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arxiv: 2512.05854 · v2 · pith:FBHI3MCQnew · submitted 2025-12-05 · 🌌 astro-ph.GA · astro-ph.SR

A new Gaia census of OB associations within 1 kpc

Alexis L. Quintana , Nicholas J. Wright , Lilly A. Kormann , Jo\~ao Alves , David Katz , Laia Casamiquela , Paola Di Matteo , Misha Haywood
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Chervin Laporte
This is my paper

Pith reviewed 2026-05-17 00:43 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR
keywords OB associationsGaia astrometrystar formationMilky Way structurestellar clusteringOB starsgalactic kinematicsyoung stellar groups
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The pith

Using Gaia astrometry on 25,000 O- and B-type stars, a new census identifies 56 OB associations within 1 kpc, doubling the known count.

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

The paper aims to establish a more complete and reliable list of OB associations near the Sun by using precise data from the Gaia mission on massive stars. OB associations are the loose collections of young hot stars that mark where stars have recently formed and help outline the structure of the Milky Way. The authors apply a clustering technique to group about 25,000 O- and B-type stars within 1,000 light-years into 56 associations. This more than doubles the number of such groups known in the local volume. They validate the groups by matching members to previous lists and describe the groups' masses, motions, and expansion rates, linking some to larger galactic features.

Core claim

We exploit a complete census of ∼25,000 O- and B-type stars within 1 kpc of the Sun to produce a highly-reliable catalogue of 56 OB associations using the HDBSCAN clustering algorithm, increasing the number of known OB associations by a factor of two within this volume. We assess the validity of this catalogue by crossmatching our OB association members with other catalogues of OB associations, star clusters and young stellar groups, confirming the high-confidence of our census of OB associations. We characterize these OB associations physically (total initial stellar mass, number of OB stars, ...) and kinematically (velocity dispersion, linear expansion ages, ...). The majority of the OB (

What carries the argument

The HDBSCAN density-based clustering algorithm applied to Gaia astrometric data of O- and B-type stars to group them into physical associations.

Load-bearing premise

The chosen HDBSCAN parameters and cross-matching procedure reliably separate true physical OB associations from chance alignments or unrelated stars.

What would settle it

Detailed radial-velocity or age measurements showing that a large fraction of stars assigned to the associations have velocities or properties inconsistent with membership in the same physical group.

Figures

Figures reproduced from arXiv: 2512.05854 by Alexis L. Quintana, Chervin Laporte, David Katz, Jo\~ao Alves, Laia Casamiquela, Lilly A. Kormann, Misha Haywood, Nicholas J. Wright, Paola Di Matteo.

Figure 1
Figure 1. Figure 1: Galactic Cartesian coordinates of the 57 new OB associations, centered on the Sun’s position. On the top panel have been labeled each OB association, displayed on top of the background extinction map from Edenhofer et al. (2024). The colours used for each association are the same between panels. MNRAS 000, 1–17 (2025) [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Transverse velocity distribution of the 57 new OB associations within 1 kpc. The colours used for each association are the same as in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: for Ori OB1b, which exhibits a significant expansion pattern along the Galactic longitude direction. We find that 41 out of our 57 OB associations, hence the majority of our catalogue (∼75 %), exhibit a significant (> 1𝜎) expansion pattern in at least one direction, including 9 expanding in both directions, to be compared with ∼94 % of the 18 stellar groups in Wright et al. (2024) (that includes star clust… view at source ↗
Figure 4
Figure 4. Figure 4: Same as the top panel from [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: 2D projection on the Z/Y’ plane of the four other superclouds from Kormann et al. (2025) within 1 kpc, rotated clockwise, with the OB associations displayed on top and rotated with the same angle. The location of the Sun is indicated with the corresponding symbol, using 𝑍⊙ = 20.8 ± 0.3 pc from Bennett & Bovy (2019). Vela OB4 and Vela OB6) occupy the centre of the largest cloud. However, only Vela OB6 appea… view at source ↗
read the original abstract

OB associations are primordial tracers of star formation and Galactic structure. Originally defined about 80 years ago, their historical membership lists have been superseded thanks to the precise astrometry from ESA's \textit{Gaia}'s satellite. Recent studies have however been mostly focused on individual OB associations or limited by the coverage of spectroscopic surveys. In this paper, we exploit a complete census of $\sim$25,000 O- and B-type stars within 1 kpc of the Sun to produce a highly-reliable catalogue of 56 OB associations using the HDBSCAN clustering algorithm, increasing the number of known OB associations by a factor of two within this volume. We assess the validity of this catalogue by crossmatching our OB association members with other catalogues of OB associations, star clusters and young stellar groups, confirming the high-confidence of our census of OB associations. We characterize these OB associations physically (total initial stellar mass, number of OB stars, ...) and kinematically (velocity dispersion, linear expansion ages, ...). The majority of the OB associations (38 out of 56) exhibit a significant expansion pattern in at least one direction, including 12 in both plane-of-the-sky directions, though differences in expansion velocity suggest anisotropical expansion patterns. We compare the locations of these OB associations with superclouds and features in the local Milky Way such as the Radcliffe Wave and discuss the implications for star formation in the solar neighbourhood.

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 / 2 minor

Summary. The paper exploits a complete Gaia-based census of ~25,000 O- and B-type stars within 1 kpc to identify 56 OB associations via HDBSCAN clustering, claiming this doubles the number of known associations in the volume. Validity is assessed through cross-matching with existing OB association, cluster, and young-group catalogues. The associations are then characterized by total initial stellar mass, number of OB stars, velocity dispersion, and linear expansion ages; 38 show significant expansion (12 in both plane-of-sky directions), and their locations are compared to superclouds and features such as the Radcliffe Wave.

Significance. If the catalogue proves reliable, the work would provide a valuable doubled census of local OB associations with kinematic and mass characterizations, enabling improved studies of star formation, expansion patterns, and connections to Galactic structures. The use of a complete stellar sample and HDBSCAN is a methodological strength, though the central reliability claim requires quantitative support.

major comments (2)
  1. [§5] §5 (Validation and cross-matching): The manuscript states that validity was assessed via cross-matching with other catalogues, confirming high confidence. However, this procedure primarily recovers previously known structures and provides no reported purity, completeness, false-discovery-rate, or contamination statistics specifically for the 28 newly identified associations. No tests against randomized realizations or parameter-sensitivity analyses for HDBSCAN are described, leaving the 'highly-reliable' claim for the new entries unquantified and load-bearing for the doubled-census result.
  2. [§4] §4 (The OB association catalogue): The central claim of a factor-of-two increase rests on the 56 associations being physically distinct groups rather than chance alignments. Without the missing quantitative validation metrics noted above, the expansion-age and mass characterizations for the new associations cannot be confidently interpreted as representative of true OB associations.
minor comments (2)
  1. [Abstract / §3] The abstract refers to 'linear expansion ages' and 'anisotropical expansion patterns' without a brief definition or reference to the exact fitting procedure used; this should be clarified in the methods or results section for reproducibility.
  2. [Table 1 / §4] Table or figure presenting the full catalogue should include columns for the number of member stars, estimated mass, and expansion velocity components to allow direct comparison with prior catalogues.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for their constructive feedback on our manuscript. We address the major comments regarding the validation and reliability of the new OB associations in the point-by-point responses below. We agree that additional quantitative support would strengthen the claims and will revise the manuscript accordingly where possible.

read point-by-point responses

  1. Referee: §5 (Validation and cross-matching): The manuscript states that validity was assessed via cross-matching with other catalogues, confirming high confidence. However, this procedure primarily recovers previously known structures and provides no reported purity, completeness, false-discovery-rate, or contamination statistics specifically for the 28 newly identified associations. No tests against randomized realizations or parameter-sensitivity analyses for HDBSCAN are described, leaving the 'highly-reliable' claim for the new entries unquantified and load-bearing for the doubled-census result.

    Authors: We acknowledge that the cross-matching primarily validates the recovery of known associations and does not directly quantify the reliability of the 28 new ones through metrics such as purity or false discovery rate. The 'highly-reliable' description is based on the consistent application of HDBSCAN to a complete sample and the physical coherence of the detected groups, including their expansion signatures. However, we agree that this leaves the claim somewhat unquantified. In the revised manuscript, we will include a parameter-sensitivity analysis for HDBSCAN by varying the min_cluster_size and min_samples parameters and reporting how many associations remain stable. We will also discuss the limitations regarding the lack of randomized tests for the new associations. revision: partial

  2. Referee: §4 (The OB association catalogue): The central claim of a factor-of-two increase rests on the 56 associations being physically distinct groups rather than chance alignments. Without the missing quantitative validation metrics noted above, the expansion-age and mass characterizations for the new associations cannot be confidently interpreted as representative of true OB associations.

    Authors: The factor-of-two increase is determined by comparing our catalogue of 56 associations to the number previously known within 1 kpc from literature compilations. We maintain that the associations are physically distinct because they are identified as overdensities in the 6D phase space (position and velocity) using HDBSCAN, and a majority exhibit expansion, which is unlikely for chance alignments. Nevertheless, we recognize the referee's concern about interpreting the characterizations for the new associations. We will add a caveat in the revised text noting that while the method is uniform, independent confirmation for the new groups is limited to the internal consistency of the data, and future spectroscopic follow-up would be beneficial. revision: yes

standing simulated objections not resolved
  • Full Monte Carlo simulations to compute purity, completeness, and false discovery rates for the newly identified associations

Circularity Check

0 steps flagged

Direct application of HDBSCAN to external Gaia data with external cross-match validation

full rationale

The paper applies the HDBSCAN clustering algorithm directly to an external complete census of ~25,000 O- and B-type stars from Gaia within 1 kpc. The resulting catalogue of 56 associations is validated by cross-matching members against independent external catalogues of OB associations, star clusters, and young stellar groups. No equations, fitted parameters, or self-citations are used to derive the associations themselves; the chain consists of standard clustering on public astrometric data followed by external confirmation. This is self-contained against external benchmarks with no reduction of outputs to inputs by construction.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on the completeness of the input OB-star census from Gaia, the ability of HDBSCAN to recover physically meaningful groups, and the validity of cross-matching for confirmation. No new entities are postulated.

free parameters (1)
  • HDBSCAN hyperparameters
    Minimum cluster size, epsilon, and other clustering parameters must be selected to yield exactly 56 associations; these choices are not detailed in the abstract.
axioms (1)
  • domain assumption Gaia DR3 (or equivalent) astrometry supplies sufficiently accurate positions, parallaxes, and proper motions for reliable clustering of OB stars within 1 kpc
    Invoked implicitly when applying HDBSCAN to the 25,000-star sample.

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Forward citations

Cited by 2 Pith papers

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Reference graph

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