SaNDi-SHoP: Searching for Satellites'N'Disks with a Star-Hopping Program II. Spectrophotometric analysis and orbital monitoring of directly imaged companions

Alice Zurlo; Andrea Bernardi; Anuroop Dasgupta; Cecilia Lazzoni; Dino Mesa; Domenico Barbato; Pedro Henrique Nogueira; Sebastian P\'erez; Silvano Desidera

REVIEW 4 major objections 5 minor 152 references

SaNDi-SHoP: Searching for Satellites'N'Disks with a Star-Hopping Program II. Spectrophotometric analysis and orbital monitoring of directly imaged companions

T0 review · 4 major / 5 minor · reviewed 2026-08-02 · deepseek-v4-flash

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Pith's one-line read This paper uses 13 directly imaged planets and brown dwarfs to argue that wide-orbiting substellar companions are systematically eccentric, pointing to formation by gravitational fragmentation or dynamical scattering rather than core accret

desk verdict Useful astrometric and photometric survey, but the 'all non-circular' conclusion outruns what short-arc orbits can support. read the letter →

arxiv 2607.13545 v1 pith:5KR372C2 submitted 2026-07-15 astro-ph.EP

Andrea Bernardi , Alice Zurlo , Cecilia Lazzoni , Silvano Desidera , Dino Mesa , Sebastian Pérez , Pedro Henrique Nogueira , Domenico Barbato

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Anuroop Dasgupta

This is my paper

classification astro-ph.EP

keywords directlyimagedcompanionswide-orbitplanetsbrowndwarfsorbitaleccentricityKeplerianorbitfittingnear-infraredspectroscopyspectralclassificationhigh-contrastimaging

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 is a survey of 13 directly imaged planets and brown dwarfs, adding new near-infrared photometry and astrometry and combining them with archival measurements to fit Keplerian orbits. For four companions—CT Cha b, HIP 78530 B, HIP 64892 B, and RX J1609.5-2105 b—these are the first orbital solutions. The central result is that every companion is consistent with a non-circular orbit, with fitted eccentricities between roughly 0.2 and 0.8. The authors read this as evidence against core-accretion formation inside a circumstellar disk and in favor of gravitational fragmentation or dynamical scattering, consistent with the very wide separations observed. A sympathetic reader cares because this shifts the default formation story for an entire class of massive, wide-orbiting companions and sharpens what future astrometric monitoring needs to confirm.

What carries the argument

The central object is the 13-companion sample; the carrying mechanism is Keplerian orbit fitting of high-contrast-imaging astrometry, supplemented where available by absolute proper-motion anomalies and radial-velocity time series, using a parallel-tempered Markov-chain Monte Carlo sampler to map posterior distributions over semimajor axis, eccentricity, inclination, and companion mass. The diagnostic element is the eccentricity posterior: formation by core accretion should leave e near zero, while a uniform prior on e in [0,1] provides a benchmark with median 0.5. Photometric and low-resolution spectroscopic extraction supplies the spectral classifications.

What would settle it

For one of the four first-orbit systems, compare the eccentricity posterior against the uniform prior: if the posterior is indistinguishable from the prior, or if a decade of additional astrometry shifts e toward zero, the claim that wide-orbit companions are systematically eccentric would not survive.

Watch

Extended reading notes

Core claim

The central claim, stated on the paper's own terms, is that the updated orbital fits for 13 wide-orbit substellar companions are consistent with non-circular orbits in all cases. The sample includes the first orbital solutions for CT Cha b, HIP 78530 B, HIP 64892 B, and RX J1609.5-2105 b, and tighter constraints for the rest. Companion masses range roughly 7-70 Jupiter masses and semimajor axes 25-500 au, and spectral types derived from color-magnitude diagrams and low-resolution YJ spectra span mid-M to mid-L. The authors argue that near-zero eccentricity is the signature of core accretion, so the retrieved eccentricities (0.21-0.82) potentially disfavor that pathway and instead point to mo

Load-bearing premise

The argument that all thirteen orbits are non-circular rests on eccentricity posteriors that, for the seven systems with less than one percent of the orbit observed, are assumed to be driven by the astrometry rather than by the adopted uniform prior.

Editorial extensions

If this is right

The four first solutions (CT Cha b, HIP 78530 B, HIP 64892 B, RX J1609.5-2105 b) give quantitative orbital elements where none existed, so future epochs can directly test and refine them.
If the eccentricities are real, core-accretion formation in the circumstellar disk becomes unlikely for this population; gravitational fragmentation or disk instability becomes the more probable route, consistent with the wide separations.
The refined classifications—GQ Lup B M8-M8.5, PZ Tel B M5-M6.5, HD 984 B M7.75-M8.5—change the inferred luminosities and, through evolutionary models, the companion masses and temperatures used in later atmospheric studies.
The 5-sigma detection limits rule out additional 1-15 Jupiter-mass companions out to roughly 300 au in these systems, so any scattering origin for the eccentric orbits must involve either unseen lower-mass companions, satellites, or objects interior to the coronagraph.
Most of the dynamical masses are still unconstrained; only PZ Tel B and HD 984 B have enough orbital coverage for reliable masses, meaning the formation argument rests on eccentricities rather than on measured masses.

Reading between the lines

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

The paper's own note that the eta Tel posteriors 'remain largely prior-driven' suggests the same may hold for the seven systems with less than 1% orbital coverage; a uniform eccentricity prior peaks at 0.5, so the reported medians near 0.5-0.6 could partly reflect the prior rather than the astrometry.
A sharper comparison would be eccentricity versus system age: the youngest targets (<10 Myr) should retain the birth eccentricity from formation, while older systems have had time for scattering or circularization; the present sample is too small and too heterogeneous to separate these effects.
If GQ Lup B is truly M8-M8.5 rather than the L6 classification, its bolometric luminosity and evolutionary mass likely drop, which would affect claims about its circumplanetary disk and whether it straddles the deuterium-burning limit.
The null detection of additional wide companions suggests that if planet-planet scattering produced these orbits, the scattering partner has since been ejected or now orbits at sub-arcsecond separations; a targeted search for close-in companions in these systems would test that scenario.

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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

Let me get to the point. The paper gives the field something real: new SPHERE H2H3 epochs for 13 directly imaged companions, first orbit solutions for four of them, and updated spectra for three. The astrometric baseline extension is a solid contribution that will be used in future studies. The reduction appears careful, and the comparison with past works is genuine and even-handed.

But the headline claim doesn't survive contact with the data. The abstract and conclusions say all companions have non-circular orbits, with e ranging ~0.21–0.82, and use that to disfavor core accretion. Section 6.2 says 'nearly all' — already a retreat. For the six or seven systems with <1% orbital coverage, the eccentricity posterior is mostly the uniform prior: the medians cluster near 0.5, and the intervals are wide. The paper admits for eta Tel that the posteriors are largely prior-driven; nothing in the paper shows the other short-arc targets behave differently. No prior-sensitivity or injection-recovery tests are presented. So the strong formation claim rests on exactly the systems where eccentricity is least constrained. That is a load-bearing weakness, not a minor quibble.

There is also mild circularity in the mass treatment. The total-mass priors in orbitize! are built from photometric companion masses derived in this same paper (H2 + ATMO/AMES-Dusty), and the resulting 'dynamical masses' are then quoted and compared with the literature. For most systems the dynamical masses are unconstrained, and the paper says so. But the phrasing still risks presenting the photometric masses as independent dynamical checks.

The exclusions of the DH Tau and HIP 78530 epochs are defensible in isolation, but they are post-hoc, and the stated reason for dropping the HIP 78530 point — that it inflated posterior uncertainties — is backwards: large uncertainties are usually a reason to include a point, not exclude it.

Who benefits from this paper? Anyone working on the orbits of wide substellar companions. The table of astrometric epochs itself is a resource. The paper deserves a serious referee. My recommendation: send it to review, but tell the authors to add prior-sensitivity tests (or at least run the same fits with a Beta prior on e), to harmonize the 'all' vs 'nearly all' language, and to either justify the epoch exclusions quantitatively or keep the points in and show the fits are stable.

Referee Report

4 major / 5 minor

Summary. This paper presents new VLT/SPHERE IRDIS H2H3 photometry and astrometry for 13 directly imaged substellar companions, IFS YJ spectra for three of them, updated orbitize! orbital fits combining the new epochs with literature astrometry and, where available, RVs and Hipparcos-Gaia accelerations, and the first orbital solutions for CT Cha b, HIP 78530 B, HIP 64892 B, and RX J1609.5-2105 b. The authors derive spectral types from color-magnitude diagrams and template matching, and use the orbital fits to argue that all companions have non-circular orbits (e ~ 0.21-0.82), which they interpret as disfavoring core-accretion formation in favor of cloud/disk fragmentation or dynamical scattering.

Significance. The observational data products are valuable: the new SPHERE epochs extend orbital baselines for 13 systems, four of which previously had no published orbit, and the IFS spectra provide useful spectral-type constraints. The paper also compiles homogeneous astrometric and photometric tables. However, the central scientific claim — that the eccentricities are well enough determined to discriminate formation pathways — is not supported for the seven systems with less than 1% orbital coverage, whose eccentricity posteriors are largely prior-dominated (as the paper itself admits for eta Tel in Sec. 6.1). If the claim were robust, it would be an important contribution to the formation of wide-orbit substellar companions, but in its current form the inference overreaches the data. The paper's main value is thus the data compilation and the improved orbits for the better-covered systems, not the population-level formation conclusion.

major comments (4)

[Abstract and Sec. 6.2] The claim that all 13 companions have non-circular orbits is not supported for the seven systems with <1% orbital coverage (Table B.1): AB Pic, TYC 8047-232-1, CT Cha, HIP 78530, DH Tau, HIP 64892, RX J1609.5-2105. Their eccentricity posteriors (e.g., AB Pic 0.54+0.32-0.28, CT Cha 0.60+0.29-0.38, DH Tau 0.58+0.32-0.26) are consistent with the uniform e∈[0,1] prior median of 0.5 and do not exclude e=0 at high significance. The paper itself states for eta Tel (Sec. 6.1) that 'the posteriors remain largely prior-driven.' A prior-sensitivity test (e.g., a beta prior or a fixed-e=0 model comparison) is required before any formation inference; without it, the abstract's 'consistent with non-circular orbits in all cases' is a prior artifact.
[Sec. 4 and Sec. 6.1] There is a circularity in the mass treatment: the Gaussian Mtot priors in the orbit fits are constructed from the paper's own photometric companion masses (Table 2, derived from H2 photometry and ATMO/AMES-Dusty models in Sec. 3). Later, the same fits are used to quote 'dynamical masses' that are compared with evolutionary masses as if they were independent confirmations (e.g., Sec. 6.1 discussions of AB Pic, CT Cha, HIP 78530). For short-arc systems the companion mass posterior is essentially the prior, so these 'dynamical masses' are not independent. The authors should either use literature-only stellar masses and a wide companion-mass prior, or explicitly label Table B.1 masses as prior-informed, and avoid presenting them as independent dynamical constraints.
[Sec. 5.2.6 and Sec. 5.2.7] The post-hoc exclusion of published astrometric epochs is not rigorously justified. For HIP 78530, the Bailey et al. (2013) 2011 epoch is excluded because its large uncertainties 'inflated uncertainties in the posterior' — this is not a valid reason for exclusion, since large uncertainties are naturally downweighted by the likelihood. For DH Tau, two Bryan et al. (2016) epochs are excluded as >15σ outliers based partly on a comparison with one SPHERE epoch; the reasoning is plausible but the paper does not demonstrate that the orbital results are robust to their inclusion. The authors should show fits with and without these epochs, or employ a robust outlier model; otherwise the eccentricity posteriors for these two systems are conditional on the exclusions.
[Sec. 6.3 and Sec. 7] The formation conclusion is overstated. Even if the eccentricities were well measured, the paper itself notes (Sec. 6.3) that dynamical scattering can produce e up to ~0.8 and that several systems are young enough that gas-disk dissipation may not have completed. The phrase 'disfavoring core-accretion formation within their circumstellar disks' is too strong for data that are merely 'consistent with non-circular orbits'; the posterior probability of e=0 is not quantified. The conclusion should be restricted to the few systems with >3% orbital coverage (GQ Lup, PZ Tel, HD 984) where the eccentricity is actually constrained, and the rest should be described as unconstrained rather than as evidence against core accretion.

minor comments (5)

[Sec. 6] The text says 'only four show an orbital coverage greater than 3% (Table B.1)', but Table B.1 lists only three systems with coverage >3%: GQ Lup B (4.0%), PZ Tel B (12.9%), HD 984 B (12.6%). Please check and correct.
[Sec. 5.2.13] In the eta Tel paragraph, the sentence fragment '(Desidera et al. 2021).' appears before 'It is a member of the β Pictoris moving group...' This looks like a leftover reference and should be removed or integrated.
[Table B.1] The table mixes quantities: some rows report Mtot (e.g., AB Pic, TYC 8047-232-1, CT Cha, DH Tau, RX J1609, HII 1348) and others report Mstar and Mcomp separately (HIP 78530, HIP 64892, PZ Tel, HD 984, eta Tel). The header and caption should clarify which parameters were directly fitted and which are derived, and should flag that Mcomp values for short-arc systems are prior-dominated.
[Throughout] Typos and reference formatting: 'distint' (Secs. 5.2.5, 5.2.11), 'Tetzlaffet al.' (Refs), 'Proocedings' (Refs), 'V ousden' (Refs), inconsistent 'Lafrèniere' vs 'Lafrenière'. Please proofread.
[Sec. 2] The paper states 'eight targets were previously observed within the SHINE GTO program' but then describes the sample as 13 targets; the relationship between the SHINE subsample and the full sample could be stated more clearly for readers not familiar with Paper I.

Circularity Check

2 steps flagged · score 6.0 of 10

The 'non-circular in all cases' result is built into the uniform e∈[0,1] prior for the seven <1%-coverage systems, and several reported 'dynamical masses' are echoes of photometric-mass priors.

self definitional [Table 4; Sec. 6.1 (eta Tel); Sec. 6.3]
"Eccentricity (e) Uniform on [0, 1] ... the posteriors remain largely prior-driven ... Even when accounting for the uncertainties, all our retrieved eccentricities are consistent with non-circular orbits for nearly all substellar companions in our sample."

The prior places zero probability on exactly circular orbits (e=0 is a measure-zero point under a continuous uniform distribution on [0,1]). For the seven targets with less than 1% of the orbit sampled (Sec. 6), the astrometry provides only a short arc, and the paper itself concedes for eta Tel that the posterior is 'largely prior-driven'. The eccentricity posteriors for such systems therefore inherit the prior's exclusion of e=0; concluding that they are 'consistent with non-circular orbits' is a restatement of the prior's support, not a measurement. The subsequent inference that core accretion is 'potentially disfavored' for these systems is thus premised on the prior rather than on the data.
fitted input called prediction [Sec. 5.2.4 (CT Cha); Sec. 7]
"We performed an orbital fit adopting a prior on the total system mass of 0.81±0.05 M⊙, based on a companion mass of 9.7+1.2−1.1 MJup, and a stellar mass of 0.80±0.05 M⊙ ... We derived a total dynamical mass of 0.807+0.050−0.051 M⊙ ... With the exception of PZ Tel B and HD 984 B ... the dynamical masses of all other companions remain essentially unconstrained."

The Gaussian prior on total system mass is constructed directly from the photometric companion mass (H2 photometry plus ATMO/AMES-Dusty evolutionary models) added to the stellar mass. The 'derived total dynamical mass' posterior for CT Cha (0.807 M⊙) is essentially identical to the input prior (0.81 M⊙), and similar near-prior values appear for other short-arc systems (e.g., DH Tau, where the prior is 0.422 M⊙ and the derived mass is 0.418 M⊙). Labeling these as 'dynamical' masses and comparing them with literature evolutionary masses in Sec. 6.1 presents a photometric prior as an independently derived result, even though Sec. 7 concedes that these masses are essentially unconstrained by the orbital data.

full rationale

The paper's headline result, that all companions have non-circular orbits and that this 'potentially disfavors' core accretion, is substantially prior-driven for the seven systems with <1% orbital coverage. Because the adopted eccentricity prior is uniform on [0,1], it has zero prior mass at exactly e=0, so the statement 'consistent with non-circular orbits' is guaranteed by the prior for any system with weak astrometric constraints. The paper explicitly acknowledges this for eta Tel and notes that most dynamical masses are unconstrained, yet the abstract and Sec. 6.3 still elevate the prior-induced eccentricities to a formation-scenario conclusion. A second, lesser circularity is the use of photometric companion masses to build the Mtot prior and the subsequent presentation of near-prior posterior values as 'derived dynamical masses.' The paper is honest in Sec. 7 about the lack of mass constraints, which limits the severity, and the well-covered systems (PZ Tel B, HD 984 B, HII 1348 B, GQ Lup B) provide independent eccentricity information. Overall, the central claim is partially circular rather than fully so, warranting a score of 6.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central claims rest on standard priors and literature inputs rather than new physics. The most consequential choices are the photometric mass priors (which feed the total-mass priors) and the exclusion of published astrometric epochs for DH Tau and HIP 78530. The paper postulates no new particles, forces, or entities.

free parameters (3)

PZ Tel RV uncertainty inflation factor = 10
Multiplies HARPS RV errors by 10 to account for stellar variability; hand-chosen and directly changes the RV weight in the PZ Tel orbital fit (Sec. 5.2.11).
Photometric companion masses used as M_tot priors = 9.7-75 M_Jup across systems
Derived from H2 photometry + ATMO/AMES-Dusty models; used as Gaussian priors on total mass in the orbit fits (Table 2, Sec. 4). For eta Tel the dynamical-mass posterior is admitted to be prior-driven.
Excluded astrometric epochs = DH Tau 2014.934/2015.844 (Bryan+16); HIP 78530 2011.397 (Bailey+13)
Hand-chosen data exclusions; the DH Tau exclusion is justified by >15 sigma deviation and NIRC2 systematics, but the choice affects the fitted eccentricity.

assumptions (5)

standard math Each companion follows a Keplerian two-body orbit around its host star.
Invoked in Sec. 4 where orbitize! fits Keplerian orbits to relative astrometry and RVs.
domain assumption Adopted stellar masses and system ages from the literature are accurate to the stated uncertainties.
Table 2 lists stellar masses, ages, and parallaxes from literature; these are used as Gaussian priors and drive the fits for poorly covered systems.
domain assumption SpeX Prism field-dwarf templates are valid spectral comparators for young, low-gravity substellar companions.
Used in Sec. 5.1 to classify GQ Lup B, PZ Tel B, and HD 984 B; young dusty atmospheres can differ significantly (the GQ Lup B vs L6 discrepancy shows this).
ad hoc to paper The excluded astrometric epochs (Bryan et al. 2016 for DH Tau; Bailey et al. 2013 for HIP 78530) are true outliers.
Sec. 5.2.6-5.2.7 exclude these points as outliers; the DH Tau exclusion is based on >15 sigma deviations and NIRC2 systematics, but the conclusion that the SPHERE epoch is correct rather than the NIRC2 points is a judgment call.
ad hoc to paper orbitize! priors do not dominate the eccentricity posteriors for short-arc systems.
Section 6 notes 7 targets have <1% orbital coverage; for eta Tel it is admitted that 'the posteriors remain largely prior-driven,' which undermines this assumption for the least-covered systems.

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Cite this review

Pith. "Pith review of SaNDi-SHoP: Searching for Satellites'N'Disks with a Star-Hopping Program II. Spectrophotometric analysis and orbital monitoring of directly imaged companions." pith.science (2026). https://pith.science/paper/5KR372C2

@misc{pith2026260713545,
  author       = {Pith},
  title        = {Pith review of: SaNDi-SHoP: Searching for Satellites'N'Disks with a Star-Hopping Program II. Spectrophotometric analysis and orbital monitoring of directly imaged companions},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5KR372C2}},
  note         = {Machine review of arXiv:2607.13545}
}

read the original abstract

Over the past decade, advances in high-contrast imaging instrumentation, coupled with extreme adaptive optics systems, have enabled the discovery of tens of planets and brown dwarfs orbiting at wide separations from their host stars (a larger than 10 au). The existence of companions at these separations challenges current planet-formation paradigms, highlighting the importance of high-contrast imaging as the only technique capable of directly probing this region of planetary systems. In this paper, we present a survey of thirteen planets and brown dwarfs observed with VLT/SPHERE between June 2023 and July 2025. These data provide updated photometry in the 1.0-1.7 micron range and new high-precision astrometry, enabling tighter constraints on their orbital properties. We used the IRDIS subsystem to acquire dual-band H2H3 images (H2 = 1.593 microns, H3 = 1.667 microns) for all companions in our sample. For the three objects located within the IFS field of view (GQ Lup B, PZ Tel B, and HD 984 B), we additionally obtained low-resolution (R ~ 50) near-infrared (0.96-1.34 micron) spectra. We combined our new astrometric measurements with those available in the literature to derive updated orbital solutions. The orbital fitting was performed using the orbitize! Python package. For CT Cha b, HIP 78530 B, HIP 64892 B, and RX J1609.5-2105 b, this work provides the first orbital solutions to date. We derived new photometry for all objects, which, when compared with field dwarfs in color-magnitude diagrams, indicates spectral types ranging from mid-M to mid-L. For the companions observed with IFS, their spectra are best matched by those of M6-M8.5 field dwarfs. Our updated orbital fits provide tighter constraints for nearly all companions and are consistent with non-circular orbits in all cases, potentially disfavoring core-accretion formation within their circumstellar disks.

Figures

Figures reproduced from arXiv: 2607.13545 by the authors.

**Figure 1.** Left: H2-H3 color magnitude diagram for the objects in our sample. Right: Y-J color magnitude diagram for the objects in our sample with IFS observations. ATMO-CEQ, AMES-Cond, and AMES-Dusty evolutionary tracks models at an age of 20 Myr (solid lines) and 100 Myr (dashed lines) are overplotted. In both figures mid-M to late T-type objects from the SpeX Prism Libraries are shown for reference. The color bars above th… view at source ↗

**Figure 2.** Spectrum of GQ Lup B as extracted from IFS and IRDIS observations. A comparison with an M8.5 V field dwarf and an L6 [PITH_FULL_IMAGE:figures/full_fig_p010_2.png] view at source ↗

**Figure 3.** Spectrum of PZ Tel B as extracted from IFS and IRDIS observations. A comparison with an M6 V field dwarf is overplotted, [PITH_FULL_IMAGE:figures/full_fig_p010_3.png] view at source ↗

Figures from the paper (4 more)

**Figure 4.** Figure 4: Spectrum of HD 984 B as extracted from IFS and IRDIS observations. The GPI [PITH_FULL_IMAGE:figures/full_fig_p011_4.png]

**Figure 5.** Figure 5: Corner plot for PZ Tel B. Upper right: orbital fit for PZ Tel B. [PITH_FULL_IMAGE:figures/full_fig_p011_5.png]

**Figure 6.** Figure 6: Top left: eccentricity distribution as a function of the companion mass. Top right: eccentricity distribution as a function of [PITH_FULL_IMAGE:figures/full_fig_p012_6.png]

**Figure 7.** Figure 7: Left: 5σ contrast curves in separation versus contrast relative to the host star. Right: corresponding detection limits converted into mass using ATMO evolutionary models. ets within the same system, leading to planet–planet scattering events (e.g., Weidenschilling & M…

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