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REVIEW 3 major objections 5 minor 268 references

The paper claims that the occultation of HD 98800 AaAb by the circumbinary disc around BaBb can be predicted to windows of 5–15 days, with specific ingress and egress dates between August 2025 and June 2031.

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2026-08-02 06:49 UTC pith:BUYRJG33

load-bearing objection Solid orbital update with genuinely useful timing tables, but the abstract oversells the 5–15 day windows and the two astrometric solutions shift crossing dates by more than the quoted 1σ. the 3 major comments →

arxiv 2607.11599 v2 pith:BUYRJG33 submitted 2026-07-13 astro-ph.EP astro-ph.SR

Peering through the disc of HD 98800 BaBb. Precise timing predictions for the HD 98800 AaAb occultation

S. Z\'u\~niga-Fern\'andez , A. Bayo , J. Olofsson , J. Ehrhardt , \'A. Ribas This is my paper
classification astro-ph.EP astro-ph.SR
keywords HD 98800hierarchical quadruple systemcircumbinary discpolar discoccultation timingorbital fittingradial velocityastrometry
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This letter refines the orbital solution of the young quadruple system HD 98800 and uses it to predict when the inner binary AaAb will pass behind the circumbinary disc around its sibling binary BaBb. Adding new radial-velocity and astrometric data to a joint fit of all three orbits cuts the uncertainty in the outer orbital period and periastron epoch by about a factor of two. Projecting the adopted disc geometry (inclination 26°, position angle 15.6°, dust from 2.5 to 4.6 au, gas from 1.6 to 6.4 au) onto the sky and comparing it with the revised orbit gives median ingress and egress dates for eight gas and dust crossing phases, with formal 1σ windows of 5–15 days. The authors are explicit that the dates remain model-dependent, because the 1σ windows reflect only the orbital posterior while the disc structure is taken as fixed. These narrow windows matter because they turn a multi-year eclipse into a schedulable campaign, and the sequence of ingress, cavity crossings, and egress can be used to learn the disc's radial structure and geometry.

Core claim

The authors establish that the upcoming occultation of HD 98800 AaAb by the circumbinary disc around HD 98800 BaBb can be predicted to considerably higher precision than before. Their revised joint orbital solution is consistent with earlier dynamical masses, but the outer orbit's period and periastron epoch are now roughly twice as well constrained, and the resulting sky-plane crossing windows for eight gas and dust disc boundaries shrink to 5–15 days at the 1σ level. Table 3 lists median ingress/egress dates starting with gas-outer ingress around September 2025, dust-outer ingress around July 2026, the inner cavity crossings in 2027–2029, and egress phases ending around May–June 2031.

What carries the argument

The load-bearing object is a sky-plane projection of the adopted circumbinary disc: a circular, axisymmetric ring with fixed inclination, position angle, and gas/dust radii. The authors evaluate the revised outer-orbit posterior in the sky plane and identify crossing times wherever the separation of A relative to B changes sign relative to each projected disc boundary, linearly interpolating between time samples. Doing this for the 16th, 50th, and 84th percentile orbital tracks converts the orbital uncertainty into a median epoch and a formal 1σ window for each crossing phase.

Load-bearing premise

The predicted dates assume the disc is a simple circular ring at a fixed tilt and orientation with specific gas and dust radii taken from earlier millimetre-wave observations; if the real disc is warped, lopsided, or extends farther, the crossing times shift outside the quoted 5–15 day windows.

What would settle it

Monitor the light curve of HD 98800 AaAb from August 2025 onward: if the first sustained dimming begins more than about two weeks from the predicted gas-outer ingress (around 1 September 2025) or if no sharp dust-edge ingress appears around early July 2026, the assumed disc geometry or orbit is wrong. Stronger: compare the full observed sequence of ingress, cavity recovery, and egress against the eight windows in the paper's Table 3.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Observers can schedule dedicated photometric and spectroscopic monitoring of AaAb around the predicted ingress (mid-2026), cavity crossings (2027–2029), and egress (2030–2031) rather than watching continuously for years.
  • The sequence of dust and gas crossings, including the cavity phase, can probe the disc's radial extent, opacity structure, and how the inner cavity is shaped by the binary.
  • A precise comparison of the observed dimming chronology with these predictions tests whether the occulting disc really follows the simple axisymmetric geometry assumed here.
  • The improved outer orbit tightens the dynamical masses of both the AaAb and BaBb subsystems, reducing uncertainty in the system's physical scale through the revised parallax.
  • If the predicted windows are confirmed, the 2025–2031 event becomes a controlled experiment on polar disc–binary interaction in a pre-main-sequence multiple system.

Where Pith is reading between the lines

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

  • Editorial inference: the same crossing-time machinery can be inverted; once real light-curve timings are measured, offsets between predicted and observed gas/dust crossings can solve for the disc's actual outer radius, inclination, and position angle instead of assuming them.
  • Editorial inference: because the sightline sweeps across several distinct radii over six years, synchronized multi-band photometry could separate a sharp optically thick dust edge from a tenuous extended halo, a distinction the geometric model cannot make on its own.
  • Editorial inference: the two solutions (I and II) bracket the uncertainty in pre-1991 astrometry; a single clean astrometric epoch around 2026–2027 could discriminate between them and further narrow which predicted window is most likely.

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

3 major / 5 minor

Summary. The paper presents a revised joint orbital fit of the HD 98800 AaAb and BaBb subsystems and the wide AB orbit, combining new HARPS/NIRPS RVs, PIONIER and speckle/VLA astrometry with published data. The fit is used to update the predicted epochs when the BaBb circumbinary disc crosses the line of sight to AaAb. The authors find that the outer AB orbit is improved by about a factor of two in period and periastron epoch uncertainty, and they report 1σ crossing windows of 5–15 days for eight gas/dust ingress/egress phases between 2025 and 2031, based on the disc geometry of Kennedy et al. (2019) and Faruqi et al. (2025).

Significance. If the timing predictions hold, this is a valuable resource for planning multi-wavelength monitoring of a rare occultation event. The paper's orbital fits are standard and reproducible: the posterior samples and code are made public, per-instrument zero points and a KI V2 jitter term are included, and the two pre-1991 astrometric uncertainty cases bracket the unknown systematics. However, the headline precision claim is stated for each solution separately; the systematic difference between the two solutions is comparable to the quoted 1σ windows, and the disc geometry is fixed. The real predictive precision is therefore lower than advertised, though still an improvement over SZF21.

major comments (3)
  1. [§3.3 and Table 3] The abstract claims that the crossing windows are narrowed to 5–15 days at 1σ. This is not supported when the two AB solutions are considered. Solution I and II (different assumed pre-1991 astrometric uncertainties) yield median crossing epochs that differ by 8–12 d for key phases: dust outer ingress 3 Jul vs 15 Jul 2026 (difference 12 d) and gas outer ingress 1 Sep vs 9 Sep 2025 (8 d). These differences are equal to or larger than the per-solution 1σ ranges (Table 3). The statement in §3.3 that the T0 difference of ~2.2 yr translates into 'only a modest positional uncertainty' of ~60 mas over 5 yr is misleading in this context: 60 mas is comparable to the projected disc radii (dust outer 4.6 au ≈ 0.10″, gas outer 6.4 au ≈ 0.14″), so it shifts the crossing epochs by weeks. To support the headline precision, the authors should either combine/marginalize over the two astrometric treatments
  2. [§4 and Appendix B] The quoted 1σ windows reflect only the orbital posterior, not the adopted disc geometry. The disc inclination (26°), PA (15.6°), and radii (dust 2.5–4.6 au; gas 1.6–6.4 au) are taken as fixed from Kennedy et al. (2019)/Faruqi et al. (2025). The authors acknowledge this in §4, but the abstract and conclusions present 5–15 d as the precision of the predictions. A few degrees of inclination/PA uncertainty or 10% radius uncertainty will shift the crossing epochs by more than the quoted 5–15 d. The authors should either propagate disc-geometry uncertainties (even a simple sensitivity study) or state clearly in the abstract that the 5–15 d is the orbital-only contribution and that the total model uncertainty is larger.
  3. [§4, Appendix B] The crossing-time intervals are derived from the 16th, 50th, and 84th percentile tracks of the sky-plane separation, rather than by evaluating crossing times for random samples from the joint orbital posterior. Percentile tracks of the separation do not correspond to a single orbit and can mix different orbital phases, so the quoted '1σ' interval is not a proper posterior predictive interval. I recommend sampling the full posterior (e.g., 1000 orbits) and computing crossing times per orbit; the resulting distribution is the correct basis for the early/median/late columns.
minor comments (5)
  1. [Abstract/Aims] In the Aims paragraph, 'combining the orbit based on the most recent knowledge of the disc structure' appears to be missing a word; probably 'combining the orbit with the most recent knowledge...'.
  2. [Table A.3] The MJD value 660128.935957 in the BaBb RV table is likely a typo for 60128.935957.
  3. [Table 3] Please specify in the caption or footnotes that the −1σ/+1σ columns are derived from the orbital posterior only and do not include disc-geometry or inter-solution systematics.
  4. [§3.1] The BaBb period uncertainty is reported as 0.00015 d, an improvement of two orders of magnitude over SZF21. This result depends on the KI V2 jitter term, but the best-fit jitter value is not reported. Please include the fitted jitter in Table 1 or in the text.
  5. [Fig. C.3] The caption mentions 'mid-March disc position' but the context suggests the epoch is 2026.202; please clarify whether 'mid-March' is intentional and if so, specify the year.

Circularity Check

0 steps flagged

No circularity: timing predictions are a forward projection of an independently fitted orbit through externally adopted disc geometry; the only self-citation is a non-load-bearing baseline.

full rationale

The derivation chain is self-contained and non-circular. The orbital solution (Section 3, Table 2) is fit to published and new radial velocities and astrometry, not to the predicted occultation epochs. The predicted crossing times (Table 3) are then computed by projecting the fitted orbit against a fixed, externally adopted disc geometry from Kennedy et al. (2019) and Faruqi et al. (2025), as described in Appendix B. No crossing epoch or disc parameter is used as an input to the orbital fit, so there is no fitted-input-called-prediction or self-definitional loop. The only self-citation is SZF21 (Zuniga-Fernandez et al. 2021), which provides the prior baseline and some of the same measurements; the new solution adds new RVs and astrometry and is compared with SZF21 rather than justified by it, so the self-citation is not load-bearing. The paper explicitly cautions that the quoted windows are model-dependent and could shift if the disc structure differs from the adopted ALMA-based geometry (Section 4), which is an honest limitation rather than a circular step. The difference between Solutions I and II (from unknown pre-1991 astrometric uncertainties) shifts some median epochs by 8-15 days, larger than the per-solution 1-sigma windows; this is a robustness/precision concern about the headline 5-15 day figure, but it is not circularity because both solutions are fits to the same data under different error assumptions and no predicted time is fed back into the fit.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 0 invented entities

The timing prediction rests on the fitted orbital elements (which are standard outputs, not hidden degrees of freedom) and on four hand-chosen/adopted inputs: the KI jitter term, per-instrument RV zero points, the pre-1991 astrometry error cases, and the disc geometry. The disc geometry is the largest source of model dependence and is explicitly flagged by the authors.

free parameters (4)
  • KI V2 jitter term = not quoted in text
    Added in quadrature to Keck Interferometer pipeline V2 errors to account for instrumental systematics and atmospheric phase jitter (Sect. 3.1). This is a fitted error-inflation parameter that affects the BaBb orbital solution.
  • Instrument RV zero points (gamma_TO95, gamma_ELODIE, gamma_CTIO, gamma_Mercator, gamma_HARPS, gamma_NIRPS, gamma_FEROS, = Table 1 (e.g., gamma_HARPS=7.06±0.50 km/s for BaBb)
    Each spectrograph has a separate systemic velocity zero point fitted jointly with the orbital elements (Sect. 3). These are necessary because RVs come from multiple instruments with unknown relative offsets.
  • Pre-1991 AB astrometric uncertainties (sigma~0.1 and sigma~0.02) = two hand-chosen cases: 0.1 and 0.02 arcsec
    The original USNO astrometric uncertainties are not reported; the authors test two typical values, producing Solution I and II (Sect. 3.3). These choices directly affect the inferred AB period and periastron epoch, hence the predicted windows.
  • Adopted disc geometry: inclination=26°, PA=15.6°, dust 2.5–4.6 au, gas 1.6–6.4 au = 26 deg, 15.6 deg, 2.5/4.6 au, 1.6/6.4 au
    These parameters are taken by hand from Kennedy et al. (2019) and Faruqi et al. (2025) and are central to the timing calculation (Sect. 4, Appendix B). They are not refit here; if wrong, all quoted epochs shift.
axioms (4)
  • standard math Each binary orbit is Keplerian and the system remains gravitationally stable over the prediction window.
    The joint fit solves Keplerian orbits for AaAb, BaBb, and AB; the disc geometry is projected assuming those orbits persist (Sect. 3).
  • domain assumption The circumbinary disc is intrinsically circular; its sky projection is an ellipse with semiminor axis reduced by cos(i).
    Appendix B: 'Assuming that the disc is intrinsically circular, its projection on the sky is an ellipse.' This is a standard geometric assumption but is not tested against the ALMA data in this paper.
  • domain assumption The disc geometry (inclination, PA, inner/outer radii) is fixed and axisymmetric over the 2025–2031 prediction window.
    Section 4 adopts the ALMA-based geometry of Kennedy et al. (2019)/Faruqi et al. (2025) and does not evolve it. The authors acknowledge that a different disc structure would shift the epochs.
  • domain assumption Instrument RV zero points are constant over the time span of each dataset.
    The fit assigns one gamma per instrument (Sect. 3). This ignores possible long-term drifts or activity-induced RV variations, which are presumably small relative to the stated errors.

pith-pipeline@v1.3.0-alltime-deepseek · 11351 in / 12539 out tokens · 114092 ms · 2026-08-02T06:49:16.248434+00:00 · methodology

0 comments
read the original abstract

HD 98800 is a young hierarchical quadruple system composed of the tight binaries AaAb and BaBb on a wide, highly inclined outer orbit. The B subsystem hosts a circumbinary disc in a polar configuration, and the geometry of the system offers a rare opportunity to observe the passage of the disc around BaBb in front of AaAb. We aim to update the overall orbital solution to offer precise time windows of the main occultation features by combining the orbit with the state-of-the-art knowledge of the disc's structure. We combine new and published radial-velocity measurements and multi-wavelength astrometry for the outer AB orbit and both inner subsystems, AaAb and BaBb, in a joint orbital fit. The revised solution is consistent with previous dynamical masses and improved the outer orbit, reducing the uncertainties in the period and periastron epoch by about a factor of two. It also narrows the predicted crossing-phase windows to 5--15 days at the 1{\sigma} level, improving the timing of ingress, egress, and the first cavity-crossing predictions. These results provide a more accurate timing framework for future observations of the occultation, although the predicted epochs remain model-dependent because of uncertainties in the disc structure.

Figures

Figures reproduced from arXiv: 2607.11599 by A. Bayo, \'A. Ribas, J. Ehrhardt, J. Olofsson, S. Z\'u\~niga-Fern\'andez.

Figure 1
Figure 1. Figure 1: Projected sky-plane separation of HD 98800 AaAb relative to the HD 98800 BaBb disc as a function of time, compared with [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗

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