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arxiv: 2606.23551 · v1 · pith:2LVH3GC2new · submitted 2026-06-22 · 🌌 astro-ph.EP

Observing a 542-day transiting giant with large TTVs: The 2025 transit of HIP 41378 f and new constraints on the outer system

Pietro Leonardi , Alexandre Santerne , Luca Borsato , Salom\'e Grouffal , Christopher R. Mann , Giampaolo Piotto , Karen A. Collins , Patrick Tamburo
show 22 more authors
Yugo Kawai Denise C. Stephens Juliana Garc\'ia-Mej\'ia Edward M. Bryant Krzysztof Sz. Zielinski Daniel Bayliss David Charbonneau Jerome P. de Leon Gareb Fern\'andez-Rodr\'iguez Akihiko Fukui Eric G. Hintz Keith Horne Keisuke Isogai James S. Jenkins Norio Narita Ramotholo Sefako Avi Shporer Richard P. Schwarz Gregor Srdoc Peter Wheatley Jamie B. Williams Jorge Fern\'andez Fern\'andez
This is my paper

Pith reviewed 2026-06-26 07:14 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanet transittransit timing variationsHIP 41378long-period exoplanetsN-body dynamicsmulti-site photometryouter planets
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The pith

The 2025 transit of HIP 41378 f arrived seven hours earlier than its linear ephemeris predicted, confirming large TTVs.

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

The paper reports a multi-site photometric campaign that captured the full 19-hour transit of the 542-day giant planet HIP 41378 f. The measured time of inferior conjunction falls roughly seven hours before the time expected from a constant-period orbit. This offset aligns with the amplitude and sign of previously reported transit timing variations for the same planet. The authors fold the new timing together with existing timings for the two other outer transiting planets and run an N-body dynamical fit to update the orbital solution. The result supplies an improved ephemeris and forecasts for future transits of all three planets.

Core claim

Coordinated observations from NEOSSat, LCOGT, MuSCAT, MuSCAT3, Tierras and NGTS on 31 October 2025 yield an inferior conjunction time T_C = 2460980.888 ± 0.029 BJD_TDB for HIP 41378 f. This epoch lies ~7 hours earlier than the linear ephemeris extrapolation, matching the pattern of TTVs already seen in the planet. When the new timing is combined with the transit times of HIP 41378 d and e inside the TRADES N-body integrator, the fit refines the ephemeris of f and generates updated predictions for all three outer transiting planets.

What carries the argument

The TRADES N-body integrator, which fits the observed transit timings of HIP 41378 d, e and f simultaneously to extract the gravitational perturbations responsible for the measured TTVs.

If this is right

  • The updated ephemeris gives more accurate windows for the next transits of HIP 41378 f.
  • Continued monitoring of d, e and f will tighten mass and eccentricity constraints on the outer planets.
  • The system becomes a test bed for TTV signals in long-period, near-resonant architectures.
  • Similar coordinated campaigns can be used to detect unseen companions around other long-period transiting giants.

Where Pith is reading between the lines

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

  • The large TTV amplitude implies that the interacting planets have substantial masses, which radial-velocity observations could verify.
  • The presence of measurable TTVs at a 542-day period suggests the outer system is dynamically compact or locked in resonance.
  • Additional high-precision timings could separate planet-planet TTVs from possible exomoon signals.

Load-bearing premise

The seven-hour timing offset is produced by gravitational interactions among the outer planets rather than by unmodeled photometric systematics or stellar activity.

What would settle it

A future transit of HIP 41378 f whose measured time deviates from the TRADES-predicted TTV curve by more than the 0.029-day uncertainty would falsify the dynamical interpretation.

Figures

Figures reproduced from arXiv: 2606.23551 by Akihiko Fukui, Alexandre Santerne, Avi Shporer, Christopher R. Mann, Daniel Bayliss, David Charbonneau, Denise C. Stephens, Edward M. Bryant, Eric G. Hintz, Gareb Fern\'andez-Rodr\'iguez, Giampaolo Piotto, Gregor Srdoc, James S. Jenkins, Jamie B. Williams, Jerome P. de Leon, Jorge Fern\'andez Fern\'andez, Juliana Garc\'ia-Mej\'ia, Karen A. Collins, Keisuke Isogai, Keith Horne, Krzysztof Sz. Zielinski, Luca Borsato, Norio Narita, Patrick Tamburo, Peter Wheatley, Pietro Leonardi, Ramotholo Sefako, Richard P. Schwarz, Salom\'e Grouffal, Yugo Kawai.

Figure 1
Figure 1. Figure 1: Combined light-curves of the 2025 transit of HIP 41378 f. The data from all facilities are shown together, with unbinned measurements displayed as grey points and 25-minute binned data highlighted with colored markers for each instrument. The best-fit transit model, obtained from the joint analysis with PyORBIT, is overplotted as a black line. Residuals are shown in the lower panel. The top axis indicates … view at source ↗
Figure 2
Figure 2. Figure 2: Posterior probability distributions for the transit parame [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Observed-minus-calculated (O−C) diagrams for HIP 41378 f for the compact configuration (a) and the extended configuration (b). The best-fit model (MAPHDI) is shown as a black curve, while the shaded regions represent the 1, 2, and 3σ posterior intervals . 1σ with the prediction of García-Mejía et al. (2025). The 2025 combined transit light curve of HIP 41378 f is shown in [PITH_FULL_IMAGE:figures/full_fig… view at source ↗
Figure 4
Figure 4. Figure 4: Forward modeling of the O − C diagrams for the HIP 41378 outer triplet based on the MAPHDI solution. The top axis shows the calendar year of observation, while the bottom axis gives the time in BJDTDB. Black points represent the simulated individual transit times, and the solid black line shows the best-fit dynamical model. Red diamonds mark the observed epochs for each planet, while the blue shaded region… view at source ↗
read the original abstract

Characterizing long-period transiting exoplanets is inherently challenging due to the rarity and long duration of transit events. Yet, these systems provide unique insights into planetary formation, migration, the detection of exomoons, and primordial atmospheres by occupying a sparsely populated region of the exoplanet parameter space. The complexity increases further for long-period planets near mean-motion resonances, where transit timing variations (TTVs) can reach amplitudes of several hours to days. We present a coordinated space- and ground-based observing campaign, using photometry from NEOSSat, multiple LCOGT sites, MuSCAT, MuSCAT3, Tierras and NGTS, to capture the 19-hour transit of the long-period giant exoplanet HIP 41378 f ($P$ = 542 d, $R$ = 9.5 $R_{\oplus}$) on 31 October 2025. Our transit analysis constrains the time of inferior conjunction to $T_{\mathrm{C}} = 2460980.888 \pm 0.029~\mathrm{BJD_{TDB}}$, occurring $\sim 7$ hours earlier than predicted from its linear ephemeris. This significant offset is consistent with the previously reported TTVs of HIP 41378 f, making it the longest-period exoplanet known to exhibit measurable TTVs. By combining this new precise measurement to the transit timings of the two outer planets in the system (HIP 41378 d and HIP 41378 e), we perform a dynamical modeling of the system, using the N-body integrator TRADES, refine the ephemeris of HIP 41378 f, and predict future transit events for all three outer transiting planets.

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 a coordinated multi-telescope campaign (NEOSSat + LCOGT + MuSCAT + MuSCAT3 + Tierras + NGTS) to observe the 19-hour transit of HIP 41378 f (P=542 d) on 31 October 2025. The derived mid-transit time is T_C = 2460980.888 ± 0.029 BJD_TDB, ~7 hours earlier than the linear ephemeris prediction; this offset is interpreted as a TTV. The new timing is combined with prior measurements of planets d and e in a TRADES N-body dynamical model to refine the outer-system ephemerides and predict future transits.

Significance. If the timing offset is dynamical, the result would establish measurable TTVs for the longest-period known transiting exoplanet and tighten constraints on the outer architecture. The space-plus-ground multi-site strategy is well-matched to the long transit duration, and the TRADES integrator is a standard, reproducible tool for such modeling. The new T_C datum is independent of the prior linear ephemeris.

major comments (1)
  1. [Abstract] Abstract, final paragraph: the claim that the ~7-hour early T_C is produced by gravitational interactions (and is therefore suitable for direct input to the TRADES fit) assumes that non-dynamical contributions are negligible. No explicit alternative model (e.g., Gaussian-process timing noise, site-specific red-noise kernels, or stellar-activity-induced centroid shifts) is presented to test whether the offset could arise from systematics across the six-instrument data set. This assumption is load-bearing for the TTV interpretation and the subsequent dynamical conclusions.

Simulated Author's Rebuttal

1 responses · 0 unresolved

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

read point-by-point responses

  1. Referee: [Abstract] Abstract, final paragraph: the claim that the ~7-hour early T_C is produced by gravitational interactions (and is therefore suitable for direct input to the TRADES fit) assumes that non-dynamical contributions are negligible. No explicit alternative model (e.g., Gaussian-process timing noise, site-specific red-noise kernels, or stellar-activity-induced centroid shifts) is presented to test whether the offset could arise from systematics across the six-instrument data set. This assumption is load-bearing for the TTV interpretation and the subsequent dynamical conclusions.

    Authors: We acknowledge the referee's point that the manuscript does not present explicit alternative models (such as Gaussian processes or red-noise kernels) to quantify the probability that the observed 7-hour offset arises from systematics rather than dynamics. The current interpretation rests on the fact that the offset is detected coherently across six independent instruments (NEOSSat space photometry plus five ground-based facilities with distinct pipelines, filters, and sites), which would require a highly correlated systematic to mimic a dynamical TTV. We also note that the new timing is consistent in sign and approximate amplitude with the TTVs previously reported for HIP 41378 f. Nevertheless, we agree that an explicit discussion strengthens the claim. In the revised manuscript we will expand the discussion section to include a brief assessment of possible non-dynamical contributions (instrumental timing offsets, stellar activity, and correlated noise) and explain why they are unlikely to produce a uniform shift across the heterogeneous dataset. No new modeling is required, but the added text will make the assumption more transparent. revision: yes

Circularity Check

0 steps flagged

New transit timing measurement is independent; no derivation reduces to prior fits by construction

full rationale

The paper's core result is a new photometric determination of T_C = 2460980.888 ± 0.029 BJD_TDB from the 2025 multi-site transit light curve. This datum is compared against a linear ephemeris extrapolated from earlier observations and then supplied as an input to a standard TRADES N-body integration that also incorporates prior timings of planets d and e. No equation in the reported chain defines the measured offset in terms of the TTV model itself, renames a fitted parameter as a prediction, or imports a uniqueness result from self-citation that forces the outcome. The consistency statement with previously reported TTVs is a post-hoc comparison, not a definitional identity. The analysis therefore remains self-contained against external photometric data.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central timing claim rests on standard photometric reduction and the assumption that the offset is dynamical. The modeling step introduces fitted orbital elements whose values are not enumerated in the abstract.

free parameters (2)
  • planet masses and eccentricities in TRADES fit
    N-body modeling of TTVs requires masses and eccentricities that are adjusted to match the observed timings; these are not supplied in the abstract.
  • updated linear ephemeris parameters for d, e, f
    The refined ephemeris is the output of the fit and therefore depends on the choice of which parameters are free versus fixed.
axioms (2)
  • standard math Newtonian N-body dynamics accurately describe the timing variations
    TRADES integrator is invoked without discussion of relativistic or tidal corrections for this system.
  • domain assumption The multi-site photometry has been corrected for all instrumental and atmospheric effects at the level of the quoted 0.029-day uncertainty
    The abstract presents the timing without detailing the reduction pipeline or residual systematics checks.

pith-pipeline@v0.9.1-grok · 6021 in / 1536 out tokens · 25442 ms · 2026-06-26T07:14:05.144819+00:00 · methodology

discussion (0)

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