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arxiv: 2605.01487 · v1 · submitted 2026-05-02 · 🌌 astro-ph.SR

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Speckle Interferometry at SOAR in 2024 and 2025

Andrei Tokovinin, Brian D. Mason, Edgardo Costa, Rene A. Mendez

Pith reviewed 2026-05-09 18:14 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords binary starsspeckle interferometrystellar orbitsvisual binariesSOAR telescopehigh-resolution astrometrypre-main sequence starseccentric orbits
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The pith

Speckle interferometry at SOAR yields 5316 new binary star position measurements and orbital elements for 202 systems.

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

The paper reports results from speckle interferometry observations conducted at the 4.1 m SOAR telescope in 2024 and 2025. These yield 5316 measurements of relative positions and magnitude differences across 3532 pairs, with many separations below 0.2 arcseconds and a minimum of 12 milliarcseconds. More than 400 pairs appear resolved here for the first time and were missed by Gaia, including numerous TESS targets, inner subsystems in wider binaries, and subdwarfs. The positions support computation or refinement of 202 orbits with reported errors, among them examples with extreme eccentricities and pre-main sequence binaries. A reader would care because such close-pair data directly constrains stellar masses, ages, and formation pathways in multiple systems while also documenting non-detections that limit companion possibilities.

Core claim

We present 5316 measurements of relative positions and magnitude differences in 3532 pairs (including 524 unpublished measures made before 2024) with median and minimum separations of 0.19 arcsec and 12 mas, respectively; non-resolutions of 1723 stars are documented as well. More than 400 pairs have been resolved here for the first time and not resolved by Gaia; among those are 222 TESS objects of interest, 46 inner subsystems in known wider binaries within 100 pc, and 43 subdwarfs. Positional measurements are used to compute or improve binary orbits; elements of 202 orbits with meaningful errors are given here, while preliminary and tentative orbits are published elsewhere. Of special note

What carries the argument

Speckle interferometry at the SOAR 4.1 m telescope, which records short-exposure images to measure binary separations and magnitude differences down to 12 mas, followed by fitting of accumulated position data to derive orbital elements.

If this is right

  • The 202 orbits supply mass and period constraints for systems including pre-main sequence binaries.
  • High-eccentricity examples such as e = 0.9866 provide direct data points for testing dynamical evolution models.
  • First-time resolutions of 222 TESS objects of interest supply companion information relevant to exoplanet candidate validation.
  • The 46 newly resolved inner subsystems clarify the architecture of hierarchical multiples within 100 pc.
  • Parameters of 86 calibration binaries support ongoing and future use of the instrument for consistent pixel scale and orientation.

Where Pith is reading between the lines

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

  • These optical measurements could be combined with future Gaia or other astrometric releases to tighten orbital solutions for the same systems.
  • The catalog of non-resolutions offers statistical upper limits on companion fractions at small separations for population studies.
  • The dataset of resolved subdwarfs and young binaries may help anchor age and metallicity relations when masses become available from the orbits.
  • Continued monitoring of the high-eccentricity systems could reveal whether periastron passages produce observable activity or mass transfer.

Load-bearing premise

The speckle measurements contain no significant unaccounted systematic errors at the stated precision and the available observation epochs permit robust determination of orbital elements.

What would settle it

Independent position measurements of several reported binaries, obtained at a different facility or epoch, that fall outside the error ranges predicted by the published orbital elements.

Figures

Figures reproduced from arXiv: 2605.01487 by Andrei Tokovinin, Brian D. Mason, Edgardo Costa, Rene A. Mendez.

Figure 1
Figure 1. Figure 1: Mean centered images of single stars (in nega￾tive square-root rendering) recorded with HRCam on 2024 November 16/17 under excellent seeing at an elevation around 60◦ in the I filter. The size of each image is 3. ′′15. The FWHM along horizontal and vertical directions is indi￾cated. The first image HI.727, recorded immediately after tuning the SOAR optics, shows clear signs of residual aber￾rations. The im… view at source ↗
Figure 2
Figure 2. Figure 2: The rms deviations of the calibrator binaries from their models in the tangential (squares) and radial (crosses) direction vs. angular separation. The line is a linear approx￾imation σ ≈ 1.64ρ which corresponds to the relative pixel scale accuracy of 0.16% or the position angle accuracy of 0. ◦ 09. Calibration of the pixel scale and orientation of HRCam is based on observations of relatively wide pairs, ca… view at source ↗
Figure 3
Figure 3. Figure 3: Cumulative distribution of angular separations in view at source ↗
Figure 4
Figure 4. Figure 4: Fragments of speckle ACFs of two new 2+2 quadruples, in negative rendering. The orientation is stan￾dard (north up, east left). The components corresponding to specific peaks are marked, with the ACF center marked by O and by a white dot. Peaks corresponding to cross-cor￾relations between secondaries, e.g. Ba,Ab, are marked by ’x’ (ACF of a resolved quadruple has 12 secondary peaks). The outer and two inne… view at source ↗
Figure 5
Figure 5. Figure 5: Speckle ACFs of 9 new close triples with sub-arc￾second outer separations and separation ratios above 1:10. based on the SOAR data is published in (A. Tokovinin 2023b, 2025a, 2026a,b). For some stars, speckle interfer￾ometry is combined with radial velocities (A. Tokovinin 2023c, 2025b). Speckle interferometry was also used by Z. D. Hartman et al. (2025) to resolve inner subsystems in wide binaries. R. A. … view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of the magnitude difference ∆I mea￾sured by HRCam with ∆G measured by Gaia for the physi￾cal TOI pairs. The dashed line corresponds to ∆I = 0.9∆G. The outlier (J21564+2041, HD 208258, 2. ′′09, ∆G = 3.34, ∆I = 4.13) may have a blue companion. The TESS-Gaia pairs have been discovered at SOAR independently, offering a blind test of the HRCam data. The comparison is limited here to the 82 physical p… view at source ↗
Figure 6
Figure 6. Figure 6: Magnitude difference ∆m vs. separation ρ for 220 TOIs resolved at SOAR in 2021–2024 (squares) and for 149 wider pairs also found in GDR3 (crosses). Many pairs wider than ∼0. ′′8 are also detected by Gaia. They are marked by the tag ’G’ when both components have common parallaxes and/or PMs in GDR3 and by the tag ’g’ otherwise (likely unrelated or optical pairs); there are 82 and 67 pairs with G and g tags,… view at source ↗
Figure 8
Figure 8. Figure 8: Six new visual orbits with well-constrained elements. In each plot, the ellipse shows the fitted orbit, squares connected to the ellipse are accurate speckle data (bigger red squares for 2024–2025), while visual measures and tentative speckle data are plotted as crosses. The primary component (asterisk) is at coordinate origin, the axis scale is in arcseconds, the orientation is standard (north up, east le… view at source ↗
Figure 9
Figure 9. Figure 9: Two new orbits with large and accurately mea￾sured eccentricity. The eccentricity and its error are indi￾cated. For this paper, we selected 202 orbits where all ele￾ments are constrained by the data and their errors de￾termined by the least squares fit are meaningful; they are grades A or B in the sense of A. Tokovinin (2024b). The updates of known orbits are deemed substantial or dramatic to warrant publi… view at source ↗
Figure 10
Figure 10. Figure 10: Orbits of three young binaries (see text) view at source ↗
read the original abstract

Results of speckle interferometry observations at the 4.1 m SOuthern Astrophysical Research (SOAR) telescope obtained during 2024-2025 are presented. We present 5316 measurements of relative positions and magnitude differences in 3532 pairs (including 524 unpublished measures made before 2024) with median and minimum separations of 0.19" and 12 mas, respectively; non-resolutions of 1723 stars are documented as well. More than 400 pairs have been resolved here for the first time and not resolved by Gaia; among those are 222 TESS objects of interest, 46 inner subsystems in known wider binaries within 100 pc, and 43 subdwarfs. Positional measurements are used to compute or improve binary orbits; elements of 202 orbits with meaningful errors are given here, while preliminary and tentative orbits are published elsewhere. Of special note are orbits with large and accurately measured eccentricties (e.g. e=0.9866+/-0.0014 for J13038-2035) and orbits of pre-main sequence binaries. Appendix contains parameters of 86 binaries used for calibration of pixel scale and orientation.

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 / 3 minor

Summary. The manuscript reports speckle interferometry results from the SOAR 4.1 m telescope in 2024–2025. It presents 5316 measurements of relative positions and magnitude differences for 3532 pairs (including 524 pre-2024 measures), with median and minimum separations of 0.19 arcsec and 12 mas; 1723 non-resolutions are also documented. More than 400 pairs are resolved for the first time (including 222 TESS objects of interest). Elements of 202 orbits with meaningful errors are derived from the new and prior data, with an appendix listing parameters for 86 calibration binaries.

Significance. If the positional accuracies and orbit fits hold, the work substantially augments the high-resolution binary catalog, particularly for nearby systems, pre-main-sequence stars, and TESS targets. The large volume of new measurements and the provision of 202 orbits with uncertainties directly support improved dynamical studies and multiplicity statistics.

major comments (2)
  1. [§3] §3 (Observations and Data Reduction): The claimed minimum resolution of 12 mas and median precision are central to the data-release value, yet the section provides no quantitative error budget (e.g., contributions from atmospheric speckle, detector noise, or residual calibration uncertainty) that would allow independent verification of the stated accuracies.
  2. [§5] §5 (Orbit Computation): The highlighted orbit for J13038-2035 (e = 0.9866 ± 0.0014) is presented as having meaningful errors, but the text does not report the number of epochs, time baseline, or reduced χ² of the fit; without these, it is impossible to judge whether the small eccentricity uncertainty is robust or sensitive to sparse sampling near periastron.
minor comments (3)
  1. [Abstract] Abstract: the statement that 202 orbits have “meaningful errors” would be clearer if it distinguished newly computed orbits from those merely refined by the new data.
  2. [Appendix A] Appendix A: the table of 86 calibration binaries lists pixel-scale and orientation values but omits the individual residuals or formal uncertainties on the derived calibration parameters.
  3. [Tables of orbital elements] Tables of orbital elements: inclusion of a column for the number of observations and the observational time span per orbit would allow readers to assess fit reliability without consulting external catalogs.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the positive assessment of our manuscript and the constructive comments. We address each major comment below and will revise the paper to incorporate the requested information.

read point-by-point responses

  1. Referee: [§3] §3 (Observations and Data Reduction): The claimed minimum resolution of 12 mas and median precision are central to the data-release value, yet the section provides no quantitative error budget (e.g., contributions from atmospheric speckle, detector noise, or residual calibration uncertainty) that would allow independent verification of the stated accuracies.

    Authors: We agree that a quantitative error budget would improve the manuscript and allow independent verification. In the revised version, we will expand §3 to include a detailed error budget, breaking down contributions from atmospheric speckle, detector noise, and residual calibration uncertainties based on our data analysis. revision: yes

  2. Referee: [§5] §5 (Orbit Computation): The highlighted orbit for J13038-2035 (e = 0.9866 ± 0.0014) is presented as having meaningful errors, but the text does not report the number of epochs, time baseline, or reduced χ² of the fit; without these, it is impossible to judge whether the small eccentricity uncertainty is robust or sensitive to sparse sampling near periastron.

    Authors: We acknowledge the omission of these fit details. We will revise §5 to include the number of epochs, time baseline, and reduced χ² for the J13038-2035 orbit, enabling readers to assess the robustness of the eccentricity uncertainty. revision: yes

Circularity Check

0 steps flagged

No significant circularity

full rationale

This is a standard observational catalog paper reporting new speckle interferometry measurements of binary stars, including positions, magnitude differences, and non-resolutions, plus derived orbit elements computed from those measurements. The derivation chain proceeds from raw observations through standard calibration (using an appendix list of reference binaries) to orbit fitting without any self-definitional loops, fitted inputs renamed as predictions, or load-bearing self-citations that reduce the reported results to the inputs by construction. The work is self-contained against external benchmarks such as Gaia non-resolutions and prior orbit catalogs.

Axiom & Free-Parameter Ledger

1 free parameters · 0 axioms · 0 invented entities

The work rests on standard assumptions of speckle interferometry (atmospheric statistics, detector linearity) and orbit fitting (Keplerian motion, no unseen companions). Calibration of pixel scale and orientation is performed by fitting to 86 known binaries listed in the appendix; these are free parameters determined from external reference stars.

free parameters (1)
  • pixel scale and orientation
    Fitted to 86 calibration binaries in the appendix to convert measured pixel offsets into arcseconds and position angles.

pith-pipeline@v0.9.0 · 5525 in / 1166 out tokens · 54702 ms · 2026-05-09T18:14:12.617418+00:00 · methodology

discussion (0)

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Reference graph

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