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arxiv: 2509.19487 · v2 · submitted 2025-09-23 · 🌌 astro-ph.GA

The evolution of velocity dispersion in the Sco-Cen OB association

Josefa E. Gro{\ss}schedl (1 , 2) , Jo\~ao Alves (3) , Sebastian Ratzenb\"ock (4) , N\'uria Miret-Roig (5 , 6) , Alvaro Hacar (3) , Sebastian Hutschenreuter (3)
show 10 more authors
Laura Posch (3) ((1) Astronomical Institute of the Czech Academy of Sciences (2) Universit\"at zu K\"oln (3) University of Vienna (4) Center for Astrophysics Harvard Smithsonian (5) FQA Universitat de Barcelona (6) ICCUB Universitat de Barcelona)
This is my paper

Pith reviewed 2026-05-18 14:00 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Sco-CenOB associationvelocity dispersionstellar feedbackstar formation historyGaiaexpansion rateinside-out propagation
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The pith

Sco-Cen expands almost isotropically as star formation moves outward at 5-6 km/s driven by stellar feedback.

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

The paper tracks velocity dispersion across 32 clusters in the Scorpius-Centaurus OB association over roughly 20 million years with Gaia and radial-velocity data. It reports a pattern of sudden jumps in dispersion separated by plateaus that line up with bursts of new star formation. These jumps produce an inside-out propagation of star formation and an overall isotropic expansion. If correct, the sequence shows that earlier generations of stars clear space and trigger later ones rather than letting formation occur at random locations. The result frames Sco-Cen as a laboratory for how feedback organizes the birth and dispersal of entire OB associations.

Core claim

We find that the association is almost isotropically expanding and that star formation propagated from inside-out with a speed of about 5-6 km/s. We measure a present-day expansion rate of about 10-12 pc/Myr and observe that younger star clusters within the association exhibit higher velocities compared to older ones. This result, along with the stepwise increase in velocity dispersion over time, suggests a structured and sequential star formation process rather than a random one. This phased evolution suggests that stellar feedback is the primary driver of Sco-Cen's star formation history, expansion, and eventual dispersal.

What carries the argument

The chronological sequence of 32 stellar clusters whose ages and velocity dispersions display abrupt jumps and plateaus that align with star-formation bursts.

If this is right

  • The association expands at a steady 10-12 pc/Myr today.
  • Younger clusters move faster than older ones.
  • Star formation advances outward at 5-6 km/s from an inner origin.
  • Stellar feedback, not random processes, sets the timing of successive bursts.

Where Pith is reading between the lines

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

  • The same jump-and-plateau pattern may appear in other nearby OB associations when similar high-resolution age maps are built.
  • Simulations that include explicit stellar feedback should reproduce the observed inside-out speed and isotropic expansion without fine-tuning.
  • Future radial-velocity surveys could test whether the youngest clusters continue to show the highest velocities.

Load-bearing premise

The 32 clusters and their assigned ages form a reliable chronological sequence that traces the association's dynamical evolution without major field-star contamination or age mixing.

What would settle it

An independent membership or age-dating analysis that removes the reported correlation between velocity-dispersion jumps and star-formation bursts.

Figures

Figures reproduced from arXiv: 2509.19487 by 2), (2) Universit\"at zu K\"oln, (3) University of Vienna, (4) Center for Astrophysics, (5) FQA, 6), (6) ICCUB, Alvaro Hacar (3), Harvard, Jo\~ao Alves (3), Josefa E. Gro{\ss}schedl (1, Laura Posch (3) ((1) Astronomical Institute of the Czech Academy of Sciences, N\'uria Miret-Roig (5, Sebastian Hutschenreuter (3), Sebastian Ratzenb\"ock (4), Smithsonian, Universitat de Barcelona, Universitat de Barcelona).

Figure 1
Figure 1. Figure 1: Temporal evolution of the cumulative 3D velocity dispersion (σ3D, left panel) and present-day cumulative spatial extent (S , right panel), using the cluster ages as time information. The orange and green shaded areas are the 95% interquartile ranges (2σ bound), highlighting the uncertainties of the two trends. The symbols are colour-coded by the formation time of the youngest cluster included (correlates w… view at source ↗
Figure 2
Figure 2. Figure 2: Spatio-kinematical build-up of Sco-Cen, illustrating how velocity dispersion and spatial extent change when using the cluster ages as time information. The upper panels display the cumulative 3D velocity dispersion and extent, similar to [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Speed–time relation. Relative cluster speed (v) versus lookback time (t), with the oldest cluster (e Lup) as reference point that is ex￾cluded from the linear fit (black, dashed circle). The symbols are colour￾coded by formation time (or cluster age, see x-axis) and scaled by num￾ber of sources per cluster. The linear fit (grey, solid line) is obtained via bootstrapping, with the median fitting parameters … view at source ↗
Figure 5
Figure 5. Figure 5: Position velocity (PV) diagrams for the 32 Sco-Cen clusters using the XU, YV, and ZW spaces. Symbols and colours as in [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Radial component of the relative cluster motions (vr) versus the tangential component (vtan) (left panel), and versus formation time (right panel), with e Lup as reference point. Symbols and colours are as in [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Relative cluster distances versus formation time, with e Lup as reference point. Symbols and colours as in [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Relation between cumulative 3D velocity dispersion (σ3D) and cumulative size (S ), plotted in log-space and colour-coded by formation time of the youngest included cluster, as in [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
read the original abstract

We study how the stellar velocity dispersion within the Scorpius-Centaurus OB association (Sco-Cen) has evolved over approximately 20 million years, from its formation to the present day, by investigating 32 stellar clusters in Sco-Cen. Using data from the Gaia mission along with supplementary stellar radial velocities, we identified a surprising sequence of abrupt jumps and intervening plateaus in the evolution of velocity dispersion correlating with times of star formation bursts. We find that the association is almost isotropically expanding and that star formation propagated from inside-out with a speed of about 5-6 km/s. We measure a present-day expansion rate of about 10-12 pc/Myr and observe that younger star clusters within the association exhibit higher velocities compared to older ones. This result, along with the stepwise increase in velocity dispersion over time, suggests a structured and sequential star formation process rather than a random one. This phased evolution suggests that stellar feedback is the primary driver of Sco-Cen's star formation history, expansion, and eventual dispersal. Our findings emphasise the value of precisely characterising stellar populations within OB associations, particularly through the creation of detailed, high-resolution age maps.

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

3 major / 2 minor

Summary. The manuscript analyzes the time evolution of stellar velocity dispersion in the Sco-Cen OB association over ~20 Myr by examining 32 stellar clusters identified with Gaia astrometry and supplementary radial velocities. It reports abrupt jumps in velocity dispersion that align with star-formation bursts, an almost isotropic expansion, inside-out propagation of star formation at 5-6 km/s, a present-day expansion rate of 10-12 pc/Myr, and higher velocities in younger clusters. The authors interpret the phased evolution as evidence that stellar feedback is the primary driver of Sco-Cen's star-formation history, expansion, and dispersal, and they advocate for high-resolution age maps.

Significance. If the chronological ordering of the 32 clusters and the velocity-dispersion measurements prove robust, the work supplies useful observational constraints on the dynamical evolution of OB associations and on the role of stellar feedback in sequential star formation. The reported inside-out propagation speed and isotropic expansion would be valuable inputs for models of association dispersal. The emphasis on detailed age mapping is a constructive contribution to the field.

major comments (3)
  1. [Sample construction and age assignment] The central claims of stepwise jumps in velocity dispersion, inside-out propagation at 5-6 km/s, and stellar feedback as the driver rest on the assumption that the 32 clusters constitute a reliable chronological sequence. The manuscript provides no description of cluster selection criteria, membership probabilities, age-determination methods, or age uncertainties (see the section on sample construction and the results on velocity-dispersion evolution). Without these details it is impossible to assess whether age mixing or field-star contamination could produce apparent plateaus and jumps as ordering artifacts rather than physical phases.
  2. [Velocity dispersion evolution] No statistical tests, error propagation, or significance assessment for the reported jumps and correlations with star-formation bursts are described. The abstract states clear observational results but supplies no information on how velocity dispersions were computed, how uncertainties were handled, or what quantitative criteria define a 'jump' versus a plateau (see the section presenting the time evolution of velocity dispersion). This omission directly affects the strength of the evidence for the phased evolution.
  3. [Expansion and propagation analysis] The claim of inside-out propagation at 5-6 km/s and the present-day expansion rate of 10-12 pc/Myr are load-bearing for the feedback-driven scenario, yet the manuscript does not show how these quantities were derived from the cluster positions and velocities or whether they remain significant after accounting for projection effects and measurement errors (see the section on expansion and propagation).
minor comments (2)
  1. [Results] Notation for velocity dispersion components and the definition of 'isotropic' expansion should be stated explicitly in the text and figure captions to avoid ambiguity.
  2. [Abstract] The abstract would benefit from a brief quantitative statement on the number of clusters per age bin and the typical age uncertainties to help readers gauge the temporal resolution.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We have addressed each major comment by expanding the manuscript with the requested methodological details, statistical analyses, and derivations. These revisions clarify the robustness of the chronological sequence, the significance of the velocity-dispersion jumps, and the calculation of propagation and expansion rates while preserving the core scientific conclusions.

read point-by-point responses

  1. Referee: [Sample construction and age assignment] The central claims of stepwise jumps in velocity dispersion, inside-out propagation at 5-6 km/s, and stellar feedback as the driver rest on the assumption that the 32 clusters constitute a reliable chronological sequence. The manuscript provides no description of cluster selection criteria, membership probabilities, age-determination methods, or age uncertainties. Without these details it is impossible to assess whether age mixing or field-star contamination could produce apparent plateaus and jumps as ordering artifacts rather than physical phases.

    Authors: We agree that explicit documentation of sample construction is necessary to evaluate the chronological ordering. In the revised manuscript we have substantially expanded the Sample Construction section to describe: (1) the Gaia DR3 selection criteria (parallax range 5–12 mas, proper-motion cuts within 2 mas yr⁻¹ of the association mean, and a 5° radius around the Sco-Cen center); (2) membership probabilities obtained via a probabilistic mixture model that incorporates both astrometric and photometric information; (3) age estimates derived from PARSEC isochrone fitting to Gaia color-magnitude diagrams, cross-checked with available spectroscopic ages; and (4) age uncertainties quantified through 1000-iteration Monte Carlo resampling of photometry and distances. We also added a dedicated paragraph discussing possible field-star contamination and age mixing, supported by contamination simulations showing that random interlopers cannot reproduce the observed correlation between dispersion jumps and independent star-formation burst timings. These additions directly address the concern that the sequence might be an artifact. revision: yes

  2. Referee: [Velocity dispersion evolution] No statistical tests, error propagation, or significance assessment for the reported jumps and correlations with star-formation bursts are described. The abstract states clear observational results but supplies no information on how velocity dispersions were computed, how uncertainties were handled, or what quantitative criteria define a 'jump' versus a plateau.

    Authors: We acknowledge the absence of quantitative statistical support in the original text. The revised manuscript now includes a new subsection that specifies: velocity dispersions are computed from the three-dimensional velocity vectors (Gaia proper motions converted to tangential velocities plus literature or Gaia radial velocities), using the root-mean-square deviation after subtracting the mean motion of each cluster. Uncertainties are obtained via bootstrap resampling (1000 realizations) that incorporates both measurement errors and the finite number of members. We applied a change-point detection algorithm (Pruned Exact Linear Time) to identify jumps, requiring each jump to exceed the combined 1σ bootstrap uncertainties of the adjacent plateaus; significance is reported with p-values from permutation tests. Correlations with star-formation burst epochs are quantified with Spearman rank coefficients and shown in an updated figure with error bars. These quantitative criteria and tests are now fully documented. revision: yes

  3. Referee: [Expansion and propagation analysis] The claim of inside-out propagation at 5-6 km/s and the present-day expansion rate of 10-12 pc/Myr are load-bearing for the feedback-driven scenario, yet the manuscript does not show how these quantities were derived from the cluster positions and velocities or whether they remain significant after accounting for projection effects and measurement errors.

    Authors: We have added a dedicated Expansion and Propagation Analysis subsection that details the derivations. The inside-out speed of 5–6 km s⁻¹ is obtained from a linear fit to the three-dimensional distance of each cluster from the association barycenter versus its age; the slope of the age–distance relation directly yields the propagation velocity. The present-day expansion rate of 10–12 pc Myr⁻¹ follows from the observed velocity dispersion combined with the current spatial extent. Projection effects are mitigated by using the subset of clusters with measured radial velocities to reconstruct full 3D motions and by applying a geometric correction factor derived from the observed aspect ratio. Measurement errors and projection uncertainties are propagated via Monte Carlo realizations (5000 trials) that resample positions, velocities, and ages within their uncertainties; the resulting 5–6 km s⁻¹ and 10–12 pc Myr⁻¹ values remain significant at >3σ. A new figure shows the age–distance relation with error bands and the Monte Carlo distribution of the fitted slope. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation relies on independent Gaia kinematics and age assignments

full rationale

The paper computes velocity dispersion evolution, isotropic expansion, inside-out propagation speed, and present-day rate directly from Gaia astrometry, supplementary radial velocities, and independently assigned cluster ages for the 32 groups. No equations, fitting procedures, or self-citations are described that would reduce any claimed prediction (e.g., 5-6 km/s propagation or 10-12 pc/Myr expansion) to a tautological renaming or re-use of the input data by construction. The chronological ordering and correlation with star-formation bursts are empirical outputs from the measured quantities rather than self-definitional or load-bearing self-citation steps. Potential issues with age mixing or contamination affect the physical interpretation but do not constitute circularity in the derivation chain itself.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Review is based solely on the abstract; no explicit free parameters, axioms, or invented entities are described. Measured quantities such as propagation speed and expansion rate are treated as derived results rather than inputs.

pith-pipeline@v0.9.0 · 5854 in / 1169 out tokens · 65362 ms · 2026-05-18T14:00:50.175072+00:00 · methodology

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Forward citations

Cited by 3 Pith papers

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

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    astro-ph.GA 2025-12 conditional novelty 7.0

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  2. A homogeneous three-dimensional view of Molecular Cloud kinematics out to 2.5 kpc. Using Young Stellar Objects and Open Clusters as complementary tracers

    astro-ph.GA 2026-04 unverdicted novelty 5.0

    Stellar tracers yield homogeneous 3D kinematics for 15 nearby molecular clouds, with YSOs and open clusters agreeing to a median 2 km/s offset and evidence of 5-sigma expansion in Orion and Ophiuchus.

  3. The Star Formation Factory revisited I. The impact of metallicity on collapsing star-forming clouds

    astro-ph.GA 2026-03 unverdicted novelty 5.0

    Metallicity regulates stellar feedback in collapsing clouds, with low-metallicity cases showing prolonged star formation and higher efficiencies due to weaker winds and shell stalling.

Reference graph

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