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arxiv: 2606.27426 · v1 · pith:YVPVLZOCnew · submitted 2026-06-25 · 🌌 astro-ph.GA · astro-ph.HE

Too shy to spin? Cosmic wallflowers as proto-globular clusters

Floor van Donkelaar , Lucio Mayer , Pedro R. Capelo This is my paper

Pith reviewed 2026-06-29 02:07 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.HE
keywords globular clustershigh-redshift clusterscosmic filamentsstar cluster formationcluster kinematicsnumerical simulationsrotational supportgalactic discs
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The pith

Weakly rotating gas-rich cosmic wallflowers at z~7.6 overlap with Milky Way globular cluster properties while disc clusters do not.

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

The paper compares star-forming clusters at redshift 7.6 in the MassiveBlackPS simulation, separating those born in galactic discs through gravitational instability from isolated cosmic wallflowers formed in filaments. Disc clusters show strong rotational support and high velocities, whereas wallflowers display lower rotation overall and a wider spread in v/σ, with gas-rich examples falling nearest to observed globular cluster densities. The authors conclude that formation environment and gas content together set the initial dynamical state, making the low-rotation wallflowers plausible proto-globular cluster candidates that could reach present-day configurations through angular momentum loss and dynamical heating.

Core claim

At z ~ 7.6, cosmic wallflowers born from filaments exhibit systematically lower rotational velocities and a broad range in v/σ compared with strongly rotation-dominated disc clusters formed via gravitational instability; when combined with stellar surface density, a gas-rich low-rotation subset of wallflowers lies close to the Milky Way globular cluster population while disc clusters remain offset, indicating that environment imprints on initial conditions and that weakly rotating wallflowers may evolve into present-day systems via angular momentum loss and dynamical heating.

What carries the argument

Separation of clusters into disc (gravitational instability) and cosmic wallflower (filament-born) channels, quantified through stellar rotational velocity v_rot and rotational support v/σ together with surface density.

If this is right

  • Formation environment and baryonic gas content together determine the initial dynamical state of high-redshift clusters.
  • Gas-rich wallflowers preferentially occupy the low-rotation regime that overlaps globular cluster properties.
  • Denser, more rotationally supported wallflowers may follow a separate path possibly connected to massive black hole seed formation.
  • Angular momentum loss and dynamical heating provide a plausible route for wallflowers to reach present-day globular cluster configurations.

Where Pith is reading between the lines

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

  • A non-negligible fraction of today's globular clusters may have originated in isolation outside galactic discs.
  • High-redshift kinematic surveys could directly test whether the observed rotation separation persists in real clusters.
  • The distinction raises the question of how filamentary versus disc environments affect the long-term survival and structural evolution of dense stellar systems.

Load-bearing premise

The assumption that differences in rotation and density measured at z~7.6 between the two types will map directly onto present-day globular cluster properties without requiring detailed modeling of later dynamical evolution.

What would settle it

A follow-up simulation or observation demonstrating that low-rotation wallflowers systematically gain rotation or shift in surface density by z=0, erasing the overlap with Milky Way globular clusters.

Figures

Figures reproduced from arXiv: 2606.27426 by Floor van Donkelaar, Lucio Mayer, Pedro R. Capelo.

Figure 2
Figure 2. Figure 2: Stellar 𝑣/𝜎 distributions for CWs (blue) and disc clusters (red) at the final snapshot (𝑧 ∼ 7.6), shown as normalized PDFs (top panel) and CDFs (bottom panel) higher values. This separation is more clearly visible in the cumu￾lative distributions, which show that the CWs population builds up more rapidly at low 𝑣rot [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Rotational coherence as a function of stellar rotational velocity for CWs and disc clusters. From top to bottom, the panels show the gas rotational velocity with the dotted line marking the one-to-one relation, the stellar co￾rotating mass fraction, and the gas co-rotating mass fraction. Solid lines show median trends in bins of stellar 𝑣rot, with shaded regions indicating the 16th– 84th percentile range, … view at source ↗
Figure 4
Figure 4. Figure 4: Stellar kinematic and structural properties of CWs (blue) and disc clusters (red) at 𝑧 ∼ 7.6. Black crosses show local GCs from Sollima et al. (2019); Vasiliev & Baumgardt (2021), where 𝜎 is measured at the stellar half-mass radius. The green triangles show the proto-GCs discussed in van Donkelaar et al. (2023). The top panel shows the stellar 𝑣/𝜎 as a function of stellar rotational velocity, 𝑣rot. The bot… view at source ↗
Figure 5
Figure 5. Figure 5: DF time-scale, 𝜏DF, for CWs split into slow rotators (𝑣rot < 10 km s−1 ) and the remaining CW population. The top panel shows 𝜏DF against rotational velocity, the middle panel shows 𝜏DF against 𝑣/𝜎, and the bottom panel shows the normalized distribution. The dotted vertical lines in the bottom panel show the median values of each sample. (2026). We use the combined gas, stellar, and dark matter density pro… view at source ↗
Figure 6
Figure 6. Figure 6: Gas fraction versus stellar kinematics for CWs (blue) and disc clusters (red) at the final snapshot. The top panel shows the stellar rotation velocity, 𝑣rot, and the bottom panel the rotational support, 𝑣/𝜎, as a function of gas fraction, 𝑓gas. Points indicate individual clusters, whereas the solid lines show the binned median in 𝑓gas, with shaded regions marking the 16th–84th percentile range, and only sh… view at source ↗
read the original abstract

We investigate the rotational properties of star-forming clusters at $z \sim 7.6$ in the high-resolution simulation MassiveBlackPS, focusing on two formation channels: clusters forming in galactic discs via gravitational instability and isolated circumgalactic systems, referred to as cosmic wallflowers, born out of cosmic filaments. Using stellar kinematics, we compare their rotational velocities, $v_{\rm rot}$, and rotational support, $v/\sigma$, to study whether formation environment leaves a clear dynamical imprint. We find a clear separation, wherein cosmic wallflowers systematically have lower rotational velocities and span a wide range in $v/\sigma$, whereas the identified disc clusters are strongly rotation-dominated and extend to higher $v_{\rm rot}$. When combined with stellar surface densities, a subset of the low-$v_{\rm rot}$ cosmic wallflowers lie surprisingly close to the observed globular cluster population in the Milky Way, whereas disc clusters remain offset. Within the cosmic wallflower population, we identify two regimes: lower-density, weakly rotating systems that overlap with these globular cluster properties, and denser, more rotationally supported systems that likely follow a different evolutionary pathway, possibly linking them to the origin of massive black hole seeds at high redshift. We further find that the gas content correlates with this behaviour, with gas-rich cosmic wallflowers preferentially occupying this low-rotation regime. This all suggests that environment and baryonic content together play a key role in setting the initial dynamical state and possible fate of clusters. In particular, weakly rotating, gas-rich cosmic wallflowers emerge as natural proto-globular cluster candidates, potentially evolving towards present-day systems through angular momentum loss and dynamical heating.

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 / 1 minor

Summary. The manuscript analyzes star-forming clusters at z ≈ 7.6 in the MassiveBlackPS high-resolution simulation, distinguishing disc clusters (formed via gravitational instability, strongly rotation-dominated) from isolated 'cosmic wallflowers' (born from filaments, lower v_rot and wider v/σ range). It reports that a gas-rich subset of the low-v_rot wallflowers overlaps the Milky Way globular cluster locus in the (v_rot, stellar surface density) plane, proposing them as proto-GC candidates that could reach local properties via subsequent angular momentum loss and dynamical heating.

Significance. If the results hold, the work supplies a concrete high-redshift formation channel for globular clusters that originates outside galactic discs and ties initial kinematics and gas content to later evolution. The simulation enables a direct kinematic comparison that is difficult to obtain observationally. The reported separation between the two populations is a clear, testable outcome of the analysis.

major comments (2)
  1. [Abstract] Abstract: the claim that low-v_rot, gas-rich wallflowers are proto-globular cluster candidates because their z ≈ 7.6 (v_rot, surface-density) locus overlaps the Milky Way GC population is load-bearing, yet the manuscript supplies no forward integration, orbit-averaged torque estimates, mass-loss timescales, or dynamical-heating calculations to show that the overlap persists to z = 0. The evolutionary pathway is therefore stated as an assumption rather than a demonstrated outcome.
  2. [Cluster classification and measurement section] Cluster classification and measurement section: the criteria used to assign clusters to the disc versus wallflower categories, the number of objects in each sample, and the precise definitions and uncertainties on v_rot and surface density are not stated, preventing assessment of whether the reported separation and overlap are robust to reasonable variations in identification thresholds.
minor comments (1)
  1. The novel term 'cosmic wallflowers' should be defined explicitly on first use and its relation to standard circumgalactic or filamentary structures clarified.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for their constructive and detailed report. We address the two major comments below, clarifying the scope of the present simulation snapshot analysis while committing to improvements in clarity and precision where feasible.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the claim that low-v_rot, gas-rich wallflowers are proto-globular cluster candidates because their z ≈ 7.6 (v_rot, surface-density) locus overlaps the Milky Way GC population is load-bearing, yet the manuscript supplies no forward integration, orbit-averaged torque estimates, mass-loss timescales, or dynamical-heating calculations to show that the overlap persists to z = 0. The evolutionary pathway is therefore stated as an assumption rather than a demonstrated outcome.

    Authors: We agree that the manuscript does not contain forward modeling, torque estimates, or dynamical evolution calculations to z=0, as the analysis is restricted to a single high-resolution snapshot at z≈7.6. The candidacy is proposed on the basis of the direct kinematic and density overlap plus the correlation with gas richness, which we argue provides a plausible initial condition for subsequent angular momentum loss and heating. We will revise the abstract and discussion sections to explicitly frame the result as identifying promising candidates whose properties match the local GC locus at formation, rather than claiming a fully demonstrated evolutionary track. revision: partial

  2. Referee: [Cluster classification and measurement section] Cluster classification and measurement section: the criteria used to assign clusters to the disc versus wallflower categories, the number of objects in each sample, and the precise definitions and uncertainties on v_rot and surface density are not stated, preventing assessment of whether the reported separation and overlap are robust to reasonable variations in identification thresholds.

    Authors: We acknowledge that these methodological details were insufficiently explicit. In the revised manuscript we will add a dedicated subsection (or expanded paragraph) that states the exact classification criteria (including any thresholds on isolation, filament association, and disc membership), reports the final sample sizes for each population, and provides the precise operational definitions of v_rot (including the radius and projection used) together with the measurement uncertainties and surface-density calculation method. revision: yes

standing simulated objections not resolved
  • Forward integration, orbit-averaged torque estimates, mass-loss timescales, or dynamical-heating calculations demonstrating evolution from z≈7.6 to z=0

Circularity Check

0 steps flagged

No significant circularity: claims rest on direct simulation analysis and external observational comparison

full rationale

The paper derives its classification of disc clusters versus cosmic wallflowers from the formation environments identified in the MassiveBlackPS simulation output at z~7.6, then measures v_rot, v/σ, surface density, and gas content directly from the stellar particles. The overlap of a low-v_rot, gas-rich wallflower subset with the Milky Way GC locus is an external comparison to observed data, not a fitted parameter or self-referential definition. No equations redefine quantities in terms of the claimed proto-GC status, no predictions are statistically forced by prior fits, and the evolutionary suggestion (angular momentum loss) is presented as a hypothesis without being used to justify the initial classification. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 1 invented entities

The central claim relies on the simulation's ability to distinguish formation channels and the assumption that low rotation and density match to GCs indicates proto-GC status. No free parameters explicitly mentioned, but simulation parameters are implicit. The new term 'cosmic wallflowers' is introduced without independent evidence outside the simulation.

axioms (1)
  • standard math Standard cosmological model and simulation physics in MassiveBlackPS
    The simulation relies on established cosmological assumptions and hydrodynamics.
invented entities (1)
  • cosmic wallflowers no independent evidence
    purpose: To label isolated circumgalactic star-forming systems born from filaments as distinct from disc clusters
    New term introduced to describe a formation channel identified in the simulation.

pith-pipeline@v0.9.1-grok · 5839 in / 1277 out tokens · 45276 ms · 2026-06-29T02:07:05.109691+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

300 extracted references · 286 canonical work pages · 135 internal anchors

  1. [1]

    , keywords =

    Far and extreme UV radiation feedback in molecular clouds and its influence on the mass and size of star clusters. , keywords =. doi:10.1093/mnras/stac244 , archivePrefix =. 2201.09995 , primaryClass =

    work page doi:10.1093/mnras/stac244

  2. [2]

    , keywords =

    On the ubiquity of extreme baryon concentrations in the early Universe. , keywords =. doi:10.1093/mnrasl/slae101 , archivePrefix =. 2410.22138 , primaryClass =

    work page doi:10.1093/mnrasl/slae101

  3. [3]

    Cosmic wallflowers: the circumgalactic origins of isolated ultra-compact star clusters at $z>7$

    Cosmic wallflowers: the circumgalactic origins of isolated ultra-compact star clusters at z > 7. , keywords =. doi:10.1093/mnras/stag792 , archivePrefix =. 2601.05333 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stag792

  4. [4]

    , keywords =

    Gaia EDR3 view on galactic globular clusters. , keywords =. doi:10.1093/mnras/stab1475 , archivePrefix =. 2102.09568 , primaryClass =

    work page doi:10.1093/mnras/stab1475

  5. [5]

    The eye of Gaia on globular clusters kinematics: internal rotation

    The eye of Gaia on globular clusters kinematics: internal rotation. , keywords =. doi:10.1093/mnras/stz505 , archivePrefix =. 1902.05895 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz505 1902

  6. [6]

    Gas retention and its possible consequences

    Gas in globular clusters ─ I. Gas retention and its possible consequences. , keywords =. doi:10.1093/mnras/staf1925 , archivePrefix =. 2509.02677 , primaryClass =

    work page doi:10.1093/mnras/staf1925

  7. [7]

    Disentangling the independently controllable factors of variation by interacting with the world

    Embedded Clusters in Molecular Clouds. , keywords =. doi:10.1146/annurev.astro.41.011802.094844 , archivePrefix =. astro-ph/0301540 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev.astro.41.011802.094844

  8. [8]

    The Formation and Early Evolution of Young Massive Clusters

    The Formation and Early Evolution of Young Massive Clusters. Protostars and Planets VI , year = 2014, editor =. doi:10.2458/azu_uapress_9780816531240-ch013 , archivePrefix =. 1401.4175 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.2458/azu_uapress_9780816531240-ch013 2014

  9. [9]

    , keywords =

    The dynamics and outcome of star formation with jets, radiation, winds, and supernovae in concert. , keywords =. doi:10.1093/mnras/stac526 , archivePrefix =. 2201.00882 , primaryClass =

    work page doi:10.1093/mnras/stac526

  10. [10]

    D., Piro, A

    Formation and dynamical evolution of multiple stellar generations in globular clusters. , keywords =. doi:10.1111/j.1365-2966.2008.13915.x , archivePrefix =. 0809.1438 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.13915.x 2008

  11. [11]

    , keywords =

    Exploring the fate of primordial discs in Milky Way-sized galaxies with the GigaEris simulation. , keywords =. doi:10.1093/mnras/staf597 , archivePrefix =. 2406.11960 , primaryClass =

    work page doi:10.1093/mnras/staf597

  12. [12]

    On the Formation of Multiple Stellar Populations in Globular Clusters

    On the Formation of Multiple Stellar Populations in Globular Clusters. , keywords =. doi:10.1088/0004-637X/726/1/36 , archivePrefix =. 1005.4934 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/726/1/36

  13. [13]

    Multiple Stellar Populations in Globular Clusters

    Multiple Stellar Populations in Globular Clusters. , keywords =. doi:10.1146/annurev-astro-081817-051839 , archivePrefix =. 1712.01286 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-081817-051839

  14. [14]

    C.\ 2013, , 51, 511, doi:10.1146/annurev-astro-082708-101811

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

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

  15. [15]

    B., et al

    The first billion years according to JWST. Nature Astronomy , keywords =. doi:10.1038/s41550-025-02624-5 , archivePrefix =. 2405.21054 , primaryClass =

    work page doi:10.1038/s41550-025-02624-5

  16. [16]

    , keywords =

    Star Clusters Near and Far; Tracing Star Formation Across Cosmic Time. , keywords =. doi:10.1007/s11214-020-00690-x , archivePrefix =. 2005.06188 , primaryClass =

    work page doi:10.1007/s11214-020-00690-x 2005

  17. [17]

    A Fundamental Relation Between Supermassive Black Holes and Their Host Galaxies

    A Fundamental Relation between Supermassive Black Holes and Their Host Galaxies. , keywords =. doi:10.1086/312838 , archivePrefix =. astro-ph/0006053 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/312838

  18. [18]

    Direct N-body and Monte Carlo simulations of dense star clusters

    Rapid formation of a very massive star >50000 M_ and subsequently an IMBH from runaway collisions. Direct N-body and Monte Carlo simulations of dense star clusters. arXiv e-prints , keywords =. doi:10.48550/arXiv.2505.07491 , archivePrefix =. 2505.07491 , primaryClass =

    work page doi:10.48550/arxiv.2505.07491

  19. [19]

    Seeding High Redshift QSOs by Collisional Runaway in Primordial Star Clusters

    Seeding high-redshift QSOs by collisional runaway in primordial star clusters. , keywords =. doi:10.1093/mnras/stv1048 , archivePrefix =. 1502.03448 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv1048

  20. [20]

    , keywords =

    Detailed study of the Milky Way globular cluster Laevens 3. , keywords =. doi:10.1093/mnras/stz2592 , archivePrefix =. 1909.08622 , primaryClass =

    work page doi:10.1093/mnras/stz2592 1909

  21. [21]

    The observed properties of dwarf galaxies in and around the Local Group

    The Observed Properties of Dwarf Galaxies in and around the Local Group. , keywords =. doi:10.1088/0004-6256/144/1/4 , archivePrefix =. 1204.1562 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/144/1/4

  22. [22]

    A New Milky Way Companion: Unusual Globular Cluster or Extreme Dwarf Satellite?

    A New Milky Way Companion: Unusual Globular Cluster or Extreme Dwarf Satellite?. , keywords =. doi:10.1086/430214 , archivePrefix =. astro-ph/0410416 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/430214

  23. [23]

    The slope of the black-hole mass versus velocity dispersion correlation

    The Slope of the Black Hole Mass versus Velocity Dispersion Correlation. , keywords =. doi:10.1086/341002 , archivePrefix =. astro-ph/0203468 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/341002

  24. [24]

    Measuring Distance and Properties of the Milky Way's Central Supermassive Black Hole with Stellar Orbits

    Measuring Distance and Properties of the Milky Way's Central Supermassive Black Hole with Stellar Orbits. , keywords =. doi:10.1086/592738 , archivePrefix =. 0808.2870 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/592738

  25. [25]

    Cold flows and the first quasars

    Cold Flows and the First Quasars. , keywords =. doi:10.1088/2041-8205/745/2/L29 , archivePrefix =. 1107.1253 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/745/2/l29 2041

  26. [26]

    High redshift supermassive blackholes: accretion through cold flows

    High-redshift supermassive black holes: accretion through cold flows. , keywords =. doi:10.1093/mnras/stu432 , archivePrefix =. 1312.1391 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu432

  27. [27]

    , keywords =

    Resolution requirements for smoothed particle hydrodynamics calculations with self-gravity. , keywords =. doi:10.1093/mnras/288.4.1060 , adsurl =

    work page doi:10.1093/mnras/288.4.1060

  28. [28]

    Orbital Decay of Supermassive Black Hole Binaries in Clumpy Multiphase Merger Remnants

    Orbital decay of supermassive black hole binaries in clumpy multiphase merger remnants. , keywords =. doi:10.1093/mnras/stv312 , archivePrefix =. 1406.4505 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv312

  29. [29]

    The Galactic Center Massive Black Hole and Nuclear Star Cluster

    The Galactic Center massive black hole and nuclear star cluster. Reviews of Modern Physics , keywords =. doi:10.1103/RevModPhys.82.3121 , archivePrefix =. 1006.0064 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/revmodphys.82.3121

  30. [30]

    The Mass Distribution of Stellar-Mass Black Holes

    The Mass Distribution of Stellar-mass Black Holes. , keywords =. doi:10.1088/0004-637X/741/2/103 , archivePrefix =. 1011.1459 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/741/2/103

  31. [31]

    Counting Black Holes: The Cosmic Stellar Remnant Population and Implications for LIGO

    Counting black holes: The cosmic stellar remnant population and implications for LIGO. , keywords =. doi:10.1093/mnras/stx1959 , archivePrefix =. 1703.02551 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1959

  32. [32]

    J., & Zanotti, O

    On the formation and evolution of black hole binaries. , keywords =. doi:10.1046/j.1365-8711.2003.06464.x , archivePrefix =. astro-ph/0207153 , primaryClass =

    work page doi:10.1046/j.1365-8711.2003.06464.x 2003

  33. [33]

    and Strader, Jay and Ho, Luis C

    Intermediate-Mass Black Holes. , keywords =. doi:10.1146/annurev-astro-032620-021835 , archivePrefix =. 1911.09678 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-astro-032620-021835 1911

  34. [34]

    X-ray emission from active galactic nuclei with intermediate mass black holes

    X-Ray Emission from Active Galactic Nuclei with Intermediate-Mass Black Holes. , keywords =. doi:10.1086/591728 , archivePrefix =. 0801.3663 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/591728

  35. [35]

    D., Piro, A

    The XMM -Newton view of AGN with intermediate-mass black holes. , keywords =. doi:10.1111/j.1365-2966.2008.14334.x , archivePrefix =. 0812.1652 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.14334.x 2008

  36. [36]

    A New Sample of Candidate Intermediate-Mass Black Holes Selected by X-ray Variability

    A New Sample of Candidate Intermediate-mass Black Holes Selected by X-Ray Variability. , keywords =. doi:10.1088/0004-637X/751/1/39 , archivePrefix =. 1205.2772 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/751/1/39

  37. [37]

    The search for active black holes in nearby low-mass galaxies using optical and mid-IR data

    The search for active black holes in nearby low-mass galaxies using optical and mid-IR data. , keywords =. doi:10.1093/mnras/stv2238 , archivePrefix =. 1509.08483 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv2238

  38. [38]

    , keywords =

    A New Sample of (Wandering) Massive Black Holes in Dwarf Galaxies from High-resolution Radio Observations. , keywords =. doi:10.3847/1538-4357/ab4999 , archivePrefix =. 1909.04670 , primaryClass =

    work page doi:10.3847/1538-4357/ab4999 1909

  39. [39]

    An actively accreting massive black hole in the dwarf starburst galaxy Henize 2-10

    An actively accreting massive black hole in the dwarf starburst galaxy Henize2-10. , keywords =. doi:10.1038/nature09724 , archivePrefix =. 1101.1309 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature09724

  40. [40]

    , keywords =

    The origins of off-centre massive black holes in dwarf galaxies. , keywords =. doi:10.1093/mnras/stab1665 , archivePrefix =. 2102.09566 , primaryClass =

    work page doi:10.1093/mnras/stab1665

  41. [41]

    Multimessenger Signatures of Massive Black Holes in Dwarf Galaxies

    Multimessenger signatures of massive black holes in dwarf galaxies. , keywords =. doi:10.1093/mnras/sty2842 , archivePrefix =. 1806.00471 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2842

  42. [42]

    , keywords =

    Kraken reveals itself - the merger history of the Milky Way reconstructed with the E-MOSAICS simulations. , keywords =. doi:10.1093/mnras/staa2452 , archivePrefix =. 2003.01119 , primaryClass =

    work page doi:10.1093/mnras/staa2452 2003

  43. [43]

    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

  44. [44]

    Characterizing the velocity of a wandering black hole and properties of the surrounding medium using convolutional neural networks

    Characterizing the velocity of a wandering black hole and properties of the surrounding medium using convolutional neural networks. , keywords =. doi:10.1103/PhysRevD.97.063001 , archivePrefix =. 1803.06060 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.97.063001

  45. [45]

    Wandering Supermassive Black Holes in Milky Way Mass Halos

    Wandering Supermassive Black Holes in Milky-Way-mass Halos. , keywords =. doi:10.3847/2041-8213/aabc0a , archivePrefix =. 1802.06783 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aabc0a 2041

  46. [46]

    , keywords =

    A Search for Wandering Black Holes in the Milky Way with Gaia and DECaLS. , keywords =. doi:10.3847/1538-4357/ac0896 , archivePrefix =. 2105.04581 , primaryClass =

    work page doi:10.3847/1538-4357/ac0896

  47. [47]

    , keywords =

    Unveiling the Population of Wandering Black Holes via Electromagnetic Signatures. , keywords =. doi:10.3847/2041-8213/ac1170 , archivePrefix =. 2107.02132 , primaryClass =

    work page doi:10.3847/2041-8213/ac1170 2041

  48. [48]

    , keywords =

    Detectability of wandering intermediate-mass black holes in the Milky Way galaxy from radio to x-rays. , keywords =. doi:10.1093/mnras/stac1928 , archivePrefix =. 2204.12498 , primaryClass =

    work page doi:10.1093/mnras/stac1928

  49. [49]

    The impact of radiation on dwarf galaxies and their circumgalactic medium

    The Seven Dwarfs illuminated. The impact of radiation on dwarf galaxies and their circumgalactic medium. arXiv e-prints , keywords =. doi:10.48550/arXiv.2508.19396 , archivePrefix =. 2508.19396 , primaryClass =

    work page doi:10.48550/arxiv.2508.19396

  50. [50]

    , keywords =

    A Massive Black Hole 0.8 kpc from the Host Nucleus Revealed by the Offset Tidal Disruption Event AT2024tvd. , keywords =. doi:10.3847/2041-8213/add7de , archivePrefix =. 2502.17661 , primaryClass =

    work page doi:10.3847/2041-8213/add7de 2041

  51. [51]

    A luminous X-ray outburst from an intermediate-mass black hole in an off-centre star cluster

    A luminous X-ray outburst from an intermediate-mass black hole in an off-centre star cluster. Nature Astronomy , keywords =. doi:10.1038/s41550-018-0493-1 , archivePrefix =. 1806.05692 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-018-0493-1

  52. [52]

    , keywords =

    Dynamics of intermediate-mass black holes wandering in the milky way galaxy using the illustris TNG50 simulation. , keywords =. doi:10.1093/mnras/stac179 , archivePrefix =. 2201.07234 , primaryClass =

    work page doi:10.1093/mnras/stac179

  53. [53]

    , keywords =

    A vast population of wandering and merging IMBHs at cosmic noon. , keywords =. doi:10.1093/mnras/stad2198 , archivePrefix =. 2210.14960 , primaryClass =

    work page doi:10.1093/mnras/stad2198

  54. [54]

    , keywords =

    Orbital and radiative properties of wandering intermediate-mass black holes in the ASTRID simulation. , keywords =. doi:10.1093/mnras/stad347 , archivePrefix =. 2210.16319 , primaryClass =

    work page doi:10.1093/mnras/stad347

  55. [55]

    Observational evidence for intermediate-mass black holes

    Observational evidence for intermediate-mass black holes. International Journal of Modern Physics D , keywords =. doi:10.1142/S021827181730021X , archivePrefix =. 1705.09667 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1142/s021827181730021x

  56. [56]

    Nature Astronomy , keywords =

    Primordial rotating disk composed of at least 15 dense star-forming clumps at cosmic dawn. Nature Astronomy , keywords =. doi:10.1038/s41550-025-02592-w , archivePrefix =. 2402.18543 , primaryClass =

    work page doi:10.1038/s41550-025-02592-w

  57. [57]

    The James Webb Space Telescope

    The James Webb Space Telescope. , keywords =. doi:10.1007/s11214-006-8315-7 , archivePrefix =. astro-ph/0606175 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s11214-006-8315-7

  58. [58]

    , keywords =

    Formation of a low-mass galaxy from star clusters in a 600-million-year-old Universe. , keywords =. doi:10.1038/s41586-024-08293-0 , archivePrefix =. 2402.08696 , primaryClass =

    work page doi:10.1038/s41586-024-08293-0

  59. [59]

    , keywords =

    Bound star clusters observed in a lensed galaxy 460 Myr after the Big Bang. , keywords =. doi:10.1038/s41586-024-07703-7 , archivePrefix =. 2401.03224 , primaryClass =

    work page doi:10.1038/s41586-024-07703-7

  60. [60]

    , keywords =

    The First Stars. , keywords =. doi:10.1146/annurev.astro.42.053102.134034 , archivePrefix =. astro-ph/0311019 , primaryClass =

    work page doi:10.1146/annurev.astro.42.053102.134034

  61. [61]

    The Romulus Cosmological Simulations: A Physical Approach to the Formation, Dynamics and Accretion Models of SMBHs

    The Romulus cosmological simulations: a physical approach to the formation, dynamics and accretion models of SMBHs. , keywords =. doi:10.1093/mnras/stx1160 , archivePrefix =. 1607.02151 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1160

  62. [62]

    Clumpy Galaxies in CANDELS. I. The Definition of UV Clumps and the Fraction of Clumpy Galaxies at 0.5 < z < 3. , keywords =. doi:10.1088/0004-637X/800/1/39 , archivePrefix =. 1410.7398 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/800/1/39

  63. [63]

    Reports on Progress in Physics , abstract =

    Volker Bromm , title =. Reports on Progress in Physics , abstract =. 2013 , month =. doi:10.1088/0034-4885/76/11/112901 , url =

    work page doi:10.1088/0034-4885/76/11/112901 2013

  64. [64]

    First stars, very massive black holes and metals

    First Stars, Very Massive Black Holes, and Metals. , keywords =. doi:10.1086/339917 , archivePrefix =. astro-ph/0111341 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/339917

  65. [65]

    One Hundred First Stars : Protostellar Evolution and the Final Masses

    One Hundred First Stars: Protostellar Evolution and the Final Masses. , keywords =. doi:10.1088/0004-637X/781/2/60 , archivePrefix =. 1308.4456 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/781/2/60

  66. [66]

    , keywords =

    The evolution and fate of Very Massive Objects. , keywords =. doi:10.1086/162057 , adsurl =

    work page doi:10.1086/162057

  67. [67]

    The Nucleosynthetic Signature of Population III

    The Nucleosynthetic Signature of Population III. , keywords =. doi:10.1086/338487 , archivePrefix =. astro-ph/0107037 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/338487

  68. [68]

    First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star

    First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star. , keywords =. doi:10.1038/nature01571 , archivePrefix =. astro-ph/0301315 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature01571

  69. [69]

    The Formation of the First Star in the Universe

    The Formation of the First Star in the Universe. Science , keywords =. doi:10.1126/science.295.5552.93 , archivePrefix =. astro-ph/0112088 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1126/science.295.5552.93

  70. [70]

    Collapse of Primordial Gas Clouds and the Formation of Quasar Black Holes

    Collapse of Primordial Gas Clouds and the Formation of Quasar Black Holes. , keywords =. doi:10.1086/174548 , archivePrefix =. astro-ph/9401026 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/174548

  71. [71]

    Origin of Quasar Progenitors from the Collapse of Low-Spin Cosmological Perturbations

    Origin of Quasar Progenitors from the Collapse of Low-Spin Cosmological Perturbations. , keywords =. doi:10.1086/175498 , archivePrefix =. astro-ph/9401016 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/175498

  72. [72]

    Formation of the First Supermassive Black Holes

    Formation of the First Supermassive Black Holes. , keywords =. doi:10.1086/377529 , archivePrefix =. astro-ph/0212400 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/377529

  73. [73]

    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

  74. [74]

    The runaway growth of intermediate-mass black holes in dense star clusters

    The Runaway Growth of Intermediate-Mass Black Holes in Dense Star Clusters. , keywords =. doi:10.1086/341798 , archivePrefix =. astro-ph/0201055 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/341798

  75. [75]

    Massive black hole binaries from runaway collisions: the impact of metallicity

    Massive black hole binaries from runaway collisions: the impact of metallicity. , keywords =. doi:10.1093/mnras/stw869 , archivePrefix =. 1604.03559 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw869

  76. [76]

    Star cluster ecology. III. Runaway collisions in young compact star clusters. , keywords =

  77. [77]

    The formation of massive black holes through collision runaway in dense young star clusters

    Formation of massive black holes through runaway collisions in dense young star clusters. , keywords =. doi:10.1038/nature02448 , archivePrefix =. astro-ph/0402622 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature02448

  78. [78]

    Can Supermassive Black Holes Form in Metal-Enriched High-Redshift Protogalaxies ?

    Can Supermassive Black Holes Form in Metal-enriched High-Redshift Protogalaxies?. , keywords =. doi:10.1086/591636 , archivePrefix =. 0804.3141 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/591636

  79. [79]

    R., Quirion, P

    High-redshift formation and evolution of central massive objects - I. Model description. , keywords =. doi:10.1111/j.1365-2966.2010.17363.x , archivePrefix =. 1001.3874 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17363.x 2010

  80. [80]

    D’Avanzo, et al., A complete sample of bright Swift Gamma-Ray Bursts: X-ray afterglow luminosity and its correlation with the prompt emission

    High-redshift formation and evolution of central massive objects - II. The census of BH seeds. , keywords =. doi:10.1111/j.1365-2966.2012.20406.x , archivePrefix =. 1201.3761 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.20406.x 2012

Showing first 80 references.