REVIEW 2 minor 2 cited by
The SPHERE infrared survey for exoplanets (SHINE) V. Full sample characterization
T0 review · 0 major / 2 minor · reviewed 2026-07-01 · grok-4.3
Pith's one-line read SHINE survey constructs a vetted subsample of 333 stars spanning ages and masses for direct-imaging exoplanet statistics.
desk verdict This paper defines the 333-star vetted subsample from SHINE's 460 targets using standard age and binarity methods, which is necessary groundwork but not a methodological advance. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
Homogeneous stellar property derivation via kinematic indicators, lithium abundance, rotation, activity, isochrone fitting, combined with binarity vetting from astrometric, spectroscopic, and imaging data.
What would settle it
A significant fraction of stars in the subsample later shown to have undetected companions or to have ages inconsistent with independent methods such as asteroseismology.
Extended reading notes
Core claim
The SHINE survey observed 460 stars and, after homogeneous derivation of stellar properties and thorough vetting for binarity, constructed a subsample of 333 stars covering a large extent of stellar ages and masses to be used as a starting point for the final statistical analysis of the survey.
Load-bearing premise
The combination of kinematic indicators, lithium abundance, rotation, activity, and isochrone fitting yields reliable ages and the binarity vetting is complete enough to produce an unbiased statistical sample.
Editorial extensions
If this is right
- The 333-star subsample supports derivation of unbiased exoplanet occurrence rates at 5-300 au.
- The sample enables direct comparison of direct-imaging results with occurrence statistics from radial velocity and transit surveys.
- The wide coverage in stellar mass and age allows tests of how planet formation efficiency varies with host properties.
- The vetted sample provides a reference catalog for follow-up observations with future high-contrast imagers.
Reading between the lines
- Cross-matching this sample with Gaia data releases could further refine membership in young moving groups.
- The characterization methods could be applied to upcoming direct-imaging surveys to maintain consistency across datasets.
- If age estimates prove robust, the sample may help calibrate gyrochronology relations for field stars.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper reports the full SHINE sample of 460 stars observed with SPHERE/VLT (2015-2023), homogeneously derives stellar ages and properties via kinematic membership, lithium abundance, rotation, activity, and isochrone fitting, performs binarity vetting with astrometric/spectroscopic/imaging data, and defines a 333-star subsample of young single hosts spanning a range of ages and masses for subsequent statistical analysis of direct-imaging exoplanet occurrence.
Significance. If the age and binarity characterizations hold, the subsample supplies a large, homogeneously characterized reference set for occurrence-rate studies at 5-300 au, complementing transit and RV statistics and enabling tighter constraints on outer-planet formation models. The use of multiple standard age diagnostics and multi-technique binarity vetting is a positive feature for reproducibility.
minor comments (2)
- The abstract states that 'selection criteria, global features, as well as the properties of individual stars are reported and discussed,' yet no explicit table or section reference is given for the final 333-star selection cuts; adding a dedicated table listing the quantitative thresholds applied to each age and binarity indicator would improve clarity.
- Error bars or uncertainty ranges on the derived ages and masses are not mentioned in the provided abstract; the manuscript should state how uncertainties from the combined kinematic/lithium/isochrone methods are propagated and reported for the subsample.
Simulated Author's Rebuttal
We thank the referee for their supportive summary of our manuscript and the recommendation for minor revision. The referee's description accurately captures the scope of the SHINE full-sample characterization, including the homogeneous derivation of stellar properties and the definition of the 333-star young single subsample.
Circularity Check
No significant circularity
full rationale
The paper's central activity is homogeneous application of standard, externally established methods (kinematic membership, lithium, rotation, activity, isochrone fitting for ages; astrometric/spectroscopic/imaging vetting for binarity) to observational data to construct a 333-star subsample. No load-bearing step reduces by the paper's own equations or self-citation to a definition or fit supplied by the authors themselves. The process is data-driven selection, not a closed derivation.
Assumptions & free parameters
assumptions (2)
- domain assumption Isochrone fitting, lithium abundance, rotation, and activity provide reliable stellar ages when combined with kinematic membership.
- domain assumption Combined astrometric, spectroscopic, and imaging data yield a complete binarity census.
Cite this review
Pith. "Pith review of The SPHERE infrared survey for exoplanets (SHINE) V. Full sample characterization." pith.science (2026). https://pith.science/paper/ND5BXNZO
@misc{pith2026260527247,
author = {Pith},
title = {Pith review of: The SPHERE infrared survey for exoplanets (SHINE) V. Full sample characterization},
year = {2026},
howpublished = {\url{https://pith.science/paper/ND5BXNZO}},
note = {Machine review of arXiv:2605.27247}
}
read the original abstract
Unbiased surveys of large stellar samples are the prime means through which the prevalence of exoplanets can be derived, and crucial constraints to planet formation models can be set. Direct imaging (DI) is ideally positioned to probe the outer regions (5-300au) of planetary systems, providing complementary information to techniques such as transits and radial velocities. We present the full sample of the SpHere INfrared survey for Exoplanets (SHINE), the second largest DI campaign to date. SHINE observed 460 stars between 2015 and 2023 thanks to the guaranteed time observations (GTO) allocated by ESO to the SPHERE consortium at VLT. The goal of this paper is to homogeneously derive the stellar properties of the targets and to define a subsample of young single hosts to be used as a starting point for the final statistical analysis of the survey. Stellar ages were determined based on kinematic indicators (such as the membership to young moving groups), age diagnostics (lithium abundance, rotation, activity), and isochrone fitting. A thorough vetting for binarity was undertaken combining astrometric, spectroscopic, and imaging data. A subsample of 333 stars, covering a large extent of stellar ages and masses, was constructed. Selection criteria, global features, as well as the properties of individual stars are reported and discussed.
Figures
Figures from the paper (2 more)
Forward citations
Cited by 2 Pith papers
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SaNDi-SHoP: Searching for Satellites'N'Disks with a Star-Hopping Program II. Spectrophotometric analysis and orbital monitoring of directly imaged companions
Thirteen directly imaged substellar companions get updated SPHERE photometry, three get low-resolution spectra, and four get their first orbital solutions; all fitted orbits favor non-zero eccentricity.
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SAXO+, the second-stage adaptive optics for SPHERE: NCPA compensation and dark-hole loop with a pyramid wavefront sensor
Monte Carlo Zemax modeling predicts SAXO+ NCPAs of 27±8 nm RMS, consistent with SPHERE, and a three-step calibration offloads static correction onto the first-stage DM while preserving second-stage stroke.
Reference graph
Works this paper leans on
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[1]
with a significant RUWE ((S/N)RUWE =7.3). The star has AstroSpectroSB1 solution in Gaia-NSS, with nominal mass in the substellar regime (Marcussen & Albrecht 2023). This is confirmed by our independentGaiaPMEXanalysis; therefore, we retained it in the statistical sample. Appendix B: Notes on individual objects in the statistical sample: new targets 2MASS ...
work page 2023
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[2]
and its rotational period fromvsini(P=15.30 d; Reiners et al. 2018) suggest an aget ⋆ =1.0±0.3 Gyr. HIP 37349=HD 61606A=V869 Mon.Very nearby (d=14 pc) wide binary system with HD 61606B (ρ=57.9”∼ 815 au). Both components were included in the sample and observed in the SHINE survey. Age from Vigan et al. (2017). HIP 40706.Field early type (A8V) star. We ado...
work page 2018
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[3]
(2024) argue instead for membership to the Theia92 group, with an age of 35 Myr
Vach et al. (2024) argue instead for membership to the Theia92 group, with an age of 35 Myr. EW(Li),P rot,R X are fully compatible with an age of about 40 Myr, independently confirmed by isochrone fitting. Appendix C: Notes on individual objects: removed stars C.1. Multiple stars 2MASS J02000918-8025009=TYC 9357-1011-1.It was in- cluded in the sample as a...
work page 2024
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[4]
In Gaia DR3 a large RUWE and astrometric acceleration (acceleration 9) are reported. Highly discrepant SpT in the literature (M1 vs.K3.7). Photo- metric colors are fully compatible with K3.7 classification by Kraus et al. (2014). The position on CMD is not on pre-MS after correction of the magnitudes for binarity, further ex- cluding the THA membership. T...
work page 2014
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[5]
and PMa ((S/N) PMa =19) clearly indicate the presence of a companion, whose minimum mass lies in the substellar regime (M=60M Jup). A mass of 0.091M ⊙ for this compan- ion was inferred by Gratton et al. (2025) in a similar anal- ysis. The star has a wide companion UCAC4 311-003056 at 59.34", with slightly discrepant astrometric parameters likely due to th...
work page 2025
Reviewed July 1, 2026 · model on record in the stance chip above.
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