Three new exoplanet systems from the Dispersed Matter Planet Project

A.T. Stevenson; C.A. Haswell; D. Alves; D. Staab; E. Rutherford; J.R. Barnes; J.S. Jenkins; L. Fossati; M.R. Standing; Z.O.B. Ross

REVIEW 1 major objections 4 minor 287 references

Three new exoplanet systems from the Dispersed Matter Planet Project

T0 review · 1 major / 4 minor · reviewed 2026-08-16 · deepseek-v4-flash

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Pith's one-line read DMPP-7b: a 0.72-Saturn-mass planet confirmed in a 4.93-day orbit around a bright, slightly evolved star.

desk verdict Solid confirmation of DMPP-7b plus two honest but unconfirmed candidates; title oversells the system count, and the activity-kernel truncation deserves a direct test. read the letter →

arxiv 2608.11902 v1 pith:YWLARHGQ submitted 2026-08-12 astro-ph.EP astro-ph.SR

J.R. Barnes , C.A. Haswell , Z.O.B. Ross , E. Rutherford , M.R. Standing , A.T. Stevenson , D. Staab , L. Fossati

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J.S. Jenkins D. Alves

This is my paper · ORCID

classification astro-ph.EPastro-ph.SR

keywords exoplanetsradialvelocitiesstellaractivityGaussianprocessesBayesianmodelcomparisonshort-periodgiantplanetsNeptuniandesertlow-activitystars

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper aims to establish which of three bright, very low-activity stars selected by the Dispersed Matter Planet Project genuinely host close-orbiting planets once stellar activity is modelled rather than assumed away. Its main claim is that DMPP-7 (HD 118006) hosts one confirmed planet: DMPP-7b, a 0.72-Saturn-mass object with minimum mass $m_\mathrm{p}\sin i = 69.0\pm 1.7\,M_\oplus$ and period $P = 4.92666 \pm 0.00030$ d, supported by very strong Bayesian evidence (Bayes factor $>4564$) and consistent across two independent high-precision spectrograph datasets. The paper also argues that allowing for quasi-periodic stellar activity reverses an earlier two-planet claim for HD 67200, leaving only weak-to-moderate evidence for a $2.07\,M_\oplus$ candidate at $P = 2.67$ d, and moderate evidence for a $2.86\,M_\oplus$ candidate at $P = 2.78$ d around HD 2134. The wider point is methodological: when the number of Keplerian signals is a free parameter inside an activity-aware model, multi-planet claims around quiet stars can be demoted rather than confirmed.

What carries the argument

The mechanism carrying the argument is a joint Bayesian model in which the radial velocities are the sum of an unknown number of Keplerian orbits plus a quasi-periodic Gaussian process representing stellar activity, with activity indicators (the Ca ii H&K S-index, line width, bisector, and line-asymmetry moment) modelled alongside the RVs where they help. The activity kernel is an exponential--sine periodic process with a characteristic period $\eta_3$, a decay timescale $\eta_2$, and a tunable harmonic-complexity parameter $\eta_4$ controlling how much power sits in the rotation period's harmonics; the number of planets $N_\mathrm{p}$ is itself a sampled quantity, and models are compared by global evidence expressed as Bayes factors. This machinery lets the analysis ask directly whether a candidate signal is better described as another planet or as correlated stellar noise --- the question that separates the confirmed DMPP-7b from the still-tentative HD 67200 and HD 2134 candidates.

What would settle it

Continue monitoring DMPP-7's radial velocities across several more stellar rotation cycles while measuring the S-index, line width, and line asymmetry: a dynamical 4.93-day planet must stay phase-coherent with constant amplitude and no matching line-shape variability, whereas a stellar origin should eventually show amplitude or phase drift, a period change, or the same period appearing in the line-shape indicators.

Watch

Extended reading notes

Core claim

The paper's central claim is that DMPP-7 (HD 118006), a bright, slightly evolved early-G star, hosts a single close-orbiting giant planet. Combining two high-precision spectrograph datasets in a Bayesian model where the number of Keplerians and a quasi-periodic Gaussian-process activity component are both free, the authors find very strong evidence for one planet: DMPP-7b, with minimum mass $m_\mathrm{p}\sin i = 68.96^{+1.69}_{-1.66}\,M_\oplus$ (about $0.72$ Saturn masses), period $P = 4.92666 \pm 0.00030$ d, semi-amplitude $K \approx 22.6$ m s$^{-1}$, and low eccentricity $e \approx 0.05$ at $0.0607$ AU. The planet parameters are essentially unchanged whether the residual variability is modelled as a second Keplerian or as correlated activity noise, and the evidence for the planet over activity alone exceeds a Bayes factor of 4564. A longer $21$--$22$ d signal cannot be conclusively assigned to a second planet rather than stellar rotation, and the paper prefers the single-planet-plus-activity reading. The same machinery demotes the previously reported two-planet interpretation of HD 67200 in favour of stellar activity, with only weak-to-moderate evidence for a $P = 2.67$ d, $2.07\,M_\oplus$ candidate; for HD 2134, all models give moderate evidence for a $P = 2.78$ d, $2.86\,M_\oplus$ candidate. No transits are found in the space-based photometry, and DMPP-7b is placed at the transition between the high-radius population and the Neptunian ridge and savannah regions.

Load-bearing premise

The planetary reading of the 4.93-day signal assumes that any stellar activity mimicking it would leave a trace in the spectral-line shapes or be absorbed by the Gaussian process, and that the two spectrograph datasets can be combined with constant per-instrument offsets; if the star instead produces a clean 4.93-day activity signal with no line-shape change, or if the offsets drift between runs, the planetary identification weakens.

Editorial extensions

If this is right

A bright ($V = 8.8$), nearby star hosts a short-period giant whose minimum mass is measured to about 2.4%, making DMPP-7b a strong target for atmospheric, orbital, and formation follow-up.
DMPP-7b's low eccentricity at the edge of the Neptunian ridge and savannah favours disc migration over high-eccentricity (Kozai--Lidov) migration as the origin of close-in giants.
For HD 67200, the earlier two-planet claim (DMPP-6b/c) is superseded: activity modelling changes the inferred architecture, so previously announced multi-planet systems around very quiet stars should be re-examined with the same machinery.
If the HD 67200 and HD 2134 short-period signals are confirmed as planets, they would be $2.07$ and $2.86\,M_\oplus$ objects on 2.67 d and 2.78 d orbits, hot enough ($\approx 1500$--$1650$ K) that the paper argues magma-ocean or wind-driven mass loss could supply the dispersed matter the survey was designed to find.
The absence of transits despite a target-selection bias toward near-edge-on orbits implies inclinations below roughly $82^\circ$--$83^\circ$ if the photometry is not the limiting factor.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

A systematic re-run of this activity-aware machinery on the remaining DMPP survey stars would show how often purely Keplerian multi-planet claims are demoted; the paper demonstrates the effect for one target but does not quantify the rate across the survey.
The $2.78$ d HD 2134 signal sits just above the typical supergranulation timescale; if future data show its coherence breaking, convective jitter could mimic ultra-short-period planets of a few $M_\oplus$ in quiet stars, implying some published masses in this regime are systematically optimistic.
DMPP-7b's predicted radius ($\approx 9.6\,R_\oplus$) lies on the steep part of the mass--radius relation; a single well-timed transit or any direct inclination measurement would test whether the relation holds at exactly this mass.
The success of jointly modelling RVs with the S-index for HD 67200 suggests that future RV campaigns on quiet stars should collect simultaneous activity-indicator timeseries by design, since the rotation signal needed to separate spots from planets is otherwise badly undersampled.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Short version: DMPP-7b is a real detection and worth knowing about; the other two “systems” are still just candidates, and the title oversells them. The paper earns its keep on the strength of the DMPP-7 analysis.

What’s new: fresh ESPRESSO data for DMPP-7, a careful nested-sampling comparison between Keplerian and Gaussian-process models, and an explicit supersession of the earlier DMPP-6b/c interpretation of HD 67200. The DMPP-7b signal is robust: K=22.6 m/s, BF>4564 for GP+Np=1 over GP+Np=0, and the parameters barely move between purely Keplerian and GP models. That consistency is the strongest evidence in the paper.

The modeling is thoughtful. Using Np as a free parameter, fitting RV and activity indicators simultaneously, and honestly labeling the 2.1–2.9 M_Earth signals as moderate evidence are all good practice. The authors also correctly note that RV–activity correlations can be non-stationary, which keeps them from overclaiming what the line-profile non-detections mean.

Where I push back: the stress-test concern about the ESP kernel truncated at n_harm=3. Because the GP cannot represent a fourth rotational harmonic, a Prot/4 signal near 4.93 d would necessarily be absorbed by a Keplerian. On reading the paper, I think this is a legitimate caveat but not a fatal one. A 22.6 m/s RV signal from spots would be unusually large given the star’s photometric quietness (R_var=546 ppm, no 4.9 d term in TESS), and the HARPS/ESPRESSO phase coherence over a long baseline is not what I’d expect from evolving spots. Still, the authors should test the Prot/4 hypothesis directly—by extending the η3 prior below 10 d or by fitting the activity indicators at 4.93 d. As written, the model comparison alone cannot rule it out.

Lesser issues: the title claims “three new exoplanet systems” when the paper itself says only DMPP-7b has strong evidence; the two short-period candidates are correctly framed as unconfirmed and possibly stellar. The data-availability clause (“on reasonable request”) is weak; the kima adaptation is described but no code is released. Minor typos (e.g., “4.297 d” instead of 4.93 d) will be caught in proof.

Who gets value: RV survey folks and anyone working on activity modeling with GPs. The demographic discussion near the Neptunian savannah is fine but not the main draw.

Recommendation: yes, engage with it. A serious referee should ask for the Prot/4 test and a more honest title; neither should change the central detection.

Referee Report

1 major / 4 minor

Summary. The paper presents a radial-velocity analysis of three bright, low-activity stars selected by the Dispersed Matter Planet Project (DMPP), comparing purely Keplerian models with models that include stellar activity via a Gaussian process (GP). For DMPP-7 (HD 118006), the authors claim strong Bayesian evidence for a single short-period giant planet, DMPP-7b, with P = 4.92666 d and m_p sin i = 68.96 M_Earth, based on HARPS and ESPRESSO data and a Bayes factor BF > 4564 in the GP model. A longer 21–22 d period is interpreted as likely stellar rotation, and a second, more tentative 11.8 d signal is not conclusively distinguished from activity. For HD 67200, a GP-only model is strongly favored over the purely dynamical model, with moderate evidence for a 2.67 d Keplerian (m sin i = 2.07 M_Earth). For HD 2134, the paper finds moderate evidence in all models for a 2.78 d Keplerian (m sin i = 2.86 M_Earth), while the 21–32 d signal is associated with tentative FWHM variability. The paper also reports no transit detections in TESS photometry and places DMPP-7b in the transition region between the high-radius population and the Neptunian ridge/savannah.

Significance. If DMPP-7b is confirmed as a planet, it is a precisely characterized Saturn-mass companion (mass uncertainty ~2.4%) on a 4.93 d orbit around a slightly evolved, bright star, adding a useful anchor point for planet formation and migration models. The paper's methodological approach is a strength: it uses nested sampling with the number of Keplerians as a free parameter, computes global model evidences, and jointly models RVs with simultaneous activity indicators using the s+leaf ESP kernel. The two lower-mass candidates are appropriately presented as moderate-evidence detections with explicit caveats that they may be stellar in origin. The explicit comparison of Keplerian and GP models and the discussion of activity-indicator correlations are valuable for interpreting RV surveys of low-activity stars. However, the central claim of a confirmed planet for DMPP-7b depends on the GP's ability to represent all plausible activity signals, which is the focus of the major comment below.

major comments (1)

[Appendix A / §4.2.5, Table 4] The GP activity model uses the s+leaf ESP kernel with n_harm = 3, so it can represent variability at the characteristic period η3 and at η3/2 and η3/3, but not at η3/4. DMPP-7's rotation period is estimated at a median of 20.4 d with a 68.3% range of 12.9–28.3 d, so a fourth rotational harmonic would fall at 3.2–7.1 d, fully encompassing the 4.93 d orbital period of the claimed planet. The paper interprets the 11.8 d and 9.4 d signals as Prot/2 and related aliases, but it never tests whether the strong 4.93 d signal could be a Prot/4 spot harmonic. If such a harmonic is present, the truncated GP cannot absorb it, and the large Bayes factor BF > 4564 for a Keplerian would be a model artefact. The absence of correlations with BIS, FWHM, SMW, and M3 reduces but does not eliminate this possibility, as the authors themselves note in §4.1.7 that RV–activity correlations are not stationary and may be phase-dependent. I request a robustness test, for example by allowing more harmonics in the GP (n_harm ≥ 4) or including an explicit Prot/4 activity term, or an explicit physical argument for why a Prot/4 harmonic is negligible for this star.

minor comments (4)

[§4.2.7] The text states 'the 4.297d planet candidate parameters' where the context clearly indicates P = 4.927 d; this appears to be a typo.
[§5] The equilibrium temperature quoted for HD67200b in §5 is Teff = 616 K, which is inconsistent with Teq = 1650 K (AB = 0) or 1475 K (AB = 0.36) listed in Table 3; please correct the number or the definition used.
[Table 2 and Table 4] The offset parameters are labelled as γp15,p20−15032.84 and γHARPS−36651, which are confusing because the reference value is embedded in the label; recommend defining the zero-point explicitly in the caption.
[§4.1.5] The phrase 'we allowed for harmonics with 3 : 2 and 3 : 1 amplitude contributions of η3/2 and η3/3' is unclear; consider rewording to indicate that the GP kernel permits relative harmonic amplitudes at η3/2 and η3/3 as controlled by η4.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the planet parameters are fitted to the data and the model comparisons are genuine.

full rationale

The central claim for DMPP-7b is derived from a Bayesian fit to HARPS and ESPRESSO radial velocities, with the number of Keplerian signals treated as a free parameter and compared against GP-only activity models. The planet parameters are not defined in terms of the DMPP selection hypothesis, and the strong Bayes factor (BF > 4564) is a genuine model comparison between GP+Np=1 and GP+Np=0. The predicted radii are explicitly labeled as derived from the fitted minimum masses via the external M24 mass-radius relation; this is a conversion from a fitted parameter and is not used as evidence for the planet. Self-citations to Standing et al. (2026) are for data provenance, prior RVs, and prior survey analysis; the present paper re-derives the signals and even supersedes the earlier Keplerian-only interpretation for HD67200. The n_harm=3 truncation of the ESP kernel is a documented modeling limitation that could affect robustness against a hypothetical Prot/4 activity signal, but it is not a circular reduction: the detection is not defined by the kernel truncation, and the same GP is applied in the comparison models. No fitted parameter is renamed as a prediction, no load-bearing result is imported solely from the authors' prior work, and no known empirical pattern is merely re-expressed in new coordinates. Thus the paper exhibits no significant circularity.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The central detections are measurements, not inventions; no new particles, forces, or mediators are introduced. The model parameters listed are fitted quantities or priors that the analysis depends on. External anchors are the stellar parameters (species/Gaia), the M24 mass-radius relation, and the assumed activity kernel.

free parameters (4)

GP hyperparameters eta1, eta2, eta3, eta4 = Posterior values in Tables 2-5; e.g., DMPP-7 eta3 ~ 22.2 d, eta4 ~ 1.46
Part of the quasi-periodic GP activity model; priors (eta3 U[10,100] d, eta4 U[0.8,10], eta2 tied to eta3) are chosen by hand and can absorb or mimic planetary signals, directly influencing the Bayes factors.
Kumaraswamy eccentricity prior shape parameters alpha=0.881, beta=2.878 = alpha=0.881, beta=2.878
Chosen to approximate the Kipping (2013) Beta prior; shapes eccentricity posteriors and, together with AMD stability checks, biases against high-eccentricity solutions.
Per-dataset white noise jitter terms = e.g., DMPP-7 sigma_HARPS ~ 2.3 m/s, sigma_ESPRESSO ~ 1.9 m/s (Table 4)
Fitted additive noise per instrument; absorbs unmodeled scatter and affects detection significance for low-amplitude Keplerian signals.
Per-dataset velocity offsets gamma = e.g., DMPP-7 gamma_ESPRESSO ~ -13 m/s relative to HARPS
Constant offsets between instrument/epoch datasets; the assumption of constancy is needed to combine HARPS and ESPRESSO RVs.

assumptions (5)

domain assumption The quasi-periodic ESP kernel (Eq. A2) with the adopted priors adequately models stellar activity in these low-activity stars.
Used in Models 2 and 3; if misspecified, the GP could absorb real planets or create spurious evidence. The paper tests some prior variations but not all.
domain assumption Bayes factor thresholds from Trotta (2008) and Standing et al. (2022) are reliable for nested sampling evidence comparisons.
Used throughout to classify evidence as strong/moderate/weak; assumes converged DNest4 sampling and unbiased logZ estimates.
domain assumption The Kipping (2013) or Kumaraswamy eccentricity prior matches the true orbital eccentricity distribution.
Applied to all Keplerian fits; combined with AMD stability checks it biases posteriors toward lower eccentricity, affecting candidate parameters.
domain assumption The DMPP target selection and the sub-basal chromospheric emission are linked to close-orbiting, mass-losing planets.
Motivates the survey and the expectation of near edge-on orbits used in the transit non-detection discussion; not directly tested here.
domain assumption The M24 mass-radius relation is valid for predicting radii from minimum masses in this mass and instellation range.
Used to convert m_p sin i to predicted R_p (Tables 2-5); intrinsic scatter dominates the radius uncertainty, and the relation may not apply to highly irradiated planets.

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Pith. "Pith review of Three new exoplanet systems from the Dispersed Matter Planet Project." pith.science (2026). https://pith.science/paper/YWLARHGQ

@misc{pith2026260811902,
  author       = {Pith},
  title        = {Pith review of: Three new exoplanet systems from the Dispersed Matter Planet Project},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YWLARHGQ}},
  note         = {Machine review of arXiv:2608.11902}
}

abstract

We present a radial velocity analysis of three bright, low-activity stars identified by the Dispersed Matter Planet Project (DMPP). We use a Bayesian framework to compare purely Keplerian models with models incorporating stellar activity via a quasi-periodic Gaussian Process (GP). DMPP-7 (HD 118006) is a slightly evolved star that harbours a single 0.72 Saturn-mass giant ($m_\textrm{p}\sin i$ = 69 M$_\oplus$) with an orbital period of P = 4.93 d. A longer 21 d - 22 d period cannot be conclusively confirmed as a stellar rotation signature rather than a purely Keplerian signal. For HD 67200, which exhibits Ca ii H&K variability, a model with only a GP is strongly favoured over a purely dynamical model. The GP model shows moderate evidence for a single Keplerian with P = 2.67 d. For HD 2134, a 21 d - 32 d rotation period signal is associated with tentative FWHM variability. A model with a GP is not conclusively favoured, but all models considered show moderate evidence for an additional single Keplerian with P = 2.78 d. Despite our target selection favouring near edge-on orbital geometries, we find no evidence for transits in TESS photometry. DMPP-7 b lies at the transition between the high-radius population and the Neptunian ridge and savannah regions. Further observations are required to establish whether the coherent short-period HD 67200 and HD 2134 signals are stellar or dynamical in origin. If planetary, the signals correspond to minimum masses of $m_\textrm{p}\sin i$ = 2.07 M$_\oplus$ and $m_\textrm{p}\sin i$ = 2.86 M$_\oplus$

Figures

Figures reproduced from arXiv: 2608.11902 by the authors.

**Figure 1.** Monte Carlo period simulations for each target. The v sin i values derived from species are used for randomly oriented (sinusoidally distributed) axial inclinations (green) and for a fixed i = 90o (light grey). The respective curves using the M16 v sin i estimates are also shown (orange and dark grey). The modal periods, Pˆ, are shown for each distribution. at the ≳ 1000 ppm level, while Boyle et al. (2025) found si… view at source ↗

**Figure 4.** HD 67200 RV correlations with activity indicator metrics. The data are colour coded as in [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗

**Figure 2.** HD 67200 log-likelihood periodograms. Panels (a), (b) and (c) show the recursive RV periodograms. The corresponding activity periodograms are shown for (d) BIS and M3 and (e) SMW and FWHM. Significant power is only seen in SMW centred around 15.99 d (grey tick). The window function in (f) shows significant peaks at 12.1, 16.3, 17.1, 18.8 and 34.5 d (highlighted by the vertical dashed lines in all panels). -0.005 0 … view at source ↗

Figures from the paper (13 more)

**Figure 3.** Figure 3: SMW phased on the P = 15.99 d period in [PITH_FULL_IMAGE:figures/full_fig_p005_3.png]

**Figure 5.** Figure 5: Solution curves for the HD 67200 RVs. The purely Keplerian solutions are shown in (a) for Np = 2 (Model 1a) and in (b) for the Np = 3 (Model 1b). The GP + Keplerian solutions are shown in (c) for Np = 0 (Model 2a) and in (d) for Np = 1 (Model 2b). See [PITH_FULL_IMAGE…

**Figure 6.** Figure 6: HD 67200 solution curves for simultaneous RV + SMW models for (a) a pure GP with Np = 0 (Model 3a) and (b) the GP + Np = 1 solution (Model 3b). This behaviour was also demonstrated between RVs and the second line moment of the RV CCF, M2, in Barnes et al. (2024). Solar…

**Figure 7.** Figure 7: HD 67200 phase-folded RVs for the purely Keplerian models with (a) Np = 2 (Model 1a) and (b) Np = 3 (Model 1b). Shown in (c) are the Keplerian phase-folds with Np = 1 (Model 2b and preferred Model 3b, highlighted in bold) after subtracting the GP components. The nightl…

**Figure 8.** Figure 8: DMPP-7 RV and activity periodograms as in [PITH_FULL_IMAGE:figures/full_fig_p013_8.png]

**Figure 9.** Figure 9: DMPP-7 Activity vs RV for the P110 and P114 observations indicating no significant correlations. tentative HD 67200 b candidate ( [PITH_FULL_IMAGE:figures/full_fig_p013_9.png]

**Figure 10.** Figure 10: Solution curves for the DMPP-7 RVs. The purely Keplerian solutions are shown in (a) for Np = 1 (Model 1a) and in (b) for the Np = 2 (Model 1b). The GP + Keplerian solution is shown in (c) for Np = 1 (Model 2). See [PITH_FULL_IMAGE:figures/full_fig_p014_10.png]

**Figure 12.** Figure 12: HD 2134 RV and activity periodograms showing (a) recursive log-likelihood periodograms, (b,c) activity periodograms and (d) the corresponding Window function with periods at 24.2 d and 31.2 d plotted as vertical dashed lines in all panels. tionships from Barnes et al.…

**Figure 13.** Figure 13: HD 2134 activity vs RV indicators correlations. The data are colour coded according to observing runs in ESO Periods P95, P97, P98 and P99. that even sky background subtraction would probably not yield activity above the basal flux level [PITH_FULL_IMAGE:figures/full…

**Figure 14.** Figure 14: Solution curves for the HD 2134 RVs. The purely Keplerian solutions are shown in (a) for Np = 1 (Model 1a) and in (b) for the Np = 2 (Model 1b). The moderately significant GP + Keplerian solution is shown in (c) for Np = 1 (Model 2). See [PITH_FULL_IMAGE:figures/full…

**Figure 15.** Figure 15: The HD 2134 moderately significant GP + Keplerian solution for Np = 1 (Model 3) using simultaneous RV (upper panels) and FWHM data (lower panels). See [PITH_FULL_IMAGE:figures/full_fig_p020_15.png]

**Figure 16.** Figure 16: HD 2134 phase-folded RVs for the purely Keplerian models with (a) Np = 1 (Model 1a) and (b) Np = 2 (Model 1b). Shown in (c) are the Keplerian phase-folds with Np = 1 (Model 2 and preferred Model 3, highlighted in bold) after subtracting the GP components. found. From …

**Figure 17.** Figure 17: shows that the HD 67200 b and HD 2134 b candidates, which lie below the radius valley with respective Teff = 1650 and 1487 K (AB = 0), are likely to be atmosphereless planets that could be responsible for mass-loss in these systems. Given their implied equilibrium t…

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Pith tools

Reviewed August 16, 2026 · model on record in the stance chip above.

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