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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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