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CORALIE radial-velocity search for companions around evolved stars (CASCADES) IV: New planetary systems around HD 87816, HD 94890, and HD 102888 and an update on HD 121056

T0 review · 2 major / 4 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Five new massive planets orbit three evolved giant stars, and the outer planet of a fourth system gets a revised orbit.

desk verdict Four secure planets and a useful period update, with a fifth planet that is an honest but overcounted long-period signal. read the letter →

arxiv 2505.14317 v2 pith:6NNRCELU submitted 2025-05-20 astro-ph.EP astro-ph.SR

E. Fontanet , S. Udry , D. Ségransan , P. Figueira , J. A. Acevedo Barroso , B. Akinsanmi , M. Attia , M. Battley
show 20 more authors
S. Bhatnagar M. Bugatti Y. Carteret H. Chakraborty A. Deline C. Farret Jentink Y.G.C. Frensch M. Houelle B. Lavie C. Lovis M. Mayor A. Nigioni G. Ottoni F. Pepe D. J. M. Petit dit de la Roche M. Shinde N. C. Santos S. Tavella N. Unger G. Viviani
This is my paper · ORCID
classification astro-ph.EPastro-ph.SR
keywords radial-velocitymethodgiantstarsevolvedmulti-planetsystemsexoplanetdemographicsCORALIEspectrographCASCADESsurveybrowndwarfcompanion
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

This paper reports five new massive planets detected by radial-velocity monitoring of three evolved giant stars, plus a distant candidate companion and a revised orbit for an outer planet in a fourth system. After more than ten years of CORALIE measurements per target, the authors identify periodic Keplerian signals in the velocity time series of HD 87816, HD 94890, and HD 102888, check them against activity indicators such as line width, bisector, and H-alpha, and conclude that the signals are true companions rather than stellar variability or instrumental jumps. The result matters because planets around intermediate-mass stars that have left the main sequence remain rare, so each secure system helps constrain how planet formation and survival depend on stellar mass and evolution.

What carries the argument

The machinery is an iterative periodogram-plus-Keplerian pipeline: a periodogram search finds the strongest peak, a Keplerian model is fit to it, the model is subtracted, and the search repeats until no peak with false-alarm probability below 1 percent remains. The final parameters come from a Markov chain Monte Carlo sampler that fits period, semi-amplitude, mean longitude, and eccentricity-related parameters, with separate velocity zero-points for the three generations of CORALIE, per-instrument precisions, and a global stellar jitter term. The activity diagnostics serve as the main discriminator between planetary signals and stellar oscillations or convection.

What would settle it

Continue observing HD 87816 past one full period of the claimed 7600-day companion with the current instrument configuration alone. If the signal is real, the velocity curve should close and the fitted period and offsets should remain consistent as new data arrive; if it is an offset artifact, the apparent period will drift or break coherence. A second test: recover the 519-day FWHM signal after the next periastron passage; if it correlates with the 484-day radial-velocity signal, the inner planet's interpretation would need revision.

Watch

Extended reading notes

Core claim

On the paper's terms, HD 87816 hosts an eccentric 6.7 Jupiter-mass planet at 484 days and a 12.2 Jupiter-mass companion at roughly 7600 days; HD 94890 hosts a 2.1 Jupiter-mass planet at 824 days and an 8.9 Jupiter-mass planet at 2492 days, with a period ratio close to 3 suggesting a possible 3:1 resonance; and HD 102888 hosts a 5.7 Jupiter-mass planet at 252 days plus a linear trend consistent with an unseen substellar companion at tens of AU. The paper also confirms the 89-day inner planet of HD 121056 and fixes the outer companion at about 3128 days rather than earlier values near 2130, 2200, or 3920 days. No significant periodicity or correlation with the radial velocities is found in the FWHM, bisector, or H-alpha activity indicators for any system, which the authors take as evidence that the velocity signals are planetary.

Load-bearing premise

The load-bearing assumption is that the long-period signal around HD 87816 is a real Keplerian companion and not an artifact of combining three generations of instrument zero-point offsets; if that offset model is wrong, or if the 519-day FWHM variation shares a stellar origin with the 484-day radial-velocity signal, the outer planet and the total planet count would be affected.

Editorial extensions

If this is right

  • The giant-star planet population gains five members, including two multi-planet systems, strengthening demographic statistics for intermediate-mass hosts.
  • The HD 94890 period ratio near 3:1 suggests a possible resonant pair; if confirmed by dynamical modelling, it would be a rare resonance among evolved-star planets.
  • HD 102888's linear trend implies a likely substellar companion, potentially a brown dwarf of roughly 14 Jupiter masses at 20 AU, 30 at 30 AU, or 57 at 40 AU.
  • The revised 3128-day period for HD 121056 c, with data spanning a full orbit, resolves earlier discrepancies and gives a more reliable minimum mass near 5 Jupiter masses.
  • If the roughly 7600-day signal around HD 87816 c survives further monitoring, it will be one of the longest-period planets known around a giant star.

Reading between the lines

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

  • Editorial inference: if the HD 87816 c signal is real, the system joins a small set of giant-star hosts with a very wide companion, and the correlation between its period and the instrument offsets suggests the stated uncertainty may be underestimated; independent radial-velocity data from another spectrograph could settle this.
  • Editorial inference: the near 3:1 period ratio in HD 94890 offers a natural test of resonance capture and orbital migration around post-main-sequence stars; a dynamical fit including planet-planet interactions could constrain the orbital inclinations and true masses.
  • Editorial inference: the HD 102888 linear trend could be followed with future astrometric monitoring or direct imaging; a roughly 14 Jupiter-mass companion at about 20 AU should be detectable at the system's distance.
  • Editorial inference: all five new planets orbit outside the expected engulfment zone, consistent with the picture that close-in planets are destroyed as their stars evolve off the main sequence.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. The paper presents a radial-velocity analysis of four evolved stars observed with CORALIE (and, for HD 121056, also FEROS and CHIRON) over more than a decade. Using iterative periodogram analysis followed by MCMC Keplerian fitting, the authors report the discovery of five new massive planets around three stars (HD 87816 b and c, HD 94890 b and c, HD 102888 b), a distant unseen substellar companion around HD 102888, and a revised orbital period for the outer companion in the known HD 121056 system. The analysis includes checks against stellar activity indicators (FWHM, BIS, H-alpha) and a genuine out-of-fit test for HD 87816 b through a targeted periastron observing campaign.

Significance. If the detections hold, the paper adds five (or four secure plus one candidate) members to the relatively sparse population of planets around intermediate-mass giant stars, including a very eccentric inner planet (HD 87816 b, e=0.78) and a possible 3:1 mean-motion resonance pair (HD 94890 b and c). A notable strength is the predicted and observed periastron passage of HD 87816 b, which provides an independent validation of the orbital solution. The paper also makes its RV data publicly available and includes MCMC corner plots for all systems. The main weakness is that one of the five claimed planets, HD 87816 c, has a period longer than the observing baseline and is strongly degenerate with the instrument zero-point offsets, as the paper itself notes.

major comments (2)
  1. [Section 4.1, Table 4, Fig. B.2] The detection of HD 87816 c is not secure under the paper's own stated criteria: its best-fit period (7596 days) exceeds the 18-year observing baseline, and the MCMC corner plot in Fig. B.2 shows clear correlations between P_c and the three CORALIE zero-point offsets. The text explicitly says that the period cannot be easily constrained and that the large uncertainties arise from this degeneracy, and it refers to the two signals as 'two candidates.' Nevertheless, the abstract and Section 5 count HD 87816 c among 'five new massive planets.' The manuscript should either provide a formal model comparison between the two-planet model and a one-planet plus acceleration (trend) model, reporting the significance (e.g., FAP or Bayesian evidence) of the second Keplerian component after accounting for the trend, or should reclassify HD 87816 c as a candidate and adjust the abstract and conclusion accordingly.
  2. [Section 4.1, Fig. A.1a] The 519-day FWHM periodicity that appeared after the high-cadence periastron campaign is close to the 484-day period of HD 87816 b, and the paper states that its origin remains unclear. While the authors report that the peaks are separated in frequency and that no correlation between FWHM and RVs was found, a more quantitative demonstration would be appropriate, for instance a joint fit of the RVs with the FWHM as an activity proxy or a periodogram of the RVs after conditioning on the FWHM variation. This is not a fatal concern given the out-of-fit periastron observation, but it is load-bearing for the confirmation of HD 87816 b and should be addressed explicitly.
minor comments (4)
  1. [Section 4.2] The period ratio of HD 94890 b and c is very close to 3:1, suggesting a possible mean-motion resonance. A brief dynamical stability check or an explicit statement about the expected interaction timescale would be a useful addition, although the current two-Keplerian fit is adequate for the detection claim.
  2. [Section 4.3, Eq. (1)] The mass estimate for the unseen companion HD 102888 c assumes a circular orbit and a companion mass much smaller than the stellar mass. These assumptions should be stated explicitly, and a short discussion of how the estimate would change for moderate eccentricities or inclinations would help the reader judge the robustness of the 'potentially substellar' classification.
  3. [Table 7] The previously published values for the period and especially the periapsis argument of HD 121056 c vary widely (P_c from about 2130 to 3920 days, omega_c from 166 to 321 degrees). A brief explanation of why the new, longer-baseline solution, with P_c=3128 d, breaks this degeneracy (e.g., a spectral window analysis or an explicit comparison of the phase coverage) would strengthen the proposed update.
  4. [Abstract and Introduction] Minor wording issues: 'offthe' in the abstract should be 'off the', and the reference list entry for Schwab et al. (2012) contains 'V ol.' instead of 'Vol.' These do not affect the science.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the reported planets are empirical RV fits, and the flagged HD 87816 c degeneracy is a robustness concern, not a by-construction reduction.

full rationale

The planet detections in this paper are empirical fits to radial-velocity time series, not consequences derived from input assumptions. The detection chain is periodogram search, iterative Keplerian fitting, and MCMC refinement; the reported periods, semi-amplitudes, eccentricities, and minimum masses are the fitted parameters themselves. No fitted constant is relabeled as a prediction: the periastron passage of HD 87816 b was predicted from an earlier fit and then observed with increased cadence, which is a genuine out-of-fit test. The one caveat worth flagging, HD 87816 c, is a model-degeneracy or robustness concern rather than circularity. Section 4.1 states that the period "exceeds the time span of our observations, its value cannot be easily constrained from our analysis," and that Fig. B.2 shows correlations between the period and the three CORALIE zero-point offsets. That means the outer candidate may be insecure or degenerate with the offset model, but the candidate is not defined as the offset values, nor is the two-planet model derived from the offsets by construction; the paper simply fits both. Self-citations to Ottoni et al. (2022) supply the stellar parameters used to convert measured semi-amplitudes into minimum masses; those parameters are inputs to the characterization, not outputs of the discovery pipeline, and the cited work is independently published prior survey analysis. There is no uniqueness theorem imported from the authors, no ansatz smuggled in via citation, and no renaming of a known empirical pattern as new organization. The central claims therefore have independent content and the derivation chain is self-contained against the RV data.

Assumptions & free parameters 5 free parameters · 7 assumptions · 1 invented entities

The results are empirical fits to RV data. The main auxiliary inputs are instrument offsets and jitter terms (fitted), stellar masses taken from the same survey's earlier isochrone analysis, and the assumption that Keplerian signals plus offsets fully describe the data. No new physics or exotic entities are introduced; HD 102888 c is an inferred companion with a falsifiable mass-distance relation.

free parameters (5)
  • sigma_jit (stellar jitter per target) = 7.65, 10.92, 8.66, 10.63 m/s (per star)
    Added to the likelihood to absorb stellar activity noise; fit with uniform prior U(0,30) m/s, rather than derived from physics.
  • Instrument zero-point offsets gamma (COR98/COR07/COR14, CHIRON, FEROS) = Table values in m/s, e.g. gamma_COR14 around 5596 m/s for HD 87816
    Required to combine data from different instrument setups over 12 to 18 years; the offset between versions is degenerate with the long-period signal of HD 87816 c (Fig. B.2).
  • Instrument stability sigma_CHIRON and sigma_FEROS = 2.39 and 3.41 m/s for HD 121056
    Additional white-noise terms fitted in the combined HD 121056 analysis.
  • Companion semi-major axis a_c of HD 102888 c = not measured; examples at 10, 20, 30, 40 AU
    The substellar companion is observed only as a linear trend; converting the trend to a mass requires assuming a_c, yielding m_c sin i_c ~ 3.6 (a_c/10 AU)^2 M_Jup (Eq. 1).
  • CORALIE per-version stability sigma_COR98/07/14 = 5, 8, 3 m/s
    Fixed from separate analysis of quiet stars and used as known precisions in the likelihood; affects the relative weighting of the three instrument epochs.
assumptions (7)
  • domain assumption Each detected signal is a single Keplerian orbit and planet-planet interactions are negligible.
    The RV model is a sum of independent Keplerians; no dynamical interaction is modeled even for the near 3:1 pair HD 94890 b/c (Sect. 4.2).
  • domain assumption The three CORALIE versions have constant RV zero-point offsets over their respective epochs.
    Data are treated as coming from different instruments; any intra-epoch drift would be absorbed into the offsets and could bias long periods (Sect. 2.2, Fig. B.2).
  • domain assumption Stellar masses from SPInS isochrone fitting (Ottoni et al. 2022) are accurate enough to convert K into m sin i.
    The paper cites Ottoni et al. (2022) for M* and notes SPInS masses are on average overestimated relative to asteroseismology; m sin i scales with M*^(2/3).
  • standard math FAP threshold of 1% from generalized Lomb-Scargle periodograms is a valid detection criterion for these sparse, unevenly sampled data.
    Used to select peaks for Keplerian fitting (Sect. 4).
  • domain assumption Absence of correlation with FWHM, BIS, and H-alpha means the RV signals are not stellar activity.
    Activity checks are limited to these three indicators; for giant stars the paper itself notes activity can produce RV variations over a wide range of periods and amplitudes (Sect. 1).
  • domain assumption For HD 102888 c, the companion is on a circular orbit and has mass much smaller than the star, so gamma_dot ~ G M_c sin i_c / a_c^2.
    Used to convert the fitted linear trend into a mass-distance relation (Eq. 1, Sect. 4.3).
  • domain assumption Secular acceleration corrections are negligible at these distances.
    Stated in Sect. 4; only affects long-term trend interpretation.
invented entities (1)
  • HD 102888 c (unseen companion) independent evidence
    purpose: Explains the residual linear RV trend of 6.4 m/s/yr after subtracting the 252-day planet.
    It is not directly detected; its existence is inferred from an acceleration, and its mass-distance relation is given. It is falsifiable through continued RV monitoring, astrometry, or direct imaging.

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Cite this review

Pith. "Pith review of CORALIE radial-velocity search for companions around evolved stars (CASCADES) IV: New planetary systems around HD 87816, HD 94890, and HD 102888 and an update on HD 121056." pith.science (2026). https://pith.science/paper/6NNRCELU

@misc{pith2026250514317,
  author       = {Pith},
  title        = {Pith review of: CORALIE radial-velocity search for companions around evolved stars (CASCADES) IV: New planetary systems around HD 87816, HD 94890, and HD 102888 and an update on HD 121056},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6NNRCELU}},
  note         = {Machine review of arXiv:2505.14317}
}
abstract

With around 200 detections of exoplanets around giant stars to date, our knowledge of the population of exoplanets orbiting evolved hosts more massive than the Sun remains limited. The CORALIE radial-velocity search for companions around evolved stars (CASCADES) was launched in 2006 with the aim of improving our understanding of the demographics of exoplanets around intermediate-mass stars, by studying them once they have evolved off the main sequence. We intend to refine the current sample of known exoplanets orbiting intermediate-mass (1.5 - 5 M$_\odot$) giant stars of spectral types G and early K. We searched for exoplanets orbiting the four stars HD 87816, HD 94890, HD 102888, and HD 121056. We used data obtained with the CORALIE spectrograph, mounted on the Leonhard Euler Swiss telescope located at La Silla Observatory in Chile. We gathered high-precision radial-velocity measurements over more than ten years for each of the aforementioned targets. We started by performing a search for periodic signals in the radial-velocity time series of the four targets by using periodograms. Following this, we fit for a Keplerian model using the significant peak with the highest power of the periodogram as the starting guess for the period. We then subtracted this model and repeated the procedure iteratively on the residuals until no significant peaks were found. Finally, to explore the posterior distribution of our models, the final solution was determined using a Markov chain Monte Carlo approach. We report the discovery of five new massive planets around HD 87816, HD 94890, and HD 102888 as well as the presence of a distant, potentially substellar, companion around HD 102888. We confirm the presence of a previously announced exoplanet orbiting the HD 121056 multi-object system with a period of 89 days and propose an update to the period of the outer companion.

Figures

Figures reproduced from arXiv: 2505.14317 by the authors.

Figure 1
Figure 1. CASCADES sample. Gray dots show all the stars of the [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Exoplanet detections around giant stellar hosts (log [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 4
Figure 4. Top: Periodogram of the RV time series of HD 87816. [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figures from the paper (10 more)
Figure 3
Figure 3. Figure 3: Top: RV time series of HD 87816 obtained between 2007 [PITH_FULL_IMAGE:figures/full_fig_p005_3.png]
Figure 6
Figure 6. Figure 6: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p006_6.png]
Figure 7
Figure 7. Figure 7: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p006_7.png]
Figure 8
Figure 8. Figure 8: Top: Phase-folded orbit of HD 94890 b obtained with [PITH_FULL_IMAGE:figures/full_fig_p006_8.png]
Figure 9
Figure 9. Figure 9: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p007_9.png]
Figure 10
Figure 10. Figure 10: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p007_10.png]
Figure 11
Figure 11. Figure 11: Phase-folded RV data of HD 102888 with the period of [PITH_FULL_IMAGE:figures/full_fig_p007_11.png]
Figure 13
Figure 13. Figure 13: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p008_13.png]
Figure 14
Figure 14. Figure 14: Top: Phase-folded RVs of HD 121056 b obtained with [PITH_FULL_IMAGE:figures/full_fig_p008_14.png]
Figure 12
Figure 12. Figure 12: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p008_12.png]

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Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.