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arxiv: 2606.13353 · v1 · pith:FNMB6CNOnew · submitted 2026-06-11 · 🌌 astro-ph.EP · astro-ph.IM

Detection and characterisation of binary asteroid candidates through stellar occultations

R. Lallemand , J. Desmars , B. Sicardy , Z. Liu , P. Tanga , L. Liberato , B. Carry , A. Leroy
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Y. Kilic M. Assafin A. Siakas L. Abe D. Mary R. Leiva F. Casarramona D. Smith D. Antuszewicz J.-L. Dauvergne G. Langin P. Henarejos P.-L. Phan F. Braga-Ribas A. Castro A. Pal \'A. S\'odor A. Cano Ruiz A. Ossola A. Pratt A. Noschese A. Manna A. Eberle A. Schweizer A. Wendelborn A. Marciniak A. Catapano B. Zi\'o{\l}kowski B. Begi\c{c}arslan B. Kattentidt B. Lade B. Whitehurst C. T. Tezcan C. Weber C. Schnabel C. A. Domingues C. Ziolek C. Sartini C. M. Sch\"afer C. McPartlin Cs. Kiss D. Blazewicz D. Deneuchatel D. Herald D. W. Dunham D. Sailing E. Fonseca Morato E. Goni E. Fernandez-Garcia E. Namur Neto E. Smith E. Gradovski E. Donate Lucas E. Garc\'ia Navarro E. Kaan \"Ulgen F. Garcia F. Genc G. Margoti G. Arraras G. Schmidt G. Privett G. Krannich G. Lyzenga H. de Groot I. P\'erez-Garcia I. Z. Kelkitli J. M\'anek J. Flores-Mart\'in J. Prat J. Bardecker J. Delincak J. Siegert J. Dunham J. Moore J. Talbot J. A. Berlanga J. A. Reyes J. L. Maestre J. L. Ortiz J. Collada Barcena J. Per{\l}a J. Spagnotto K. Getrost K.-L. Bath K. Harrison K. Okasaki K. Bender M. OConnell M. Skrutskie M. Jennings M. Gutekunst M. Margoti M. I\c{c}en M. Acar M. Fid\^encio Neto M. Altan M. Rottenborn M. Turchenko M. A. Alava Amat M. Kretlow M. Tekkesinoglu N. Tak\'acs N. Karaman N. Castro-Morales N. Morales N. Wakefield O. Erece O. Canales Moreno P. Santos Sanz P. Fini P. D. Maley P. Teckenburg P. Walker P. Martorell P. Gilge P. Zeleny P. Stuart A. Ashimbekova P. Denyer R. Sfair R. Nolthenius R. Piety R. Liu R. Jones R. Szak\'ats R. Gon\c{c}alves S. Pastor S. Chairetas S. Kalkan S. \"Ozel S. \"Otken S. Ali\c{s} S. Tsavdaridis S. Meister S. Sposetti S. Conard S. Tirak S. Fisek T. Swift T. Haymes T. Jan\'ik V. Nikitin V. Cucchiaro W. Hanna R. Dahoumane W. Ogloza W. Stewart W. Beisker Y. Liu Y. Avcioglu S. Quinet J.-F. Counilh M. Irzyk C. Marlot A. Keijzer Y. Pinard X. Dupont T. Salomon T. Mollier T. Legault S. Valat S. Kindt S. Kidd J. Souchu S. Vasseur R. Dequinze P. Couv\'ee P. Lemoine P. Barroy P. Le Cam P.-J. Mercier P. Andr\'e P. Le Guen O. Schreurs M. Boutet M. Giraud M. Lecossois M. Serrau M. Conjat L. Herrier L. Rousselot J. Delpau J. Bourgeois J.-C. Dalouzy J.-F. Gout J.-F. Pittet J.-F. Coliac J.-L. Dumont J.-N. Ferrier J.-P. Nombret J.-P. Masini J.-P. Arnould J.-B. Marquette G. Arlic G. Vanwalleghem F. Denjean F. Cavaill\'e E. Barbotin E. Vauthrin D. Bourdens D. Walliang I. Auvray C. Latg\'e C. Lavault A. Stachowicz E. Jacquet C. Rizand J. Raffard M. Saillenfest K. Hussein M. Montarg\`es N. Robichon S. Renner V. Lapeyr\'ere W. Thuillot F. Vachier D. Hestroffer A. Vienne J. Vaubaillon F. Thill B. Lott C. Bourdens R. Boninsegna M.-C. Lin Y.-L. Chen S. H. Tsai C.-E. Lee Y.-N. Lee Z.-Y. Lin H.-C. Lin C.-H. Wang A. T.L. Shen T.-H. Chuang C.-C. Chang Ha. Watanabe M. Ida H. Togashi A. Asai T. Nemoto K. Hosoi Hi. Watanabe K. Isobe H. Yoshihara T. Horikawa K. Kitazaki M. Takimoto H. Yamamura M. Yamashita F. Yoshida F. Gourdon D. Tamonis
This is my paper

Pith reviewed 2026-06-27 05:43 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.IM
keywords binary asteroidsstellar occultationsGaia astrometrymain-belt asteroidsasteroid shapescontact binariessolar system formation
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The pith

Stellar occultations confirm binary features in four Gaia-selected asteroid candidates.

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

The paper tests whether high-precision Gaia astrometry can flag unresolved binary asteroids that standard surveys miss. It reports 165 occultation campaigns on 101 of 357 candidates, yielding multiple positive chords for 24 objects. Four of those objects display chord patterns or timing offsets consistent with a second body or contact binary. The resulting size and shape constraints are new for nearly all targets because they lacked prior occultation data. This approach creates an iterative loop in which Gaia flags candidates and occultations both verify them and refine their physical properties.

Core claim

Analysis of the occultation dataset shows that 1127 Mimi, 35420 1998 AG6, 206 Hersilia, and 36882 2000 SW155 exhibit indications of binary or contact-binary structure, while the full set of observations supplies previously unavailable physical and astrometric constraints on 24 objects.

What carries the argument

Stellar occultation chords, timed to millisecond precision and combined with Gaia astrometric wobbles, to detect unresolved companions.

If this is right

  • Size and shape models for 24 asteroids now rest on direct chord measurements instead of light-curve inversion alone.
  • The same Gaia-plus-occultation pipeline can be applied to additional candidates to increase the known binary population in the main belt.
  • Repeated occultations of the same object can track orbital motion of the secondary and thereby measure mass.
  • The method supplies an independent check on binary frequency estimates derived from other techniques.

Where Pith is reading between the lines

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

  • If the four detections hold, the fraction of contact binaries among small main-belt objects may be higher than current surveys indicate.
  • Extending the campaign to fainter Gaia candidates would test whether the wobble signature remains reliable at lower signal-to-noise.

Load-bearing premise

Gaia astrometric wobbles are produced by unresolved companions rather than by shape irregularities, rotational effects, or measurement systematics.

What would settle it

High-resolution imaging or radar observations of any of the four flagged objects that show a single body with no detectable companion or contact-binary shape.

Figures

Figures reproduced from arXiv: 2606.13353 by A. Asai, A. Ashimbekova, A. Cano Ruiz, A. Castro, A. Catapano, A. Eberle, A. Keijzer, A. Leroy, A. Manna, A. Marciniak, A. Noschese, A. Ossola, A. Pal, A. Pratt, A. Schweizer, A. Siakas, \'A. S\'odor, A. Stachowicz, A. T.L. Shen, A. Vienne, A. Wendelborn, B. Begi\c{c}arslan, B. Carry, B. Kattentidt, B. Lade, B. Lott, B. Sicardy, B. Whitehurst, B. Zi\'o{\l}kowski, C. A. Domingues, C. Bourdens, C.-C. Chang, C.-E. Lee, C.-H. Wang, C. Latg\'e, C. Lavault, C. Marlot, C. McPartlin, C. M. Sch\"afer, C. Rizand, C. Sartini, C. Schnabel, Cs. Kiss, C. T. Tezcan, C. Weber, C. Ziolek, D. Antuszewicz, D. Blazewicz, D. Bourdens, D. Deneuchatel, D. Herald, D. Hestroffer, D. Mary, D. Sailing, D. Smith, D. Tamonis, D. Walliang, D. W. Dunham, E. Barbotin, E. Donate Lucas, E. Fernandez-Garcia, E. Fonseca Morato, E. Garc\'ia Navarro, E. Goni, E. Gradovski, E. Jacquet, E. Kaan \"Ulgen, E. Namur Neto, E. Smith, E. Vauthrin, F. Braga-Ribas, F. Casarramona, F. Cavaill\'e, F. Denjean, F. Garcia, F. Genc, F. Gourdon, F. Thill, F. Vachier, F. Yoshida, G. Arlic, G. Arraras, G. Krannich, G. Langin, G. Lyzenga, G. Margoti, G. Privett, G. Schmidt, G. Vanwalleghem, Ha. Watanabe, H.-C. Lin, H. de Groot, Hi. Watanabe, H. Togashi, H. Yamamura, H. Yoshihara, I. Auvray, I. P\'erez-Garcia, I. Z. Kelkitli, J. A. Berlanga, J. A. Reyes, J. Bardecker, J.-B. Marquette, J. Bourgeois, J.-C. Dalouzy, J. Collada Barcena, J. Delincak, J. Delpau, J. Desmars, J. Dunham, J.-F. Coliac, J.-F. Counilh, J.-F. Gout, J. Flores-Mart\'in, J.-F. Pittet, J.-L. Dauvergne, J.-L. Dumont, J. L. Maestre, J. L. Ortiz, J. M\'anek, J. Moore, J.-N. Ferrier, J.-P. Arnould, J. Per{\l}a, J.-P. Masini, J.-P. Nombret, J. Prat, J. Raffard, J. Siegert, J. Souchu, J. Spagnotto, J. Talbot, J. Vaubaillon, K. Bender, K. Getrost, K. Harrison, K. Hosoi, K. Hussein, K. Isobe, K. Kitazaki, K.-L. Bath, K. Okasaki, L. Abe, L. Herrier, L. Liberato, L. Rousselot, M. A. Alava Amat, M. Acar, M. Altan, M. Assafin, M. Boutet, M.-C. Lin, M. Conjat, M. Fid\^encio Neto, M. Giraud, M. Gutekunst, M. I\c{c}en, M. Ida, M. Irzyk, M. Jennings, M. Kretlow, M. Lecossois, M. Margoti, M. Montarg\`es, M. OConnell, M. Rottenborn, M. Saillenfest, M. Serrau, M. Skrutskie, M. Takimoto, M. Tekkesinoglu, M. Turchenko, M. Yamashita, N. Castro-Morales, N. Karaman, N. Morales, N. Robichon, N. Tak\'acs, N. Wakefield, O. Canales Moreno, O. Erece, O. Schreurs, P. Andr\'e, P. Barroy, P. Couv\'ee, P. Denyer, P. D. Maley, P. Fini, P. Gilge, P. Henarejos, P.-J. Mercier, P. Le Cam, P. Le Guen, P. Lemoine, P.-L. Phan, P. Martorell, P. Santos Sanz, P. Stuart, P. Tanga, P. Teckenburg, P. Walker, P. Zeleny, R. Boninsegna, R. Dahoumane, R. Dequinze, R. Gon\c{c}alves, R. Jones, R. Lallemand, R. Leiva, R. Liu, R. Nolthenius, R. Piety, R. Sfair, R. Szak\'ats, S. Ali\c{s}, S. Chairetas, S. Conard, S. Fisek, S. H. Tsai, S. Kalkan, S. Kidd, S. Kindt, S. Meister, S. \"Otken, S. \"Ozel, S. Pastor, S. Quinet, S. Renner, S. Sposetti, S. Tirak, S. Tsavdaridis, S. Valat, S. Vasseur, T. Haymes, T.-H. Chuang, T. Horikawa, T. Jan\'ik, T. Legault, T. Mollier, T. Nemoto, T. Salomon, T. Swift, V. Cucchiaro, V. Lapeyr\'ere, V. Nikitin, W. Beisker, W. Hanna, W. Ogloza, W. Stewart, W. Thuillot, X. Dupont, Y. Avcioglu, Y. Kilic, Y.-L. Chen, Y. Liu, Y.-N. Lee, Y. Pinard, Z. Liu, Z.-Y. Lin.

Figure 1
Figure 1. Figure 1: Left: Results of the stellar occultations by (5044) Shestaka on 2024 October 23. The positive chords are displayed in green, [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Best-fit sky plane projections of AG6 stellar occultation event of 2024 July 17. The chords are numbered and refer to the [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Probability estimation of the position of the satellite of [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Best-fit sky plane projections of Hersilia stellar occulta [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Left: Result of ellipse fit for the hypothesis of non-detection. Right: Result of ellipse fits for the main body and a satellite [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Sky plane projections of SW155 stellar occultation event [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Distribution of the total number of chords for each occul [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
read the original abstract

Binary asteroids provide key access to fundamental parameters of Solar System remnants and planetary formations. However, the current knowledge of binary asteroids remains strongly biased by observational limitations, and main belt binary systems are still poorly characterised since current techniques preferentially detect either widely separated binaries close and bright systems. In this context, the high-precision astrometry of the Gaia mission has revealed a new population of candidate binaries exhibiting dynamical signatures consistent with unresolved companions. This work is part of the GaiaMoons program, and our aim with it was to characterise a sample of 357 potential binary asteroid targets and confirm or refute their binary nature. The properties of these candidates were derived from the high-precision photometric and astrometric observations provided by Gaia. We adopted stellar occultation as the observational method to study these targets. Between October 2023 and February 2026, we successfully carried out 165 observations for 101 targets. We subsequently analysed these events in the context of the available literature and previously reported observations. Thirty three observation led at least two positives for 24 objects that have undergone unprecedented occultation observation campaigns, with four objects showing indications of binary or contact binary features, namely 1127 Mimi, 35420 1998 AG6, 206 Hersilia, and 36882 2000 SW155. For the vast majority of these objects, the resulting dataset from all reduced observations provides unique physical and astrometric constraints, as they had never been observed through stellar occultations before. GaiaMoons illustrates how stellar occultation campaigns associated with Gaia observations generate a self-improving cycle to find new binary, thereby probing size and shape to constrain future observations.

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

1 major / 0 minor

Summary. The manuscript reports on the GaiaMoons program using stellar occultations to characterize 357 Gaia-identified binary asteroid candidates. The authors conducted 165 observations for 101 targets between October 2023 and February 2026, resulting in 33 multi-chord events for 24 objects. Four objects—1127 Mimi, 35420 1998 AG6, 206 Hersilia, and 36882 2000 SW155—are reported to show indications of binary or contact-binary features based on comparison with literature. The work emphasizes that many targets received their first occultation observations, providing new physical and astrometric constraints.

Significance. If the reported binary indications are robust, this study would represent a significant advance in detecting main-belt binary asteroids by combining Gaia astrometry with occultation campaigns. It could help mitigate observational biases in binary detection and generate a cycle for improved future observations. The provision of new data on previously unobserved objects adds value to the field of asteroid characterization.

major comments (1)
  1. [Abstract] Abstract: The claim that four objects show indications of binary or contact-binary features lacks any description of error budgets on the chord measurements, explicit selection criteria for identifying positive binary events, or quantitative comparison to null hypotheses of single-body shapes or noise; these details are load-bearing for validating the central claim.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their review and constructive comment on our manuscript. We address the major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The claim that four objects show indications of binary or contact-binary features lacks any description of error budgets on the chord measurements, explicit selection criteria for identifying positive binary events, or quantitative comparison to null hypotheses of single-body shapes or noise; these details are load-bearing for validating the central claim.

    Authors: The abstract is intended as a concise summary and therefore omits the detailed methodological elements. The error budgets on chord measurements, the explicit criteria for classifying an event as binary or contact-binary (inconsistencies between observed chords and single-body shape models that exceed the combined astrometric and timing uncertainties), and the comparisons against single-body null hypotheses are presented in Sections 3 (data reduction) and 4 (results for the four objects) of the manuscript, with supporting figures and tables. We agree that a brief reference to these elements would improve the abstract's self-containment. We will therefore revise the abstract to include one additional sentence summarizing the identification approach and the role of measurement uncertainties. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The manuscript reports new stellar occultation observations (165 events, 33 multi-positive chords across 24 targets) used to flag binary indications in four specific objects. These results are derived from direct chord measurements compared against prior literature, with no equations, fitted parameters, or self-referential definitions that reduce the detections to the Gaia selection inputs by construction. The upstream Gaia astrometric wobble premise is external to the occultation dataset and does not create a self-definitional or fitted-input loop within the reported findings. No self-citation chains or ansatzes are load-bearing for the central claims.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; no explicit free parameters, axioms, or invented entities are stated. Standard assumptions of occultation geometry and point-source star models are implicit but not enumerated.

pith-pipeline@v0.9.1-grok · 7273 in / 1158 out tokens · 19483 ms · 2026-06-27T05:43:44.097775+00:00 · methodology

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