pith. sign in

arxiv: 2606.00205 · v1 · pith:W4OV7TPBnew · submitted 2026-05-29 · 🌌 astro-ph.GA

Ultraviolet diversity of Little Red Dots as a probe for direct-collapse black hole ages

Elia Cenci , Melanie Habouzit , Dale D. Kocevski This is my paper

Pith reviewed 2026-06-28 21:44 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Little Red Dotsdirect-collapse black holesultraviolet emissionhigh-redshift galaxiesPop III starsblack hole accretionJWST observationscosmological simulations
0
0 comments X

The pith

The UV diversity of Little Red Dots encodes the ages of their embedded direct-collapse black holes via the relative host-galaxy contribution.

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

The paper uses a cosmological hydrodynamical simulation to track how ultraviolet light from Pop III stars and an accreting direct-collapse black hole changes over the first 30 million years after black-hole formation. Early on the black hole dominates the UV output because the host has little stellar mass and low metallicity; later, star formation builds up and the stellar continuum takes over, producing bluer colors. This rapid shift means that observed UV-bright Little Red Dots are predicted to contain older black holes with higher metallicities, lower black-hole-to-stellar-mass ratios, and lower Eddington ratios. The short duration of the Little Red Dot phase therefore imposes a timing constraint on when such objects can appear in the early universe. The central result is that the relative strength of the host-galaxy UV continuum supplies an observable clock for the age of the direct-collapse black hole.

Core claim

Using the MELIORA simulation suite, the authors find that the rest-frame 0.2–0.6 μm emission from LRD candidates at z > 8.5 transitions from black-hole-dominated to stellar-dominated within roughly 30 Myr after DCBH formation. The transition is driven by the build-up of stellar mass and metal enrichment in the host, after which the stellar continuum overwhelms the accreting DCBH, yielding bluer colors and more extended morphologies. Consequently, UV-bright LRDs are expected to host older DCBHs that exhibit higher gas-phase metallicities, lower BH-to-stellar mass ratios, and lower Eddington ratios, while the short-lived nature of the LRD phase limits their cosmic emergence window.

What carries the argument

The rapid ~30 Myr evolution of the UV continuum from Pop III stars versus the accreting DCBH in simulated LRD hosts at z > 8.5, which maps observed UV brightness onto DCBH age and accretion state.

If this is right

  • UV-bright LRDs correspond to older DCBHs with elevated metallicities.
  • UV-faint LRDs correspond to younger DCBHs with higher accretion rates and lower metallicities.
  • The LRD phase lasts only tens of Myr, restricting the redshift window in which they can be observed.
  • Emission-line properties and gas-phase metallicities should correlate systematically with UV color as a direct consequence of the evolutionary sequence.

Where Pith is reading between the lines

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

  • Multi-band JWST spectra could be used to infer DCBH ages without requiring direct dynamical mass measurements.
  • The same UV-color diagnostic may distinguish DCBH hosts from other high-redshift AGN or star-forming galaxies once the simulation assumptions are tested.
  • If the 30 Myr timescale holds, the observed number density of LRDs directly constrains the formation rate of DCBHs at z > 8.5.

Load-bearing premise

The simulation accurately reproduces the UV emission history of Pop III stars and accreting DCBHs over the first 30 million years in these high-redshift systems.

What would settle it

A statistical sample of UV-bright LRDs that show low gas-phase metallicities and high Eddington ratios would falsify the predicted age–UV-brightness correlation.

Figures

Figures reproduced from arXiv: 2606.00205 by Dale D. Kocevski, Elia Cenci, Melanie Habouzit.

Figure 1
Figure 1. Figure 1: — Schematic illustration of the evolutionary sequence of LRD candidate DCBHs. We show idealized rest-frame UV-optical composite SEDs of PopIII stars (blue curves) and an enshrouded accreting DCBH (black curve), for different BH-to-stellar mass ratios. Immediately after DCBH formation (early LRD phase), the stellar mass is negligible and the UV continuum is weak, yielding BH-dominated emission and red UV-op… view at source ↗
Figure 2
Figure 2. Figure 2: — Evolution of the UV–optical colour ∆mag = log10 L5100/L2500 for simulated DCBH+host systems at z > 8.5 in meli⊙ra, as a function of the DCBH age (time since formation). Here, we only consider accreting DCBHs with bolometric luminosity Lbol > 1040 erg s−1 . The black dashed lines trace the median trend of ∆mag as a function of DCBH age, with bootstrapped (16th to 84th percentiles) uncertainties. From left… view at source ↗
Figure 3
Figure 3. Figure 3: — Stacked histograms for (from left to right) the BH-to-stellar mass ratio (MBH/M⋆), total extent of the stellar mass distribution (R⋆), bolometric luminosity (Lbol), and gas-phase metallicity (Lbol), associated with DCBHs in the early, late, and post LRD phases. Here, we only consider accreting DCBHs with Lbol > 1040 erg s−1 . In general, newborn DCBHs in early and late LRDs at z > 8.5 in meli⊙ra naturall… view at source ↗
Figure 4
Figure 4. Figure 4: — Fraction of DCBHs of a given age that are selected as LRD candidates in meli⊙ra, i.e. that have (i) compact stellar sizes R⋆ < 100 pc, (ii) large UV-optical colours with ∆mag > 0, and (iii) bolometric luminosity above three different thresholds Lbol > 1042 , 1042.7 , 1043 erg s−1 (dotted, dashed, and solid lines, respectively). Data points mark the median LRD fraction, with bootstrapped (16th to 84th per… view at source ↗
read the original abstract

Little Red Dots (LRDs) uncovered by the James Webb Space Telescope have been proposed as candidate galaxies hosting embedded accreting direct-collapse black holes (DCBHs), yet the relative ultraviolet (UV) emission of their host galaxy remains highly uncertain and diverse across the population. Using a large-scale cosmological hydrodynamical simulation from the MELIORA suite, we investigate the contribution of PopIII stars and accreting DCBHs in LRD candidates at $z>8.5$, in the rest-frame $0.2-0.6~\mu\mathrm{m}$ band. We find that the UV emission from the host galaxy evolves rapidly over the first $\sim 30~\mathrm{Myr}$ following DCBH formation, reflecting the build-up of stellar mass and metal enrichment. This evolution consists of a rapid transition from initially BH-dominated systems, with negligible stellar mass, low metallicity, and high accretion rates, to progressively more developed hosts in which rapid star formation enhances the UV output and metallicity increases. After $\sim 30~\mathrm{Myr}$, the stellar continuum typically overwhelms the accreting DCBH contribution, producing bluer colours and more extended stellar distributions. As a result, UV-bright LRDs are predicted to host older DCBHs, have higher gas-phase metallicities, lower BH-to-stellar mass ratios, and lower Eddington ratios. The short-lived nature of the LRD phase places strong constraints on their emergence over cosmic time. Overall, our results suggest that DCBH ages can be constrained from the host galaxy contribution to the UV-optical spectrum of LRDs, relative to that of the accreting DCBH, and support the picture in which a DCBH evolutionary sequence is systematically encoded in emission line properties, gas-phase metallicities, and accretion states.

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

1 major / 0 minor

Summary. The manuscript uses the MELIORA cosmological hydrodynamical simulation to model the rest-frame 0.2-0.6 μm UV emission from Pop III stars and accreting DCBHs in LRD candidates at z>8.5. It reports that host-galaxy UV output evolves rapidly over the first ~30 Myr after DCBH formation, transitioning from initially BH-dominated (negligible stellar mass, low metallicity, high accretion) to stellar-dominated systems with enhanced UV, higher metallicity, bluer colors, and more extended distributions. The work proposes that observed UV diversity can therefore constrain DCBH ages, with UV-bright LRDs corresponding to older DCBHs having higher gas-phase metallicities, lower BH-to-stellar mass ratios, and lower Eddington ratios, while the short LRD lifetime constrains their cosmic emergence.

Significance. If the reported evolutionary sequence is robust, the paper supplies a concrete theoretical mapping from UV color and spectral properties to DCBH age that could be tested with JWST spectroscopy of LRDs, linking observables (emission lines, metallicity, accretion state) into a single evolutionary picture and tightening constraints on the duty cycle of the LRD phase at z>8.5.

major comments (1)
  1. [Simulation description and results (abstract and methods)] The central claim that DCBH ages can be constrained from the relative host-galaxy versus BH UV contribution rests on the specific ~30 Myr stellar-takeover timescale produced by the MELIORA suite. No robustness tests against variations in the subgrid star-formation efficiency, metal-mixing scheme, or BH accretion/feedback prescriptions are shown; because the transition time is set by these choices, the proposed age-diagnostic mapping is not demonstrated to be general.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the constructive report. The single major comment is addressed point-by-point below.

read point-by-point responses

  1. Referee: [Simulation description and results (abstract and methods)] The central claim that DCBH ages can be constrained from the relative host-galaxy versus BH UV contribution rests on the specific ~30 Myr stellar-takeover timescale produced by the MELIORA suite. No robustness tests against variations in the subgrid star-formation efficiency, metal-mixing scheme, or BH accretion/feedback prescriptions are shown; because the transition time is set by these choices, the proposed age-diagnostic mapping is not demonstrated to be general.

    Authors: We agree that the reported ~30 Myr transition timescale is specific to the fiducial subgrid prescriptions (star-formation efficiency, metal-mixing scheme, and BH accretion/feedback) adopted in the MELIORA suite and that no explicit robustness tests are presented. The manuscript therefore does not demonstrate that the precise numerical value of the timescale, or the quantitative age-diagnostic mapping, is independent of these choices. The qualitative sequence itself—from initially BH-dominated UV emission to stellar-dominated emission—follows from the finite lifetimes of massive Pop III stars (~10 Myr) and the subsequent metal enrichment that enables more efficient star formation; these physical ingredients are present in any standard cosmological simulation. In the revised manuscript we will add a dedicated paragraph in the discussion section that explicitly qualifies the results as model-dependent, states the adopted subgrid parameters, and notes that the proposed UV-based age diagnostic applies within the context of simulations employing comparable prescriptions. We do not claim universality beyond these assumptions. revision: yes

Circularity Check

0 steps flagged

No circularity: forward simulation outputs independent of fitted LRD data

full rationale

The paper's central results derive from running the MELIORA cosmological hydrodynamical simulation suite to evolve Pop III stars and accreting DCBHs at z>8.5, then reporting the emergent UV contributions, metallicities, and timescales as model outputs. No equations or claims reduce a prediction to a quantity fitted from the same LRD observations; the ~30 Myr transition is an emergent simulation result under the chosen subgrid prescriptions rather than a self-definition or renamed fit. No load-bearing self-citations, uniqueness theorems, or ansatzes imported from prior author work appear in the provided text. The derivation chain is therefore self-contained against external simulation benchmarks and does not exhibit any of the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Only the abstract is available; therefore free parameters, axioms, and invented entities cannot be enumerated from the full text. The claim depends on the validity of the MELIORA simulation physics and the premise that LRDs host embedded DCBHs.

pith-pipeline@v0.9.1-grok · 5872 in / 1284 out tokens · 30338 ms · 2026-06-28T21:44:07.040718+00:00 · methodology

discussion (0)

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

Reference graph

Works this paper leans on

300 extracted references · 295 canonical work pages · 181 internal anchors

  1. [1]

    Laser Interferometer Space Antenna

    Laser Interferometer Space Antenna. arXiv e-prints , keywords =. doi:10.48550/arXiv.1702.00786 , archivePrefix =. 1702.00786 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1702.00786

  2. [2]

    Songlines from Direct Collapse Seed Black Holes: Effects of X-rays on Black Hole Growth and Stellar Populations

    Songlines from Direct Collapse Seed Black Holes: Effects of X-Rays on Black Hole Growth and Stellar Populations. , keywords =. doi:10.1088/0004-637X/797/2/139 , archivePrefix =. 1409.0543 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/797/2/139

  3. [3]

    , year = 1978, month = dec, volume =

    The fate of dense stellar systems. , year = 1978, month = dec, volume =. doi:10.1093/mnras/185.4.847 , adsurl =

    work page doi:10.1093/mnras/185.4.847 1978

  4. [4]

    Angular Momentum Transfer and Lack of Fragmentation in Self-Gravitating Accretion Flows

    Angular Momentum Transfer and Lack of Fragmentation in Self-Gravitating Accretion Flows. , keywords =. doi:10.1088/0004-637X/702/1/L5 , archivePrefix =. 0904.4247 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/702/1/l5

  5. [5]

    The First Massive Black Hole Seeds and Their Hosts

    The First Massive Black Hole Seeds and Their Hosts. , keywords =. doi:10.1088/0004-637X/742/1/13 , archivePrefix =. 1104.3858 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/742/1/13

  6. [6]

    Wandering Black Holes in Bright Disk Galaxy Halos

    Wandering Black Holes in Bright Disk Galaxy Halos. , keywords =. doi:10.1088/2041-8205/721/2/L148 , archivePrefix =. 1008.5147 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/721/2/l148 2041

  7. [7]

    , keywords =

    Effects of gravitational-wave recoil on the dynamics and growth of supermassive black holes. , keywords =. doi:10.1111/j.1365-2966.2008.13790.x , archivePrefix =. 0805.1420 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.13790.x 2008

  8. [8]

    Massive black hole seeds born via direct gas collapse in galaxy mergers: their properties, statistics and environment

    Massive black hole seeds born via direct gas collapse in galaxy mergers: their properties, statistics and environment. , keywords =. doi:10.1093/mnras/stt1990 , archivePrefix =. 1211.3752 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1990

  9. [9]

    The Origin and Evolution of the Mass-Metallicity Relationship for Galaxies: Results from Cosmological N-Body Simulations

    The Origin and Evolution of the Mass-Metallicity Relationship for Galaxies: Results from Cosmological N-Body Simulations. , keywords =. doi:10.1086/511765 , archivePrefix =. astro-ph/0609620 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/511765

  10. [10]

    Interpreting the Evolution of the Size - Luminosity Relation for Disk Galaxies from Redshift 1 to the Present

    Interpreting the Evolution of the Size-Luminosity Relation for Disk Galaxies from Redshift 1 to the Present. , keywords =. doi:10.1088/0004-637X/728/1/51 , archivePrefix =. 1011.0432 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/728/1/51

  11. [11]

    HD and H2 formation in low-metallicity dusty gas clouds at high redshift

    HD and H\ 2\ formation in low-metallicity dusty gas clouds at high redshift. , keywords =. doi:10.1051/0004-6361:200811302 , archivePrefix =. 0901.0514 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:200811302

  12. [12]

    Supermassive Black Hole Formation at High Redshifts via Direct Collapse: Physical Processes in the Early Stage

    Supermassive Black Hole Formation at High Redshifts via Direct Collapse: Physical Processes in the Early Stage. , keywords =. doi:10.1088/0004-637X/774/2/149 , archivePrefix =. 1304.1369 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/774/2/149

  13. [13]

    Simulating disc galaxy bulges that are consistent with observed scaling relations

    Simulating disc galaxy bulges that are consistent with observed scaling relations. , keywords =. doi:10.1093/mnrasl/slu020 , archivePrefix =. 1402.2702 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnrasl/slu020

  14. [14]

    Star Formation and Feedback in Smoothed Particle Hydrodynamic Simulations. II. Resolution Effects. , keywords =. doi:10.1088/0004-637X/717/1/121 , archivePrefix =. 1005.1681 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/717/1/121

  15. [15]

    , keywords =

    The First Stellar Cluster. , keywords =. doi:10.1086/524187 , adsurl =

    work page doi:10.1086/524187

  16. [16]

    Black hole mass estimates and emission-line properties of a sample of redshift z>6.5 quasars

    Black Hole Mass Estimates and Emission-line Properties of a Sample of Redshift z > 6.5 Quasars. , keywords =. doi:10.1088/0004-637X/790/2/145 , archivePrefix =. 1311.3260 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/790/2/145

  17. [17]

    Formation of the first nuclear clusters and massive black holes at high redshift

    Formation of the First Nuclear Clusters and Massive Black Holes at High Redshift. , keywords =. doi:10.1088/0004-637X/694/1/302 , archivePrefix =. 0810.1057 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/694/1/302

  18. [18]

    2012, MNRAS, 425, 1068, doi:10.1111/j.1365-2966.2012.21439.x

    Feeding compact bulges and supermassive black holes with low angular momentum cosmic gas at high redshift. , keywords =. doi:10.1111/j.1365-2966.2012.21160.x10.1002/asna.19141990903 , archivePrefix =. 1112.2479 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21160.x10.1002/asna.19141990903 2012

  19. [19]

    A Survey of z>5.7 Quasars in the Sloan Digital Sky Survey. II. Discovery of Three Additional Quasars at z>6. , keywords =. doi:10.1086/368246 , archivePrefix =. astro-ph/0301135 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/368246

  20. [20]

    Simulating the formation of massive seed black holes in the early Universe. II: Impact of rate coefficient uncertainties

    Simulating the formation of massive seed black holes in the early Universe - II. Impact of rate coefficient uncertainties. , keywords =. doi:10.1093/mnras/stv1781 , archivePrefix =. 1504.00514 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1781

  21. [21]

    Simulating the formation of massive seed black holes in the early Universe. III: The influence of X-rays

    Simulating the formation of massive seed black holes in the early Universe. III: The influence of X-rays. arXiv e-prints , keywords =. doi:10.48550/arXiv.1610.05679 , archivePrefix =. 1610.05679 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1610.05679

  22. [22]

    , keywords =

    Forming a large disc galaxy from a z < 1 major merger. , keywords =. doi:10.1111/j.1365-2966.2009.15143.x , archivePrefix =. 0812.0379 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15143.x 2009

  23. [23]

    Radiative Transfer in a Clumpy Universe. II. The Ultraviolet Extragalactic Background. , keywords =. doi:10.1086/177035 , archivePrefix =. astro-ph/9509093 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/177035

  24. [24]

    H_2 Cooling of Primordial Gas Triggered by UV Irradiation

    H 2 Cooling of Primordial Gas Triggered by UV Irradiation. , keywords =. doi:10.1086/177628 , archivePrefix =. astro-ph/9511126 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/177628

  25. [25]

    What is the Highest Plausible Redshift of Luminous Quasars?

    What Is the Highest Plausible Redshift of Luminous Quasars?. , keywords =. doi:10.1086/320586 , archivePrefix =. astro-ph/0011529 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/320586

  26. [26]

    , year = 2006, month = nov, volume =

    The formation of the first black holes and their host halos. , year = 2006, month = nov, volume =. doi:10.1016/j.newar.2006.06.021 , adsurl =

    work page doi:10.1016/j.newar.2006.06.021 2006

  27. [27]

    Supersonic Gas Streams Enhance the Formation of Massive Black Holes in the Early Universe

    Supersonic gas streams enhance the formation of massive black holes in the early universe. Science , keywords =. doi:10.1126/science.aai9119 , archivePrefix =. 1709.09863 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.aai9119

  28. [28]

    Gravitational Wave Recoil and the Retention of Intermediate Mass Black Holes

    Gravitational Wave Recoil and the Retention of Intermediate-Mass Black Holes. , keywords =. doi:10.1086/591218 , archivePrefix =. 0707.1334 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/591218

  29. [29]

    Gravitational Wave Signal from Assembling the Lightest Supermassive Black Holes

    Gravitational Wave Signal from Assembling the Lightest Supermassive Black Holes. , keywords =. doi:10.1088/0004-637X/713/2/1016 , archivePrefix =. 1002.3378 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/713/2/1016

  30. [30]

    Kickstarting Reionization with the First Black Holes: the effects of second-order perturbation theory in pre-reionization volumes

    Kickstarting Reionization with the First Black Holes: The Effects of Second-order Perturbation Theory in Pre-reionization Volumes. , keywords =. doi:10.1088/2041-8205/761/1/L8 , archivePrefix =. 1211.1394 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/761/1/l8 2041

  31. [31]

    , keywords =

    Hierarchical Galaxy Formation: Overmerging and the Formation of an X-Ray Cluster. , keywords =. doi:10.1086/172935 , adsurl =

    work page doi:10.1086/172935

  32. [32]

    MNRAS , keywords =

    The Distribution of Low-Mass Stars in the Galactic Disc. , keywords =. doi:10.1093/mnras/262.3.545 , adsurl =

    work page doi:10.1093/mnras/262.3.545

  33. [33]

    Black hole masses and enrichment of z ~ 6 SDSS quasars

    Black Hole Masses and Enrichment of z -0.5ex 6 SDSS Quasars. , keywords =. doi:10.1086/521596 , archivePrefix =. 0707.1662 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/521596

  34. [34]

    , keywords =

    On the Occupation Fraction of Seed Black Holes in High-redshift Dark Matter Halos. , keywords =. doi:10.1088/0004-637X/701/1/360 , adsurl =

    work page doi:10.1088/0004-637x/701/1/360

  35. [35]

    , keywords =

    Mass accretion rates and histories of dark matter haloes. , keywords =. doi:10.1111/j.1365-2966.2009.15329.x , archivePrefix =. 0902.3659 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15329.x 2009

  36. [36]

    The Merger History of Supermassive Black Holes in Galaxies

    The Merger History of Supermassive Black Holes in Galaxies. , keywords =. doi:10.1086/322310 , archivePrefix =. astro-ph/0101196 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/322310

  37. [37]

    Black Hole Growth from Cosmological N-body Simulations

    Black Hole Growth from Cosmological N-body Simulations. arXiv e-prints , keywords =. doi:10.48550/arXiv.0805.3154 , archivePrefix =. 0805.3154 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.0805.3154

  38. [38]

    Reproducing the Stellar Mass/Halo Mass Relation in Simulated LCDM Galaxies: Theory vs Observational Estimates

    Reproducing the Stellar Mass/Halo Mass Relation in Simulated CDM Galaxies: Theory versus Observational Estimates. , keywords =. doi:10.1088/0004-637X/766/1/56 , archivePrefix =. 1209.1389 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/766/1/56

  39. [39]

    The Pressure of the Star Forming ISM in Cosmological Simulations

    The Pressure of the Star-forming Interstellar Medium in Cosmological Simulations. , keywords =. doi:10.1088/2041-8205/781/1/L14 , archivePrefix =. 1312.1700 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/781/1/l14 2041

  40. [40]

    pynbody: N-Body/SPH analysis for python

  41. [41]

    doi:10.1046/j.1365-8711.2003.06515.x , Eprint =

    The inner structure of CDM haloes - I. A numerical convergence study. , keywords =. doi:10.1046/j.1365-8711.2003.05925.x , archivePrefix =. astro-ph/0201544 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.05925.x 2003

  42. [42]

    Rapid Formation of Massive Black Holes in close proximity to Embryonic Proto-Galaxies

    Rapid formation of massive black holes in close proximity to embryonic protogalaxies. Nature Astronomy , keywords =. doi:10.1038/s41550-017-0075 , archivePrefix =. 1703.03805 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-017-0075

  43. [43]

    Fragmentation inside atomic cooling haloes exposed to Lyman-Werner radiation

    Fragmentation inside atomic cooling haloes exposed to Lyman-Werner radiation. , keywords =. doi:10.1093/mnras/sty134 , archivePrefix =. 1708.07772 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty134

  44. [44]

    and Cawthorne, T.V

    Multiphase smoothed-particle hydrodynamics. , keywords =. doi:10.1046/j.1365-8711.2001.04268.x , archivePrefix =. astro-ph/0005357 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04268.x 2001

  45. [45]

    Lyman-Werner Escape Fractions from the First Galaxies

    Lyman-Werner escape fractions from the first galaxies. , keywords =. doi:10.1093/mnras/stx264 , archivePrefix =. 1701.07031 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx264

  46. [46]

    The formation of direct collapse black holes under the influence of streaming velocities

    The formation of direct collapse black holes under the influence of streaming velocities. , keywords =. doi:10.1093/mnras/stx1915 , archivePrefix =. 1705.02347 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1915

  47. [47]

    The Distribution of Recoil Velocities from Merging Black Holes

    The Distribution of Recoil Velocities from Merging Black Holes. , keywords =. doi:10.1086/519309 , archivePrefix =. astro-ph/0702641 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/519309

  48. [48]

    B., & Heggie, D

    The enrichment of the intergalactic medium with adiabatic feedback - I. Metal cooling and metal diffusion. , keywords =. doi:10.1111/j.1365-2966.2010.17047.x , archivePrefix =. 0910.5956 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17047.x 2010

  49. [49]

    , keywords =

    Bars within bars: a mechanism for fuelling active galactic nuclei. , keywords =. doi:10.1038/338045a0 , adsurl =

    work page doi:10.1038/338045a0

  50. [50]

    Wilkinson Microwave Anisotropy Probe (WMAP) Three Year Results: Implications for Cosmology

    Three-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for Cosmology. , keywords =. doi:10.1086/513700 , archivePrefix =. astro-ph/0603449 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/513700

  51. [51]

    Cosmological N-body simulations and their analysis

  52. [52]

    The Assembly of Supermassive Black Holes at High Redshifts

    The Assembly of Supermassive Black Holes at High Redshifts. , keywords =. doi:10.1088/0004-637X/696/2/1798 , archivePrefix =. 0807.4702 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/696/2/1798

  53. [53]

    2012, MNRAS, 425, 1068, doi:10.1111/j.1365-2966.2012.21439.x

    X-ray emission from high-redshift miniquasars: self-regulating the population of massive black holes through global warming. , keywords =. doi:10.1111/j.1365-2966.2012.21539.x , archivePrefix =. 1205.6467 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21539.x 2012

  54. [54]

    The formation of massive black holes in z~30 dark matter haloes with large baryonic streaming velocities

    The formation of massive black holes in z 30 dark matter haloes with large baryonic streaming velocities. , keywords =. doi:10.1093/mnras/stu042 , archivePrefix =. 1310.0859 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu042

  55. [55]

    B., & Heggie, D

    Massive black holes lurking in Milky Way satellites. , keywords =. doi:10.1111/j.1365-2966.2010.17189.x , archivePrefix =. 1001.5451 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17189.x 2010

  56. [56]

    What is the Maximum Mass of a Population III Galaxy?

    What is the maximum mass of a Population III galaxy?. , keywords =. doi:10.1093/mnras/stx909 , archivePrefix =. 1701.00814 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx909

  57. [57]

    The Assembly and Merging History of Supermassive Black Holes in Hierarchical Models of Galaxy Formation

    The Assembly and Merging History of Supermassive Black Holes in Hierarchical Models of Galaxy Formation. , keywords =. doi:10.1086/344675 , archivePrefix =. astro-ph/0207276 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/344675

  58. [58]

    , keywords =

    Journey to the M _ BH - relation: the fate of low-mass black holes in the Universe. , keywords =. doi:10.1111/j.1365-2966.2009.15577.x , archivePrefix =. 0903.2262 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.15577.x 2009

  59. [59]

    Gasoline2: A Modern SPH Code

    Gasoline2: a modern smoothed particle hydrodynamics code. , keywords =. doi:10.1093/mnras/stx1643 , archivePrefix =. 1707.03824 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1643

  60. [60]

    The role of stellar relaxation in the formation and evolution of the first massive black holes

    The role of stellar relaxation in the formation and evolution of the first massive black holes. , keywords =. doi:10.1093/mnras/stw058 , archivePrefix =. 1507.06701 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw058

  61. [61]

    Triggering the formation of direct collapse black holes by their congeners

    Triggering the Formation of Direct Collapse Black Holes by Their Congeners. , keywords =. doi:10.3847/1538-4357/aa6627 , archivePrefix =. 1612.07885 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa6627

  62. [62]

    Baryons Matter: Why Luminous Satellite Galaxies Have Reduced Central Masses

    Baryons Matter: Why Luminous Satellite Galaxies have Reduced Central Masses. , keywords =. doi:10.1088/0004-637X/761/1/71 , archivePrefix =. 1207.0007 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/761/1/71

  63. [63]

    Detecting Direct Collapse Black Holes: making the case for CR7

    Detecting direct collapse black holes: making the case for CR7. , keywords =. doi:10.1093/mnras/stw1173 , archivePrefix =. 1510.01733 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw1173

  64. [64]

    2004, MNRAS, 349, 476, doi:10.1111/j.1365-2966.2004.07508.x Light Cone Strong Lensing 17

    A model for infall around virialized haloes. , keywords =. doi:10.1111/j.1365-2966.2004.07177.x , archivePrefix =. astro-ph/0212458 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.07177.x 2004

  65. [65]

    On The Maximum Mass of Stellar Black Holes

    On the Maximum Mass of Stellar Black Holes. , keywords =. doi:10.1088/0004-637X/714/2/1217 , archivePrefix =. 0904.2784 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/714/2/1217

  66. [66]

    , keywords =

    Excursion Set Mass Functions for Hierarchical Gaussian Fluctuations. , keywords =. doi:10.1086/170520 , adsurl =

    work page doi:10.1086/170520

  67. [67]

    Mass Measurements of Stellar and Intermediate Mass Black-Holes

    Mass Measurements of Stellar and Intermediate-Mass Black Holes. , keywords =. doi:10.1007/s11214-013-0030-6 , archivePrefix =. 1311.5118 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-013-0030-6

  68. [68]

    Lower Metal Enrichment of Virialized Gas in Minihalos

    Lower Metal Enrichment of Virialized Gas in Minihalos. , keywords =. doi:10.1086/524724 , archivePrefix =. 0704.3545 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/524724

  69. [69]

    A Recipe for Galaxy Formation Shaun Cole

    A recipe for galaxy formation. , keywords =. doi:10.1093/mnras/271.4.781 , archivePrefix =. astro-ph/9402001 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/271.4.781

  70. [70]

    , keywords =

    The fate of gas in elliptical galaxies and the density evolution of of radio sources. , keywords =

  71. [71]

    doi:10.1046/j.1365-8711.2003.06515.x , Eprint =

    Radiative feedback from an early X-ray background. , keywords =. doi:10.1046/j.1365-8711.2003.06311.x , archivePrefix =. astro-ph/0205308 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06311.x 2003

  72. [72]

    doi:10.1046/j.1365-8711.2003.06515.x , Eprint =

    High-mass X-ray binaries as a star formation rate indicator in distant galaxies. , keywords =. doi:10.1046/j.1365-8711.2003.06224.x , archivePrefix =. astro-ph/0205371 , primaryClass =

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

  73. [73]

    MUSIC: MUlti-Scale Initial Conditions

  74. [74]

    Exploring the nature of the Lyman-$\alpha$ emitter CR7

    Exploring the nature of the Lyman- emitter CR7. , keywords =. doi:10.1093/mnras/stw1775 , archivePrefix =. 1512.01111 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw1775

  75. [75]

    Primordial Star Formation under the Influence of Far Ultraviolet Radiation: 1540 Cosmological Halos and the Stellar Mass Distribution

    Primordial star formation under the influence of far ultraviolet radiation: 1540 cosmological haloes and the stellar mass distribution. , keywords =. doi:10.1093/mnras/stv044 , archivePrefix =. 1501.01630 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv044

  76. [76]

    The Impact of Small-Scale Structure on Cosmological Ionization Fronts and Reionization

    The Impact of Small-Scale Structure on Cosmological Ionization Fronts and Reionization. , keywords =. doi:10.1086/429083 , archivePrefix =. astro-ph/0411035 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/429083

  77. [77]

    2007b, MNRAS, 381, 171, doi:10.1111/j.1365-2966.2007.12225.x

    Self-regulated reionization. , keywords =. doi:10.1111/j.1365-2966.2007.11482.x , archivePrefix =. astro-ph/0607517 , primaryClass =

    work page doi:10.1111/j.1365-2966.2007.11482.x 2007

  78. [78]

    2011, Monthly Notices of the Royal Astronomical Society, 415, 2101, doi: 10.1111/j.1365-2966.2011.18820.x

    Effect of cosmic ray/X-ray ionization on supermassive black hole formation. , keywords =. doi:10.1111/j.1365-2966.2011.19229.x , archivePrefix =. 1106.2812 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19229.x 2011

  79. [79]

    2012, MNRAS, 425, 1068, doi:10.1111/j.1365-2966.2012.21439.x

    Supermassive black hole formation by cold accretion shocks in the first galaxies. , keywords =. doi:10.1111/j.1365-2966.2012.20812.x , archivePrefix =. 1202.5380 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.20812.x 2012

  80. [80]

    The suppression of direct collapse black hole formation by soft X-ray irradiation

    The suppression of direct collapse black hole formation by soft X-ray irradiation. , keywords =. doi:10.1093/mnras/stv871 , archivePrefix =. 1411.2590 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv871

Showing first 80 references.