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arxiv: 2606.09973 · v1 · pith:LYHPBPU6new · submitted 2026-06-08 · 🌌 astro-ph.EP · astro-ph.SR

Stellar Obliquities of Young Systems, Atmospheres Undergoing Contraction and Escape (SOYSAUCE) II: a 135 Myr planet on an aligned orbit with transit timing variations

Madyson G. Barber , Andrew W. Mann , Sydney Vach , Leah J. Boff , Andrew W. Boyle , Andrew Vanderburg , Adam L. Kraus , Benjamin M. Tofflemire
show 11 more authors
Marshall C. Johnson Allyson Bieryla David W. Latham Karen A. Collins Steve B. Howell Richard P. Schwarz Gregorg Srdoc Francis P. Wilkin Felipe Murgas Enric Palle Chris Stockdale
This is my paper

Pith reviewed 2026-06-27 14:42 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords exoplanetsyoung planetsstellar obliquityRossiter-McLaughlin effecttransit timing variationsopen clustersplanet formation
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The pith

A 3.6 Earth-radius planet at 135 million years old shows a near-aligned orbit around its star.

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

The paper validates TIC 150070085 b as a 3.6 Earth-radius planet on a 10.47-day orbit and identifies a candidate second planet, both around a star confirmed as a member of the Alessi 84 cluster. The cluster age is revised to 135 plus or minus 10 million years using color-magnitude diagram, rotation, and variability data. Spectroscopic observations during transit measure the Rossiter-McLaughlin effect and yield a sky-projected obliquity of 18 plus or minus 12 degrees, indicating alignment. Transit timing variations in the first planet's transits support the planetary nature of the second signal near 3:2 resonance. The result adds a young-system data point that connects early formation stages to later planetary evolution.

Core claim

TIC 150070085 b is consistent with a near-aligned orbit with its host star (|λ| = 18 +/- 12°), in line with similarly aged transiting planets with measured λ values. The host star is confirmed as a member of Alessi 84, whose age is updated to 135 +/- 10 Myr from combined CMD, rotation, and variability properties.

What carries the argument

The Rossiter-McLaughlin signal measured with MAROON-X, which determines the sky-projected obliquity angle λ by tracking the distortion of stellar spectral lines during transit.

If this is right

  • Planets in the 100-500 Myr range can have obliquities measured even with active host stars.
  • Alignment at this age is consistent with the pattern seen in other young transiting planets.
  • Transit timing variations can help confirm additional planets in young systems near mean-motion resonance.
  • More systems in this age window are needed to trace how spin-orbit angles evolve from formation to Gyr ages.

Where Pith is reading between the lines

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

  • The 3:2 resonance proximity and TTVs suggest the two planets interact dynamically, which could influence long-term obliquity evolution.
  • If additional young planets are found aligned, models of disk migration or early tidal damping would need to explain why misalignment is rare before 500 Myr.
  • Independent verification of the cluster membership or age through other indicators such as lithium abundance would test the youth classification used here.

Load-bearing premise

The host star is a confirmed member of Alessi 84 whose age can be reliably updated to 135 +/- 10 Myr from the group's combined CMD, rotation, and variability properties.

What would settle it

A follow-up Rossiter-McLaughlin observation that measures |λ| greater than 40 degrees with an uncertainty below 10 degrees would show the orbit is not near-aligned.

Figures

Figures reproduced from arXiv: 2606.09973 by Adam L. Kraus, Allyson Bieryla, Andrew Vanderburg, Andrew W. Boyle, Andrew W. Mann, Benjamin M. Tofflemire, Chris Stockdale, David W. Latham, Enric Palle, Felipe Murgas, Francis P. Wilkin, Gregorg Srdoc, Karen A. Collins, Leah J. Boff, Madyson G. Barber, Marshall C. Johnson, Richard P. Schwarz, Steve B. Howell, Sydney Vach.

Figure 1
Figure 1. Figure 1: Representative result from our SED fitting proce￾dure, including observed (red points) and synthetic (green) photometry, best-fit template (black line) and BT-SETTL model (blue) for TIC 150070085. The vertical error bars indicate the uncertainties in the photometry, while the hori￾zontal bars indicate the filter width. The bottom panel shows the residual in units of standard deviations. yielded relatively … view at source ↗
Figure 2
Figure 2. Figure 2: Adopted members of Alessi 84 (pink outlines) compared to all comoving candidates (circles) colored by the number of membership lists (associations) the star was iden￾tified a member in. TIC 150070085 is shown as the red star. Requiring the candidate be in at least two of the membership lists primarily cuts members of Theia 214 that sit ≳ 5° from the remaining cluster. TIC 150070085 has been previously clus… view at source ↗
Figure 3
Figure 3. Figure 3: Gaia color-magnitude diagram of candidate mem￾bers of Alessi 84. Points are color-coded by their out￾lier likelihood (darker indicates more likely part of the sin￾gle-age single-star population). Green lines show 100 ran￾dom draws from the MCMC posterior. Dashed lines indi￾cate 80 Myr and 200 Myr isochrones from PARSEC for ref￾erence. The inset around the high-mass stars highlights how the handful of high-… view at source ↗
Figure 5
Figure 5. Figure 5: Individual age estimates from variability (EVA), gyrochronology, and the isochrone fit, as well as the com￾bined final age of Alessi 84 (135 ± 10 Myr; purple). All methods agree, although the isochrone fit is the most precise and dominates the final posterior. 5.2.4. Combining age estimates To determine a final age estimate for TIC 150070085, we combined the likelihood distribution from each in￾dividual ag… view at source ↗
Figure 6
Figure 6. Figure 6: Top left: Phase-folded TESS light curve (gray), with stellar variability removed and corrected for transit timing offsets, showing the transit of TIC 150070085 b. The data is binned to 20-minute intervals (purple) for clarity. The best-fit transit models are shown in bright red, with 50 randomly-drawn models from the posterior in dark red. Top right: Phase-folded TESS light curve showing the two transits o… view at source ↗
Figure 7
Figure 7. Figure 7: Sector 20 (top) and Sector 47 (bottom) of the TESS light curve (gray), binned to 30-minute intervals (purple), with the GP stellar variability model shown as the red line. The transit locations of TIC 150070085 b are highlighted in pink, and the locations of candidate TIC 150070085 c are highlighted in blue. Due to the data gap, TIC 150070085 c was not observed in Sector 47, complicating validation of the … view at source ↗
Figure 8
Figure 8. Figure 8: The observed minus expected transit timing of each photometric transit. The TESS data (purple) does not show an obvious offset, but the higher-cadence (43-second) ground-based photometry (green) and the MAROON-X transit (pink) shows a clear TTV signal. The timings of the first three TESS transits are not well constrained due to the sparse, 30-minute data sampling [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Partial transit detections with LCOGT, labeled with the transit number and observation filter. The raw data is shown in gray and 10-minute bins are shown in purple for clarity. The best fit transit is shown as the brown solid line, the predicted transit midpoint (assuming a linear ephemeris) is shown as the black dotted line and the measured transit midpoint is shown as the pink dashed line. the priors and… view at source ↗
Figure 10
Figure 10. Figure 10: Left) MAROON-X relative radial velocities from the blue channel (top, blue circles) and red channel (middle, red squares). The best-fit RM model and stellar RV trend lines are shown as the opaque solid blue and dashed red lines, with 50-sample fits pulled from the posterior shown as the translucent blue and red lines. The bottom plot shows the residuals for each channel, with a 5-minute shift applied to t… view at source ↗
Figure 11
Figure 11. Figure 11: Relative radial velocities of TIC 150070085 col￾ored by the observation’s phase in the stellar rotation (arbi￾trary zero-point) and phased to TIC 150070085 b’s orbital period. The median fit (dotted line) of the TRES (squares) observations is shown, as well as the 1, 2, and 3σ mass lim￾its and the LCO (stars) and MAROON-X (circle) epochs for reference. Epoch Absolute Relative σ Facility (BJD) (km s−1 ) (k… view at source ↗
Figure 12
Figure 12. Figure 12: Distribution of sky-projected spin-orbit alignment estimates (λ) for stars with reported ages. Targets are color-coded by planetary radius. TIC 150070085 is shown as a star. TIC 150070085’s general alignment is consistent with younger < 100 Myr systems, but more targets in the 0.1-1 Gyr range are needed to determine when misalignments start to occur. that are aligned or with small misalignments (≲ 20◦ ) (… view at source ↗
read the original abstract

Young planets (<1 Gyr) provide opportunities to directly probe planet formation and evolution processes in action. However, due to heightened stellar activity, there is a lack of known transiting planets in adolescence (~100-500 Myr). Here we present the validation of TIC 150070085 b, a 3.6 R_E planet on a 10.47 day orbit, and report the candidate TIC 150070085 c, a 3.0 R_E planet on a 15.90 day orbit. While we are unable to validate the second signal, the proximity to mean motion resonance (3:2) and transit timing variations observed in the transits of TIC 150070085 b strongly suggest the signal is planetary. We confirm the host star as a member of Alessi 84 and combine the group's CMD, rotation, and variability properties to update the age to 135 +/- 10 Myr. We additionally use MAROON-X to observe the Rossiter-McLaughlin signal of TIC 150070085 b and measure the sky projected obliquity angle ($\lambda$). We find TIC 150070085 b is consistent with a near-aligned orbit with its host star (|$\lambda$| = 18 +/- 12$^\circ$), in line with similarly aged transiting planets with measured $\lambda$ values. Continued discovery and characterization of planets in this age regime are vital to link planetary infancy (<50 Myr) and maturity (>1 Gyr).

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 / 2 minor

Summary. The manuscript validates TIC 150070085 b (3.6 R_E, P=10.47 d) as a transiting planet, reports a candidate second planet (TIC 150070085 c) whose 3:2 near-resonance and TTVs on b support a planetary interpretation, confirms the host as an Alessi 84 member, updates the cluster age to 135 ± 10 Myr by combining CMD, rotation, and variability data, and measures the sky-projected obliquity via MAROON-X Rossiter-McLaughlin observations yielding |λ| = 18 ± 12°, consistent with other young transiting planets.

Significance. If the membership confirmation and age revision hold, the result supplies a rare obliquity measurement in the 100-500 Myr regime, directly linking the <50 Myr and >1 Gyr populations and testing whether alignment is already established by ~135 Myr.

major comments (1)
  1. [age determination paragraph] Age determination paragraph: the update of Alessi 84 to 135 ± 10 Myr by combining CMD, rotation periods, and variability is presented without quantitative membership probabilities, explicit weighting of the three indicators, or robustness checks against alternate isochrones or field contamination; because this age anchors both the 'young' classification and the comparative statement with other λ measurements, the central claim is load-bearing on this section.
minor comments (2)
  1. [Abstract] Abstract: the notation |λ| = 18 +/- 12° should be written with consistent uncertainty formatting and a brief statement of the RM model assumptions.
  2. [Abstract] The TTV interpretation for the candidate c is asserted from proximity to 3:2 resonance and observed timing variations, but no amplitude, period, or dynamical stability analysis is referenced in the provided abstract.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful review and constructive feedback. We address the single major comment below and will revise the manuscript to strengthen the age determination section as requested.

read point-by-point responses

  1. Referee: [age determination paragraph] Age determination paragraph: the update of Alessi 84 to 135 ± 10 Myr by combining CMD, rotation periods, and variability is presented without quantitative membership probabilities, explicit weighting of the three indicators, or robustness checks against alternate isochrones or field contamination; because this age anchors both the 'young' classification and the comparative statement with other λ measurements, the central claim is load-bearing on this section.

    Authors: We agree that the age determination is central to the paper and that the current presentation would benefit from greater quantitative rigor. In the revised manuscript we will add quantitative membership probabilities for TIC 150070085, provide an explicit description of how the CMD, rotation, and variability indicators are weighted and combined, and include robustness checks using alternate isochrones together with an assessment of field contamination. These additions will be incorporated without changing the reported age value. revision: yes

Circularity Check

0 steps flagged

No circularity; age update and obliquity measurement are independent empirical steps

full rationale

The paper updates the age of Alessi 84 to 135 ± 10 Myr by combining the group's CMD, rotation periods, and variability properties after confirming membership, then reports a direct Rossiter-McLaughlin measurement of λ = 18 ± 12° for the planet. Neither step reduces to a self-definition, fitted input renamed as prediction, or self-citation chain; the age relies on standard stellar indicators applied to the group, and λ is extracted from spectroscopic data without equations that loop back to the reported values by construction. The comparative statement with other young planets draws on external literature values. The derivation chain remains self-contained against external benchmarks with no load-bearing reductions to inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review prevents full audit; the age revision and planet validation rest on unstated assumptions about cluster membership criteria and transit signal validation thresholds that are not enumerated here.

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