out, clump population, and DLA covering enhancement could in principle be caused by earlier seeding or lower ε_f. The authors' own statement in §2.1 that the simulations 'were not designed to correctly grow extremely massive SMBHs' underscores the exploratory nature. I request either an isolation run (or at least a parameter-decomposition study) or a reframing of the central claims to 'enhanced early black hole growth' with an explicit discussion of the degeneracy. This is load-bearing because the title, abstract, and conclusions (e.g., first bul
  2. [§2.3 and §4.4.4] The radiative transfer is performed in post-processing on fixed density and temperature fields, with no photo-heating or radiation-hydrodynamic response. The authors acknowledge this in §4.4.4, but the quantitative predictions of Hα size/luminosity in Figs. 11–13 and the comparison with BEES observations in Fig. 13 depend on the assumption that the gas distribution remains unchanged during the ~1 Myr quasar episode. Photo-heating can expand dense clumps and alter escape channels, so the inferred agreement with observations may be fortuitous. The paper would be strengthened by a simple test (e.g., a post-processing 'puffed' density model or a comparison with an on-the-fly RT run from the literature) to show that the qualitative trends are robust.
  3. [§3.4 and §4.4.3] The core new observable — the clumpy CGM and the associated ~64% DLA covering fraction enhancement (Fig. 9) — is likely resolution-sensitive. The authors note in §4.4.3 that limited resolution affects the formation, survival, and properties of gas clumps. Since only a single resolution is presented, it is unclear whether the predicted enhancement is a numerical artifact or a robust physical outcome. I ask for a convergence test or at least a more explicit statement in the conclusions that the quantitative covering fractions and Hα surface brightness values should be treated as lower/upper limits pending higher-resolution simulations.
minor comments (6)
  1. [§1] Typo: 'Mgiilines' should be 'Mg ii lines'.
  2. [§2.2 / Appendix A] The temperature iteration procedure for the neutral fraction is described in Appendix A, but it would help to state in the main text why this is important for the subsequent RT; currently the reader must infer it.
  3. [Fig. 13] The 'black shaded area' for BEES profiles is difficult to distinguish in the printed figure; consider using a distinctly labelled envelope or a legend entry.
  4. [§1; §5] The paper refers to the 'Aether project (Farina et al., 2026, in prep.)' without a reference; please add a citation or remove the specific project name if it is not in the reference list.
  5. [§3.2] The authors use 20000 sightlines for VoroLite and ~12000 for the grid-based method; the difference in numbers is not justified. A brief note on convergence with ray count would be useful.
  6. [§5] The conclusions contain strong population-level statements (e.g., 'demographics of unobscured/blue quasars...') based on a single halo. Please temper these or add a caveat that the results are a case study of one extreme protocluster environment.

Circularity Check

0 steps flagged

No circularity: the CGM blow-out, clump formation, DLA covering changes, and H-alpha nebulae are emergent outputs of the hydrodynamics/radiative-transfer chain, not restatements of the input parameter choices.

full rationale

No circular step is present. The paper's chain is: (i) take the Bennett et al. (2024) fable/fable-sE zoom-in runs; (ii) let AGN feedback act hydrodynamically; (iii) post-process fixed snapshots with VoroLite to solve Eq. (7) for the ionization state and then compute H-alpha emissivity via Eq. (6). The clumpy CGM, cold outflowing clumps, blow-out episodes, and the time-dependent DLA covering fraction (Fig. 9) are diagnosed from the simulated gas distribution; they are not imposed by the adopted f_Edd=2, seeding threshold, or eps_f=0.05. Likewise, the H-alpha radial profiles (Fig. 13) are obtained by ray-tracing through the simulated density field with a specified Q_Hi, so their extent and brightness depend on the gas geometry and escape channels, not merely on the input feedback parameters. The main legitimate concern is identification rather than circularity: Section 2.1 changes three things at once in fable-sE (earlier seeding, f_Edd=2, eps_f=0.05), so attributing the transformation specifically to super-Eddington accretion is underdetermined. But underdetermination is a confound/correctness caveat, not a reduction of the prediction to its input; no equation equates H-alpha size or covering fraction to f_Edd or eps_f. The self-citation to Bennett et al. (2024) supplies the simulation suite and BH growth history, but the present paper re-analyzes the actual simulation outputs rather than invoking a self-cited uniqueness theorem, and the radiative-transfer code is independently applied. The paper also explicitly frames results as relative trends and lists limitations in Sections 2.3 and 4.4 (post-processing, fixed gas density, unresolved ISM, no on-the-fly radiation), further confirming that the claims are emergent simulation findings rather than definitions or fitted predictions.

Axiom & Free-Parameter Ledger

9 free parameters · 7 axioms · 1 invented entities

The central claim rests on a chain of modeling choices: the FABLE subgrid model, the hand-tuned fable-sE black-hole parameters, the assumed UV background and SED, and post-processing radiative transfer with fixed gas. None of these are independently verified at z∼6 in this paper, and the absolute Hα predictions inherit uncertainty from each link.

free parameters (9)
  • Black hole seeding mass threshold (fable-sE) = 10^9 h^-1 M_sun (vs 5×10^10 in fiducial)
    Chosen to promote earlier seed formation and enable the 1.3×10^10 M_sun black hole; directly shapes the feedback history and thus the CGM response.
  • Eddington cap f_Edd = 2
    Allows mildly super-Eddington accretion, the central growth mechanism whose consequences the paper studies.
  • Quasar-mode feedback coupling ε_f (fable-sE) = 0.05
    Reduced from 0.1 to encourage early accretion; the paper notes stronger feedback results despite lower coupling, but the value is tuned to produce the extreme object.
  • Bondi accretion boost factor α = 100
    Standard FABLE subgrid parameter; controls BH feeding rates and hence feedback strength.
  • Radiative efficiency ε_r = 0.1
    Assumed to convert accretion rate into quasar luminosity; sets the energy input scale for all radiative and mechanical feedback.
  • Radio-mode mechanical heating efficiency ε_m = 0.8
    Standard FABLE parameter; subdominant in the quasar-mode-dominated phases studied here but part of the model.
  • ISM temperature floor for star-forming gas = 10^4 K
    Manually imposed because the effective equation of state does not yield a physical temperature; strongly affects the neutral fraction and Hα emissivity of the dense clumps.
  • Dust-to-metal mass fraction in cold gas = 15 per cent
    Assumed to estimate Hα attenuation through a foreground dust screen; authors call it a pessimistic worst-case choice.
  • Median H-ionizing cross-section <σ_HI> = 2.126×10^-18 cm^2
    Chosen for consistency across SEDs after finding the results are insensitive to it.
axioms (7)
  • domain assumption FABLE/Illustris subgrid prescriptions for cooling, star formation, and stellar feedback are a valid description of the unresolved ISM at z∼6.
    The simulations inherit the FABLE model; the paper explicitly notes in §4.4.1 that the effective equation of state is a serious limitation.
  • ad hoc to paper The fable-sE modifications (earlier seeding, f_Edd=2, ε_f=0.05) represent a plausible route to billion-solar-mass black holes at z∼6.
    The authors state these runs were not designed to 'correctly' grow extreme SMBHs but to offer a plausible pathway; the entire CGM/Hα prediction hinges on this plausibility.
  • domain assumption A homogeneous, redshift-dependent UVB (Puchwein et al. 2019) with the Rahmati et al. (2013) self-shielding fitting function describes the pre-quasar ionization state.
    Used to set initial neutral fractions before the quasar RT; stellar radiation from the host is neglected.
  • domain assumption Case B recombination and the adopted Hα emissivity formula correctly convert the ionized gas distribution into Hα luminosity.
    Standard nebular approximation, but ignores dust within the RT and any contribution from collisional excitation in shocked gas.
  • domain assumption The qsosed SED (Kubota & Done 2018), with bolometric-correction interpolation, gives the correct ionizing photon rate for these super-Eddington black holes.
    The authors test the Trinca et al. (2026) SED and find 64–70 per cent of the luminosity, so the absolute Hα brightness depends on this choice.
  • ad hoc to paper Post-processing the radiative transfer on fixed gas density and temperature fields captures the observable Hα morphology.
    Explicitly acknowledged in §4.4.4: photo-heating and hydrodynamic response are neglected, so the gas does not react to the radiation.
  • domain assumption Dust attenuation can be approximated by a foreground dust screen with a fixed dust-to-metal ratio.
    Used for the Hα surface-brightness profiles in Fig. 13; no dust is tracked self-consistently in the simulations or the RT.
invented entities (1)
  • VoroLite no independent evidence
    purpose: Ray-tracing radiative transfer code on Voronoi meshes; it is a software tool, not a physical entity.
    No new physical degrees of freedom are postulated. VoroLite is introduced as a methodological contribution but is not released.

pith-pipeline@v1.3.0-alltime-deepseek · 37896 in / 11025 out tokens · 105143 ms · 2026-08-01T06:52:30.491680+00:00 · methodology

0 comments
read the original abstract

The discovery of gargantuan black holes with masses exceeding a billion solar masses at $z\gtrsim6$ suggests rapid black hole growth and significant energy input into their host galaxies in the early Universe. With JWST probing previously unseen phases of the interstellar (ISM) and circumgalactic (CGM) medium around $z > 6$ quasars, detailed theoretical studies can now be directly confronted with observations. We use zoom-in simulations of a massive protocluster at $z\sim6$, employing both the fiducial FABLE galaxy formation model and modifications that allow earlier black hole seeding and mildly super-Eddington accretion. The central quasar remains Compton-thick throughout most of its evolution, with the obscuration arising from the ISM of its compact host galaxy. The onset of sufficiently strong quasar feedback drives a 'blow-out' episode, clearing out escape channels for ionizing radiation and leaving the central engine unobscured. This leads to a complete transformation of the CGM, whereby powerful, metal-enriched outflows produce a population of cold, fast, neutral clumps, significantly increasing the covering fraction of neutral hydrogen in the host halo. Radiative transfer calculations performed with a new ray-tracing code show that the CGM responds to quasar activity through the formation of H$\alpha$ nebulae, whose size and luminosity increase with the strength of quasar feedback and decrease with obscuration level. Enhanced early black hole growth thus fundamentally reshapes the ISM and CGM of $z\sim6$ quasars, leaving clear observable signatures in their obscuration, neutral hydrogen distribution, and extended H$\alpha$ emission.

Figures

Figures reproduced from arXiv: 2607.21719 by Debora Sijacki, Jake S. Bennett, Lucas Tortora, Tiago Costa.

Figure 1
Figure 1. Figure 1: Overview of the suite of simulations used in this work. From the bottom left, clockwise: panels A (fable-sE), B (NoAGN) and C (fable) show the metallicity-weighted gas density of the central halo hosting the quasar in each simulation at redshift 𝑧 = 6. The field-of-view in every panel covers 200 kpc × 200 kpc with a projection width of 200 kpc, and the white circle shows the virial radius 𝑅vir ≈ 80 kpc. Th… view at source ↗
Figure 2
Figure 2. Figure 2: Upper panel: Median hydrogen column density (𝑁H) along various sightlines covering a sphere of radius 5 kpc centred on the black hole for redshifts 𝑧 ∈ [5.75 − 7.8] for the simulations used in this work. Dashed lines with square markers highlight results obtained from a simplified approximation adopted in Bennett et al. 2024 (B24), see main text for details. Solid lines with point markers show results from… view at source ↗
Figure 3
Figure 3. Figure 3: Upper panel: Hydrogen column density around the central black hole for the fable-sE run obtained with VoroLite (as in [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Outflowing gas mass as a function of redshift for each simulation used in this work. All gas within a sphere of radius 3 𝑅vir centred on the SMBH and radial velocity 𝑣rad ≥ 300 km s−1 is considered here. Hot (𝑇 ≥ 106 K) gas is indicated by solid lines, while cold (𝑇 ≤ 5 × 104 K + star-forming) gas is indicated by dashed lines. In the fable-sE run, there is generally more outflowing gas at all times than in… view at source ↗
Figure 5
Figure 5. Figure 5: Outflowing gas mass per radial velocity bin within a sphere of varying radius 𝑅max centred on the SMBH at redshift 𝑧 = 6.01. Each panel shows results, from left to right, for the NoAGN, fable and fable-sE simulations. Hot (cold) gas is shown by the reddish (bluish) line histograms; the dotted, dashed and continuous lines indicate 𝑅max / 𝑅vir = 0.2, 1, 3, respectively. Gas in the fable-sE run is consistentl… view at source ↗
Figure 6
Figure 6. Figure 6: Outflowing gas mass per radial velocity bin within a sphere of radius 3 𝑅vir centred on the black hole. The left, middle and right columns correspond to results for the NoAGN, fable and fable-sE run, respectively, while the rows show histograms for redshifts 𝑧 = 8, 7.5, 7, 6.5, 6 and 5.75, from top to bottom (as also indicated on the right-hand side of every row). Hot (cold) gas is displayed with empty (fi… view at source ↗
Figure 7
Figure 7. Figure 7: Density-weighted projected pressure ratio 𝑓𝑃 = (𝑃ram − 𝑃thermal) / (𝑃ram + 𝑃thermal) for varying redshift (rows) for the NoAGN (left column), fable (middle column) and fable-sE (right column) simulation. Red-orange (blue-cyan) hues indicate regions where ram (thermal) pressure dominates. Prior to the blow-out phase in the fable-sE run (𝑧 ≳ 7), the CGM in all three simulations is similar, with gas being in … view at source ↗
Figure 8
Figure 8. Figure 8: Visual overview of the ionization state of the CGM in the suite of simulations at 𝑧 = 6.01. Here, gas is assumed to be in ionization equilibrium with a meta-galactic UVB. From left to right, the different columns show results for the NoAGN, fable and fable-sE simulations, respectively. The upper row displays the density-weighted neutral hydrogen fraction (𝑥H i), while the lower row shows 2D bivariate proje… view at source ↗
Figure 9
Figure 9. Figure 9: Difference in the H i covering fraction within 50 kpc between the NoAGN run and the fable and fable-sE runs versus cumulative feedback energy injected by the black hole in quasar mode. We adopt the threshold for DLA systems (𝑁H i > 1020.3 cm−2 ) for the covering fraction. For the abscissa, we compute the difference in cumulative energy injected by the accreting black hole into its surroundings, using the v… view at source ↗
Figure 10
Figure 10. Figure 10: Kinetic energy outflow rate of hot, outflowing gas 𝐸¤ kin, hot versus kinetic feedback energy from the AGN in quasar mode feedback 𝐸¤ FB, quasar mode. The coloured lines show tracks through time as encoded in the legend (lighter colours indicate earlier times/higher redshift, starting at 𝑧 = 7.5), and we use markers to match specific snapshots across the simula￾tions (as in [PITH_FULL_IMAGE:figures/full_… view at source ↗
Figure 11
Figure 11. Figure 11: Visual overview of the ionization state of the CGM of the NoAGN (left column), fable (middle column) and fable-sE (right column) runs at 𝑧 = 6.01 after a quasar event with a lifetime of around 1 Myr. The constant rate of ionizing photons is chosen to be 𝑄H i = 1057 s −1 for all simulations. We show the density-weighted neutral hydrogen fraction (𝑥H i , upper row), the neutral hydrogen column density (𝑁H i… view at source ↗
Figure 12
Figure 12. Figure 12: Visual overview of the ionization state of the CGM of the fable-sE simulation at 𝑧 = 7.59 (top row), 𝑧 = 6.66 (middle row) and 𝑧 = 5.75 (lower row) after a quasar event with a lifetime of around 1 Myr. The redshifts are chosen to correspond to three obscuration stages of the central engine, respectively, ‘obscured’, ‘in transition’ and ‘unobscured’ as highlighted in [PITH_FULL_IMAGE:figures/full_fig_p017… view at source ↗
Figure 13
Figure 13. Figure 13: Radial profiles of H𝛼 surface brightness for the three distinct obscuration stages in the fable-sE run: obscured (left panel), in transition (middle panel) and unobscured (right panel). The different line styles show profiles obtained for three orthogonal lines of sight (arbitrarily chosen along the ‘x’, ‘y’, and ‘z’ directions of the simulation volume). The thick lines display the intrinsic emission, whi… view at source ↗

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Reference graph

Works this paper leans on

285 extracted references · 6 canonical work pages · 1 internal anchor

  1. [1]

    The Physics and Evolution of Active Galactic Nuclei

  2. [2]

    The large-scale structure of the universe

  3. [3]

    LeVeque, Randall J. , year=. Finite Volume Methods for Hyperbolic Problems , publisher=

  4. [4]

    ARAA , keywords =

    Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies. ARAA , keywords =. doi:10.1146/annurev-astro-082708-101811 , archivePrefix =. 1304.7762 , primaryClass =

    Pith/arXiv arXiv

  5. [6]

    , keywords =

    RADAMESH: cosmological radiative transfer for Adaptive Mesh Refinement simulations. , keywords =. doi:10.1111/j.1365-2966.2010.17799.x , archivePrefix =. 1009.1625 , primaryClass =

    arXiv 2010

  6. [7]

    submitted to A&A , keywords =

    The hydrodynamical response of cold circumgalactic clouds to quasar radiation. submitted to A&A , keywords =

  7. [9]

    , keywords =

    C ^ 2 -ray: A new method for photon-conserving transport of ionizing radiation. , keywords =. doi:10.1016/j.newast.2005.09.004 , archivePrefix =. astro-ph/0508416 , primaryClass =

    Pith/arXiv arXiv 2005

  8. [10]

    , keywords =

    Equation of state of the photoionized intergalactic medium. , keywords =. doi:10.1093/mnras/292.1.27 , archivePrefix =. astro-ph/9612232 , primaryClass =

    Pith/arXiv arXiv

  9. [11]

    , keywords =

    Using 3D Voronoi grids in radiative transfer simulations. , keywords =. doi:10.1051/0004-6361/201322281 , archivePrefix =. 1310.1854 , primaryClass =

    Pith/arXiv arXiv

  10. [12]

    MNRAS , keywords =

    Core condensation in heavy halos: a two-stage theory for galaxy formation and clustering. MNRAS , keywords =. doi:10.1093/mnras/183.3.341 , adsurl =

    doi:10.1093/mnras/183.3.341

  11. [13]

    ApJ , keywords =

    Galaxy Formation through Hierarchical Clustering. ApJ , keywords =. doi:10.1086/170483 , adsurl =

    doi:10.1086/170483

  12. [14]

    ARAA , keywords =

    The Connection Between Galaxies and Their Dark Matter Halos. ARAA , keywords =. doi:10.1146/annurev-astro-081817-051756 , archivePrefix =. 1804.03097 , primaryClass =

    Pith/arXiv arXiv

  13. [15]

    AJ , keywords =

    The Demography of Massive Dark Objects in Galaxy Centers. AJ , keywords =. doi:10.1086/300353 , archivePrefix =. astro-ph/9708072 , primaryClass =

    Pith/arXiv arXiv

  14. [16]

    MNRAS , keywords =

    The growth of the gargantuan black holes powering high-redshift quasars and their impact on the formation of early galaxies and protoclusters. MNRAS , keywords =. doi:10.1093/mnras/stad3179 , archivePrefix =. 2305.11932 , primaryClass =

    Pith/arXiv arXiv

  15. [17]

    ApJ , keywords =

    Relations between Central Black Hole Mass and Total Galaxy Stellar Mass in the Local Universe. ApJ , keywords =. doi:10.1088/0004-637X/813/2/82 , archivePrefix =. 1508.06274 , primaryClass =

    Pith/arXiv arXiv

  16. [18]

    Monthly Notices of the Royal Astronomical Society , author=

    A physical model of the broad-band continuum of AGN and its implications for the UV/X relation and optical variability , volume=. Monthly Notices of the Royal Astronomical Society , author=. 2018 , month=oct, pages=. doi:10.1093/mnras/sty1890 , number=

    doi:10.1093/mnras/sty1890 2018

  17. [19]

    Monthly Notices of the Royal Astronomical Society , author=

    Modelling the spectral energy distribution of super-Eddington quasars , volume=. Monthly Notices of the Royal Astronomical Society , author=. 2019 , month=oct, pages=. doi:10.1093/mnras/stz2140 , note=

    doi:10.1093/mnras/stz2140 2019

  18. [20]

    2025 , month =

    Weakness of X-rays and variability in high-redshift active galactic nuclei with super-Eddington accretion , journal =. 2025 , month =. doi:10.1093/pasj/psaf050 , url =

    doi:10.1093/pasj/psaf050 2025

  19. [21]

    MNRAS , keywords =

    The H I covering fraction of Lyman Limit Systems in FIRE haloes. MNRAS , keywords =. doi:10.1093/mnras/stae1738 , archivePrefix =. 2311.18000 , primaryClass =

    Pith/arXiv arXiv

  20. [22]

    MNRAS , keywords =

    FIREbox: simulating galaxies at high dynamic range in a cosmological volume. MNRAS , keywords =. doi:10.1093/mnras/stad1205 , archivePrefix =. 2205.15325 , primaryClass =

    Pith/arXiv arXiv

  21. [24]

    AJ , keywords =

    A numerical approach to the testing of the fission hypothesis. AJ , keywords =. doi:10.1086/112164 , adsurl =

    doi:10.1086/112164

  22. [25]

    MNRAS , keywords =

    Smoothed particle hydrodynamics: theory and application to non-spherical stars. MNRAS , keywords =. doi:10.1093/mnras/181.3.375 , adsurl =

    doi:10.1093/mnras/181.3.375

  23. [26]

    ARAA , keywords =

    Smoothed particle hydrodynamics. ARAA , keywords =. doi:10.1146/annurev.aa.30.090192.002551 , adsurl =

    arXiv

  24. [27]

    ZEUS-2D: A Radiation Magnetohydrodynamics Code for Astrophysical Flows in Two Space Dimensions. I. The Hydrodynamic Algorithms and Tests. ApJs , keywords =. doi:10.1086/191680 , adsurl =

    doi:10.1086/191680

  25. [28]

    Journal of Computational Physics , keywords =

    Local Adaptive Mesh Refinement for Shock Hydrodynamics. Journal of Computational Physics , keywords =. doi:10.1016/0021-9991(89)90035-1 , adsurl =

    doi:10.1016/0021-9991(89)90035-1

  26. [29]

    Journal of Computational Physics , year = 1984, month = mar, volume =

    Adaptive Mesh Refinement for Hyperbolic Partial Differential Equations. Journal of Computational Physics , year = 1984, month = mar, volume =. doi:10.1016/0021-9991(84)90073-1 , adsurl =

    doi:10.1016/0021-9991(84)90073-1 1984

  27. [30]

    MNRAS , keywords =

    The FABLE simulations: a feedback model for galaxies, groups, and clusters. MNRAS , keywords =. doi:10.1093/mnras/sty1780 , archivePrefix =. 1804.05064 , primaryClass =

    Pith/arXiv arXiv

  28. [31]

    MNRAS , keywords =

    A model for cosmological simulations of galaxy formation physics. MNRAS , keywords =. doi:10.1093/mnras/stt1789 , archivePrefix =. 1305.2913 , primaryClass =

    Pith/arXiv arXiv

  29. [32]

    , keywords =

    Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe. , keywords =. doi:10.1093/mnras/stu1536 , archivePrefix =. 1405.2921 , primaryClass =

    Pith/arXiv arXiv

  30. [33]

    MNRAS , keywords =

    A model for cosmological simulations of galaxy formation physics: multi-epoch validation. MNRAS , keywords =. doi:10.1093/mnras/stt2295 , archivePrefix =. 1305.4931 , primaryClass =

    Pith/arXiv arXiv

  31. [34]

    MNRAS , keywords =

    Introducing the Illustris project: the evolution of galaxy populations across cosmic time. MNRAS , keywords =. doi:10.1093/mnras/stu1654 , archivePrefix =. 1405.3749 , primaryClass =

    Pith/arXiv arXiv

  32. [35]

    MNRAS , keywords =

    The Illustris simulation: the evolving population of black holes across cosmic time. MNRAS , keywords =. doi:10.1093/mnras/stv1340 , archivePrefix =. 1408.6842 , primaryClass =

    Pith/arXiv arXiv

  33. [36]

    MNRAS , keywords =

    Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation. MNRAS , keywords =. doi:10.1046/j.1365-8711.2003.06206.x , archivePrefix =. astro-ph/0206393 , primaryClass =

    arXiv 2003

  34. [37]

    Nature , keywords =

    Simulations of the formation, evolution and clustering of galaxies and quasars. Nature , keywords =. doi:10.1038/nature03597 , archivePrefix =. astro-ph/0504097 , primaryClass =

    Pith/arXiv arXiv

  35. [39]

    ApJs , keywords =

    Cosmological Simulations with TreeSPH. ApJs , keywords =. doi:10.1086/192305 , archivePrefix =. astro-ph/9509107 , primaryClass =

    Pith/arXiv arXiv

  36. [40]

    MNRAS , keywords =

    The effect of photoionization on the cooling rates of enriched, astrophysical plasmas. MNRAS , keywords =. doi:10.1111/j.1365-2966.2008.14191.x , archivePrefix =. 0807.3748 , primaryClass =

    arXiv 2008

  37. [42]

    Nature , keywords =

    Energy input from quasars regulates the growth and activity of black holes and their host galaxies. Nature , keywords =. doi:10.1038/nature03335 , archivePrefix =. astro-ph/0502199 , primaryClass =

    Pith/arXiv arXiv

  38. [44]

    ApJ , keywords =

    The evolution of large-scale structure in a universe dominated by cold dark matter. ApJ , keywords =. doi:10.1086/163168 , adsurl =

    doi:10.1086/163168

  39. [48]

    , keywords =

    Premature supermassive black hole mergers in cosmological simulations of structure formation. , keywords =. doi:10.1093/mnras/staf1336 , archivePrefix =. 2504.17549 , primaryClass =

    Pith/arXiv arXiv

  40. [49]

    MNRAS , keywords =

    Galaxies on FIRE (Feedback In Realistic Environments): stellar feedback explains cosmologically inefficient star formation. MNRAS , keywords =. doi:10.1093/mnras/stu1738 , archivePrefix =. 1311.2073 , primaryClass =

    Pith/arXiv arXiv 2073

  41. [50]

    MNRAS , keywords =

    Simulating galaxy formation with the IllustrisTNG model. MNRAS , keywords =. doi:10.1093/mnras/stx2656 , archivePrefix =. 1703.02970 , primaryClass =

    Pith/arXiv arXiv

  42. [51]

    MNRAS , keywords =

    The EAGLE project: simulating the evolution and assembly of galaxies and their environments. MNRAS , keywords =. doi:10.1093/mnras/stu2058 , archivePrefix =. 1407.7040 , primaryClass =

    Pith/arXiv arXiv

  43. [52]

    MNRAS , keywords =

    SIMBA: Cosmological simulations with black hole growth and feedback. MNRAS , keywords =. doi:10.1093/mnras/stz937 , archivePrefix =. 1901.10203 , primaryClass =

    Pith/arXiv arXiv 1901

  44. [53]

    A&A , keywords =

    Introducing the NEWHORIZON simulation: Galaxy properties with resolved internal dynamics across cosmic time. A&A , keywords =. doi:10.1051/0004-6361/202039429 , archivePrefix =. 2009.10578 , primaryClass =

    Pith/arXiv arXiv 2009

  45. [54]

    MNRAS , keywords =

    The ASTRID simulation: the evolution of supermassive black holes. MNRAS , keywords =. doi:10.1093/mnras/stac351 , archivePrefix =. 2110.14154 , primaryClass =

    Pith/arXiv arXiv

  46. [55]

    MNRAS , keywords =

    The FLAMINGO project: cosmological hydrodynamical simulations for large-scale structure and galaxy cluster surveys. MNRAS , keywords =. doi:10.1093/mnras/stad2419 , archivePrefix =. 2306.04024 , primaryClass =

    Pith/arXiv arXiv

  47. [56]

    Nature Reviews Physics , keywords =

    Cosmological simulations of galaxy formation. Nature Reviews Physics , keywords =. doi:10.1038/s42254-019-0127-2 , archivePrefix =. 1909.07976 , primaryClass =

    Pith/arXiv arXiv 1909

  48. [57]

    MNRAS , keywords =

    Growing the first bright quasars in cosmological simulations of structure formation. MNRAS , keywords =. doi:10.1111/j.1365-2966.2009.15452.x , archivePrefix =. 0905.1689 , primaryClass =

    arXiv 2009

  49. [58]

    Communications in Computational Physics , author=

    Upwind and High-Resolution Methods for Compressible Flow: From Donor Cell to Residual-Distribution Schemes , volume=. Communications in Computational Physics , author=. 2006 , pages=. doi:https://doi.org/2006-CiCP-7954 , number=

    2006

  50. [59]

    SIAM Journal on Scientific and Statistical Computing , author=

    On the Relation Between the Upwind-Differencing Schemes of Godunov, Engquist–Osher and Roe , volume=. SIAM Journal on Scientific and Statistical Computing , author=. 1984 , pages=. doi:10.1137/0905001 , number=

    doi:10.1137/0905001 1984

  51. [63]

    MNRAS , keywords =

    Simulating cosmic structure formation with the GADGET-4 code. MNRAS , keywords =. doi:10.1093/mnras/stab1855 , archivePrefix =. 2010.03567 , primaryClass =

    Pith/arXiv arXiv 2010

  52. [64]

    MNRAS , keywords =

    The cosmological simulation code GADGET-2. MNRAS , keywords =. doi:10.1111/j.1365-2966.2005.09655.x , archivePrefix =. astro-ph/0505010 , primaryClass =

    arXiv 2005

  53. [65]

    ApJs , keywords =

    A New Parallel N-Body Gravity Solver: TPM. ApJs , keywords =. doi:10.1086/192166 , archivePrefix =. astro-ph/9409021 , primaryClass =

    Pith/arXiv arXiv

  54. [66]

    New Astronomy , keywords =

    Performance characteristics of TreePM codes. New Astronomy , keywords =. doi:10.1016/S1384-1076(03)00056-3 , archivePrefix =. astro-ph/0212129 , primaryClass =

    Pith/arXiv arXiv

  55. [67]

    Nature , keywords =

    A hierarchical O(N log N) force-calculation algorithm. Nature , keywords =. doi:10.1038/324446a0 , adsurl =

    doi:10.1038/324446a0

  56. [68]

    Computer Simulation Using Particles

  57. [69]

    MNRAS , keywords =

    Improving the convergence properties of the moving-mesh code AREPO. MNRAS , keywords =. doi:10.1093/mnras/stv2380 , archivePrefix =. 1503.00562 , primaryClass =

    Pith/arXiv arXiv

  58. [70]

    Nature , keywords =

    Tidal disruption of stars by black holes of 10 ^ 6 - 10 ^ 8 solar masses in nearby galaxies. Nature , keywords =. doi:10.1038/333523a0 , adsurl =

    doi:10.1038/333523a0

  59. [71]

    Nature , keywords =

    An ultraluminous X-ray source powered by an accreting neutron star. Nature , keywords =. doi:10.1038/nature13791 , archivePrefix =. 1410.3590 , primaryClass =

    Pith/arXiv arXiv

  60. [72]

    Supermassive Black Holes with High Accretion Rates in Active Galactic Nuclei. IV. H Time Lags and Implications for Super-Eddington Accretion. ApJ , keywords =. doi:10.1088/0004-637X/806/1/22 , archivePrefix =. 1504.01844 , primaryClass =

    Pith/arXiv arXiv

  61. [73]

    Nature , keywords =

    A star in a 15.2-year orbit around the supermassive black hole at the centre of the Milky Way. Nature , keywords =. doi:10.1038/nature01121 , archivePrefix =. astro-ph/0210426 , primaryClass =

    Pith/arXiv arXiv

  62. [74]

    MNRAS , keywords =

    Masses of quasars. MNRAS , keywords =. doi:10.1093/mnras/200.1.115 , adsurl =

    doi:10.1093/mnras/200.1.115

  63. [75]

    ARAA , year = 1984, month = jan, volume =

    Black Hole Models for Active Galactic Nuclei. ARAA , year = 1984, month = jan, volume =. doi:10.1146/annurev.aa.22.090184.002351 , adsurl =

    arXiv 1984

  64. [76]

    Nature , keywords =

    An ultraluminous quasar with a twelve-billion-solar-mass black hole at redshift 6.30. Nature , keywords =. doi:10.1038/nature14241 , archivePrefix =. 1502.07418 , primaryClass =

    Pith/arXiv arXiv

  65. [77]

    AAR , keywords =

    Formation of supermassive black holes. AAR , keywords =. doi:10.1007/s00159-010-0029-x , archivePrefix =. 1003.4404 , primaryClass =

    Pith/arXiv arXiv

  66. [78]

    Nature , year = 1969, month = aug, volume =

    Galactic Nuclei as Collapsed Old Quasars. Nature , year = 1969, month = aug, volume =. doi:10.1038/223690a0 , adsurl =

    doi:10.1038/223690a0 1969

  67. [79]

    ApJ , year = 1964, month = aug, volume =

    Accretion of Interstellar Matter by Massive Objects. ApJ , year = 1964, month = aug, volume =. doi:10.1086/147973 , adsurl =

    doi:10.1086/147973 1964

  68. [80]

    ARAA , keywords =

    Powerful Outflows and Feedback from Active Galactic Nuclei. ARAA , keywords =. doi:10.1146/annurev-astro-082214-122316 , archivePrefix =. 1503.05206 , primaryClass =

    Pith/arXiv arXiv

  69. [81]

    MNRAS , keywords =

    Moving-mesh cosmology: properties of neutral hydrogen in absorption. MNRAS , keywords =. doi:10.1093/mnras/sts590 , archivePrefix =. 1209.2118 , primaryClass =

    Pith/arXiv arXiv

  70. [82]

    , keywords =

    X-Ray Weak Active Galactic Nuclei from Super-Eddington Accretion onto Infant Black Holes. , keywords =. doi:10.3847/2041-8213/ad90e1 , archivePrefix =. 2410.00417 , primaryClass =

    Pith/arXiv arXiv 2041

  71. [83]

    , keywords =

    The case for large-scale AGN feedback in galaxy formation simulations: insights from XFABLE. , keywords =. doi:10.1093/mnras/staf1435 , archivePrefix =. 2501.16983 , primaryClass =

    arXiv

  72. [84]

    ARAA , keywords =

    The Assembly of the First Massive Black Holes. ARAA , keywords =. doi:10.1146/annurev-astro-120419-014455 , archivePrefix =. 1911.05791 , primaryClass =

    Pith/arXiv arXiv 1911

  73. [85]

    MNRAS , keywords =

    Pulsing ULXs: tip of the iceberg?. MNRAS , keywords =. doi:10.1093/mnrasl/slx020 , archivePrefix =. 1702.00808 , primaryClass =

    Pith/arXiv arXiv

  74. [86]

    ApJ , keywords =

    Slim Accretion Disks. ApJ , keywords =. doi:10.1086/166683 , adsurl =

    doi:10.1086/166683

  75. [87]

    MNRAS , keywords =

    Can a spherically accreting black hole radiate very near the Eddington limit?. MNRAS , keywords =. doi:10.1093/mnras/187.2.237 , adsurl =

    doi:10.1093/mnras/187.2.237

  76. [88]

    ApJl , keywords =

    A Two-Phase Model for the X-Ray Emission from Seyfert Galaxies. ApJl , keywords =. doi:10.1086/186171 , adsurl =

    doi:10.1086/186171

  77. [89]

    Observational appearance

    Black holes in binary systems. Observational appearance. AA , year = 1973, month = jan, volume =

    1973

  78. [90]

    PASJ , keywords =

    Galactic Black-Hole Candidates Shining at the Eddington Luminosity. PASJ , keywords =. doi:10.1093/pasj/52.1.133 , adsurl =

    doi:10.1093/pasj/52.1.133

  79. [91]

    A&A , keywords =

    How the super-Eddington regime regulates black hole growth in high-redshift galaxies. A&A , keywords =. doi:10.1051/0004-6361/202243170 , archivePrefix =. 2201.08766 , primaryClass =

    Pith/arXiv arXiv

  80. [92]

    Living Reviews in Relativity , keywords =

    Foundations of Black Hole Accretion Disk Theory. Living Reviews in Relativity , keywords =. doi:10.12942/lrr-2013-1 , archivePrefix =. 1104.5499 , primaryClass =

    Pith/arXiv arXiv 2013

Showing first 80 references.