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Characterisation of all known multiple stellar systems within 10 pc

T0 review · 1 major / 2 minor · reviewed 2026-05-09 · grok-4.3

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Pith's one-line read The multiplicity fraction of stars and brown dwarfs falls smoothly from 41 percent above half a solar mass to 9 percent below a tenth of a solar mass within 10 parsecs.

desk verdict This is a useful update to the 10-pc stellar multiplicity census with Gaia data and new orbits, though it remains primarily a data compilation. read the letter →

arxiv 2605.04094 v1 submitted 2026-04-29 astro-ph.SR

J. González-Payo , J. A. Caballero , C. Cifuentes , M. Cortés-Contreras , F. Rica This is my paper · ORCID
classification astro-ph.SR
keywords stellarmultiplicitysolarneighborhoodmultiplestarsystemsbrowndwarfscompanionfractionorbitalperiodsvolume-limitedsamplemassdependence
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper compiles a complete volume-limited sample of 424 stars and brown dwarfs in the solar neighborhood and identifies which ones belong to multiple systems. It reports 92 such systems in double, triple, quadruple, and quintuple configurations, with the fraction of objects that have companions declining steadily as mass decreases. A reader would care because this supplies a precise local reference point for how often stars form with companions versus alone, directly informing models of star formation and the local galactic structure. The work also derives separations, masses, and orbital periods spanning ten orders of magnitude for the identified pairs.

What carries the argument

A volume-limited census of 424 nearby stars and brown dwarfs, verified for physical association through common proper motion and parallax, with orbital solutions computed for selected pairs.

What would settle it

Discovery of an additional low-mass companion to any currently single object in the sample, or demonstration that one of the wide pairs has mismatched proper motion or parallax, would alter the reported multiplicity fractions.

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Extended reading notes

Core claim

From a sample of 424 stars and brown dwarfs within 10 pc, 215 objects reside in 92 multiple systems (68 doubles, 19 triples, 3 quadruples, and 2 quintuples). The multiplicity fraction decreases smoothly from 41 plus or minus 11 percent for stars with masses at least 0.5 solar masses to 9.3 plus or minus 7.4 percent for stars and brown dwarfs with masses 0.1 solar masses or less. All but eight pairs are resolved, and orbital periods range from roughly one day to millions of years.

Load-bearing premise

The list of 424 objects is complete and every physical companion has been detected and correctly identified as bound rather than a chance alignment.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

1 major / 2 minor

Summary. The paper compiles all known multiple stellar systems within 10 pc from the Washington Double Star catalogue, literature sources, and a Gaia DR3 search for common proper motion and parallax. From a volume-limited sample of 424 stars and brown dwarfs, 215 objects are identified in 92 multiple systems (68 doubles, 19 triples, 3 quadruples, 2 quintuples), with all but eight pairs resolved. Orbital solutions are computed for seven systems using public astrometric and radial-velocity data. The multiplicity fraction is reported to decrease smoothly from 41±11% for stars with M ≥ 0.50 M⊙ to 9.3±7.4% for stars and brown dwarfs with M ≤ 0.10 M⊙, with periods spanning ~10 orders of magnitude.

Significance. This observational census supplies a valuable, updated benchmark for stellar multiplicity statistics in the solar neighborhood, directly constraining star-formation and binary-evolution models. The explicit use of public catalogs (WDS + Gaia DR3), reported uncertainties on fractions, and provision of orbital fits for seven systems are clear strengths that enhance reproducibility and utility for the community.

major comments (1)
  1. [Sample compilation and multiplicity-fraction results] The central multiplicity-fraction trend (abstract and results) rests on the assumption that the 424-object sample is complete and that all physical companions (especially wide or low-mass) have been recovered via common proper motion/parallax with negligible false positives. While incompleteness at the lowest masses is noted implicitly, the manuscript lacks a quantitative completeness estimate (e.g., via injection-recovery tests or detection-limit simulations) that would confirm the reported smooth decline is not partly driven by selection effects at M ≤ 0.10 M⊙. This directly affects the load-bearing low-mass end of the claimed trend.
minor comments (2)
  1. [Abstract] The abstract states that 'precise mass and companion star fractions' were measured, yet the quoted uncertainties reach ±7.4% at the lowest masses; a more qualified phrasing would improve accuracy.
  2. [Results on resolved systems] The eight unresolved pairs are mentioned but not listed with their specific properties or references; adding a short table or explicit enumeration would aid clarity.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the positive assessment of our work and the recommendation for minor revision. We address the single major comment below.

read point-by-point responses

  1. Referee: [Sample compilation and multiplicity-fraction results] The central multiplicity-fraction trend (abstract and results) rests on the assumption that the 424-object sample is complete and that all physical companions (especially wide or low-mass) have been recovered via common proper motion/parallax with negligible false positives. While incompleteness at the lowest masses is noted implicitly, the manuscript lacks a quantitative completeness estimate (e.g., via injection-recovery tests or detection-limit simulations) that would confirm the reported smooth decline is not partly driven by selection effects at M ≤ 0.10 M⊙. This directly affects the load-bearing low-mass end of the claimed trend.

    Authors: We agree that an explicit quantitative completeness assessment would strengthen the presentation of the multiplicity-fraction trend. Our 424-object sample is assembled as the most complete compilation possible within 10 pc by combining the Washington Double Star catalogue, all relevant literature, and a systematic Gaia DR3 search for common proper motion and parallax companions. The 10 pc volume is exceptionally well characterized, and Gaia DR3 recovers companions to low masses at wide separations with high fidelity. We did not perform injection-recovery tests because the work is a heterogeneous catalog compilation rather than a single-survey dataset with uniform selection functions. In the revised manuscript we will add a concise subsection (likely in Section 2 or 3) that (i) cites published completeness estimates for the 10 pc census of M dwarfs and brown dwarfs, (ii) quantifies the expected false-positive rate for common-proper-motion pairs using Gaia astrometric precision, and (iii) discusses how any residual incompleteness at M ≤ 0.10 M⊙ would affect the reported 9.3 ± 7.4 % multiplicity fraction. These additions will directly address the referee’s concern without changing the core results or conclusions. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: purely observational census from external catalogs

full rationale

The manuscript compiles a volume-limited 10-pc sample of 424 objects from WDS, Gaia DR3, and literature, identifies 215 members of 92 multiple systems via common proper motion/parallax, and tabulates multiplicity fractions by mass bin. No equations, fitted parameters, predictions, or derivations appear; counts and fractions are direct summaries of the input catalog. No self-citations are load-bearing, and the central claims rest on external, falsifiable astrometric data rather than internal construction.

Assumptions & free parameters 0 free parameters · 2 assumptions · 0 invented entities

The central claims rest on standard domain assumptions about the reliability of Gaia astrometry and catalog completeness rather than new postulates, fitted parameters, or invented entities.

assumptions (2)
  • domain assumption Gaia DR3 parallaxes and proper motions are sufficiently accurate to confirm physical association via common motion and to compute orbital solutions.
    Invoked throughout the data compilation and orbital fitting sections.
  • domain assumption The Washington Double Star catalogue plus literature provides a complete starting list of resolved pairs within the volume.
    Basis for the initial sample before Gaia cross-matching.

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Cite this review

Pith. "Pith review of Characterisation of all known multiple stellar systems within 10 pc." pith.science (2026). https://pith.science/paper/2605.04094

@misc{pith2026260504094,
  author       = {Pith},
  title        = {Pith review of: Characterisation of all known multiple stellar systems within 10 pc},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2605.04094}},
  note         = {Machine review of arXiv:2605.04094}
}
read the original abstract

The study of stellar multiplicity offers important constraints on the structure of the Galaxy as well as stellar and planet formation and evolution. Focusing on the most immediate solar neighbourhood benefits from obtaining both complete and accurate data for reliable statistics. Our goal is to describe the solar neighbourhood within 10 pc in terms of multiplicity by evaluating the angular and physical separations, masses, and orbital periods of the systems from the most complete volume-limited sample. We carried out a comprehensive data compilation from the Washington Double Star catalogue and the literature of all known multiple systems at any separation range, and completed this information with a common proper motion and parallax search with Gaia DR3 data. We also used public astrometric and radial-velocity data to compute orbital solutions of seven pairs. From a sample of 424 stars and brown dwarfs within 10 pc we identified 215 of them in 92 systems in double (68), triple (19), quadruple (3), and quintuple (2) configurations. All except eight pairs have been resolved. Their orbital periods range over ten orders of magnitude from about one day to millions of years. We measured precise mass and companion star fractions at different mass intervals. The multiplicity fraction smoothly decreases from 41+-11% for stars with M >= 0.50 Msun to 9.3+-7.4% for stars and brown dwarfs with M <= 0.10 Msun.

Figures

Figures reproduced from arXiv: 2605.04094 by the authors.

Figure 1
Figure 1. Orbital fit of 𝜒 01 Ori (KNG 1, WDS J05544+2017) with orvara. Top left: astrometric fit (a full legend is in Fig. B1; the outlier data point corresponds to epoch 1982). Bottom left: radial-velocity fit (red: Hamilton-pre, green: Hamilton-post, cyan: Gecko, blue: ELODIE, yellow: SOPHIE). Right: cornerplot with 𝑀primary, 𝑀secondary, 𝑎, 𝑒, and 𝑖. We show the orbital solutions of the seven pairs in [PITH_FULL_IMAGE:fig… view at source ↗
Figure 3
Figure 3. Comparison between dynamical masses 𝑀dyn computed by us and spectro-photometric masses 𝑀spec−phot determined by Kirkpatrick et al. (2024). Triangles and squares denote ‘primary’ and ‘secondary stars, respec￾tively, of the systems with orvara orbital solutions in [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

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

  1. Identification of unresolved binaries in the VVV b294 tile: A Pro-Am collaboration using the Virtual Observatory

    astro-ph.SR 2026-07 conditional novelty 5.0 of 10

    In the VVV b294 tile, 990 unresolved M-dwarf binary candidates (13–14.9% of the sample) survive RUWE<1.4 cuts, with 120 strong targets and many possible substellar secondaries.

Reference graph

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