REVIEW 2 major objections 4 minor 175 references
The Longest-period Young Transiting Exoplanets. A Duo of Puffy Giants inside a Debris Disk
T0 review · 2 major / 4 minor · reviewed 2026-07-12 · grok-4.5
Pith's one-line read Two puffy giant planets on 226- and ~314-day orbits are the longest-period young transiting exoplanets known, and they shape their star's debris disk.
desk verdict Solid multi-facility recovery of a long-period young giant (b) and a credible second planet (c), with the TTV mass cut for c being the only soft spot. 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
A global Gaussian-process joint model of multi-facility light curves and radial velocities, combined with N-body transit-timing variation filtering, that simultaneously recovers the two planetary signals, upper mass limits, and the period ratio.
What would settle it
One additional full transit of the deeper signal that yields a mid-transit time incompatible with any period near 314 days, or a radial-velocity detection that forces either planet above the stated 95-percent mass upper limits.
Extended reading notes
Core claim
HD 114082 b and c are the longest-period young transiting exoplanets known: planet b has Pb = 225.5504 ± 0.0004 days, Rb = 1.046 ± 0.014 RJ and M95% < 1.6 MJ; planet c has Pc ≈ 314 days, Rc = 1.36 ± 0.03 RJ and M95% < 2.0 MJ (0.24 MJ with TTV filtering). Both occupy nearly circular, coplanar orbits near the 3:2 or 7:5 resonance and dynamically shape the host's two-component debris disk.
Load-bearing premise
That the single deeper monotransit seen by TESS and NGTS is a second planet on a roughly 314-day orbit whose mass can be tightly bounded by radial-velocity non-detections and N-body filtering of only four partial or full transits of planet b.
Editorial extensions
If this is right
- Young giant planets can remain large and low-density for at least 15 million years even at orbital periods of several hundred days.
- Near-resonant, coplanar pairs of moderate-mass giants can carve and incline an inner planetesimal belt while leaving an outer Kuiper-belt analogue largely undisturbed.
- Transit-timing variations of a few hours already limit the outer planet to well below a Jupiter mass once the circular solution is adopted.
- Further transit detections of planet c will decide whether the pair is locked in the 3:2 or 7:5 resonance and will yield dynamical masses.
Reading between the lines
- If the TTV-filtered mass of planet c is confirmed near 0.24 MJ, the system becomes a rare example of two young super-puffs rather than classical gas giants.
- The ~7-degree misalignment between the planetary plane and the outer belt may record an early scattering or migration episode that is still frozen into the disk architecture.
- Continued monitoring of the same star with the same facilities will turn the current upper mass limits into actual masses within a few years, testing core-accretion contraction timescales directly.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The manuscript reports two long-period, large-radius planets around the young F star HD 114082. Multi-facility photometry (TESS, NGTS, CHEOPS, ASTEP+, LCO) establishes four transits of planet b and pins Pb = 225.5504 ± 0.0004 d after alias rejection; a deeper monotransit (TESS + partial NGTS) is identified as planet c with Pc ≈ 314 d (1σ uncertainty still ~6 %). Joint GP + transit + RV modeling yields radii Rb = 1.046 ± 0.014 RJ, Rc = 1.36 ± 0.03 RJ, near-zero eccentricities, nearly coplanar orbits, and 95 % mass upper limits M95%,b < 1.6 MJ, M95%,c < 2.0 MJ (tightened to 0.24 MJ after N-body TTV filtering). A two-component dust model is fit to the debris-disk SED. The authors interpret the planets as moderate-to-low-mass puffy giants on near-resonant orbits that formed in situ or beyond the snowline and migrated inward, shaping the disk.
Significance. If the two-planet interpretation holds, HD 114082 b and c become the longest-period young transiting exoplanets known, providing rare empirical anchors for giant-planet contraction, migration, and disk sculpting at ~15 Ma. The multi-facility campaign that locks Pb and rejects the half-period alias is a clear observational strength, as is the careful re-reduction of FEROS/HARPS RVs and the transparent joint modeling. The debris-disk reanalysis and architectural sketch add useful context. The result is therefore of genuine interest to the young-planet and debris-disk communities, even while the mass and period of planet c remain only loosely constrained.
major comments (2)
- [Appendix C, Table 2] Appendix C and Table 2: the reduction of M95%,c from 2.0 MJ to 0.24 MJ rests on an after-the-fact REBOUND filter that discards posterior draws producing TTV semi-amplitudes on b larger than an ad-hoc 10 h threshold. Only four mid-transit times of b exist (two full, two ~50 % coverage), the observed TTV amplitude is quoted as ≲ 4 ± 2 h, and the filter is not applied jointly with the photometric/RV likelihood. Because Pc itself is still uncertain at the ~6 % level, the dynamical mass cut is sensitive both to the Pc prior and to the arbitrary cutoff. The abstract and conclusions should present the RV-only upper limit as the primary mass constraint and clearly label the TTV-filtered value as model-dependent and provisional.
- [§4.1–4.2, Appendix D] Section 4.1–4.2 and Appendix D: planet c is still a monotransit (plus partial NGTS coverage). While the false-positive analysis with TRICERATOPS, the RUWE, and the dynamical arguments are supportive, the period remains only loosely constrained by transit shape + non-detections (Pc = 314+11−18 d for the circular model). Claims that the planets are “nearly resonant” (7:5 or 3:2) and that they are definitively “the longest-period young transiting exoplanets” should be tempered until a second transit of c is secured or the period posterior is substantially narrowed.
minor comments (4)
- [Figure 1, Appendix C] Figure 1 and the accompanying text: the partial ASTEP+ and NGTS light curves of planet b are valuable, but the mid-transit times derived from ~50 % coverage should be shown with their full uncertainty (including the fixed-duration assumption) so that the quoted TTV amplitude of ≲ 4 ± 2 h can be assessed directly.
- [Table 6] Table 6: the Bayesian evidence values (ln Z) favor the circular model by only ~5 units; a short statement on whether this difference is decisive given the GP flexibility and sparse RV sampling would help the reader.
- [§4.3, Appendix E] Section 4.3 / Appendix E: the warm-belt radius is only weakly constrained (1.3+3.8−1.1 au). The architectural sketch in Figure 3 is useful, but the text should emphasize that the inner-belt location is still highly uncertain and that any claimed dynamical interaction with the planets is therefore tentative.
- [Throughout] A few typographical and formatting issues remain (e.g., inconsistent spacing around ±, occasional missing spaces after periods, and the draft header “DRAFT VERSION JULY 7, 2026”). These are easily cleaned in revision.
Circularity Check
Mild self-consistency only in post-hoc N-body filtering of the joint posterior to tighten mass upper limits; periods, radii and primary RV bounds are independent of that step.
-
other
[Appendix C (TTVs), final paragraph; also Abstract and Table 2 parenthetical]
"After feeding REBOUND with approximately 1 million representations that settle the full posterior distributions of the parameters for the preferred circular solution shown in Table 2 and 6, those producing TTVs greater than the conservative value of 10 hr are filtered out. As a result, M95% for planets b and c decrease from 1.6 and 2.0 MJ to 1.5 and 0.24 MJ, respectively, yielding a TTV semiamplitude on planet b of about 7 hr (95% confidence limit)."
The joint photometric+RV posterior (already conditioned on the four mid-transit times of b) is re-sampled and filtered by an N-body TTV amplitude cut derived from those same times. The tighter mass bound is therefore a self-consistency refinement of the fitted posterior rather than an independent dynamical constraint; the paper itself notes that TTVs were not included jointly 'given the small statistics'.
full rationale
The derivation of Pb from four observed mid-transit times (TESS, NGTS, CHEOPS, ASTEP+), of Rb and Rc from transit depths after dilution correction, and of the primary M95% bounds from the joint photometric+RV GP model is self-contained against the new multi-facility data and re-reduced FEROS/HARPS RVs. Stellar parameters come from external PARSEC models + Gaia photometry/astrometry; the two-component disk SED fit uses literature photometry plus ALMA outer-belt geometry. The sole mild circularity is the optional TTV mass refinement in Appendix C: ~10^6 draws from the already-fitted circular posterior are discarded if they produce TTV semi-amplitudes >10 h on b, lowering M95%,c from 2.0 to 0.24 MJ. This is a post-hoc consistency filter on the same transit-timing data already used for T0 and P, not a joint dynamical model, and is presented only parenthetically. No equation equates a claimed period, radius or first-principles prediction to its own fitted inputs by construction, and no load-bearing uniqueness theorem or ansatz is imported via self-citation. Score 2 reflects that single non-central self-consistency step.
Assumptions & free parameters
free parameters (6)
- Pb, T0b, Rb/R⋆, b_b (and derived ib, ab)
- Pc, T0c, Rc/R⋆, b_c (and derived ic, ac)
- M95%,b and M95%,c (RV semi-amplitudes)
- GP hyperparameters (SHO kernels per instrument)
- Warm-belt radius, smin, q, dust masses
- Stellar mass, radius, age priors
assumptions (5)
- domain assumption Quadratic limb-darkening law and Mandel–Agol transit model are adequate for the observed light curves.
- domain assumption Eccentricities consistent with zero are preferred; circular model has higher Bayesian evidence.
- ad hoc to paper TTV semi-amplitude ≲ 10 h filters the joint posterior to tighten mass upper limits.
- domain assumption Debris-disk excess is two Gaussian belts of astronomical silicate with a single power-law size distribution.
- domain assumption No stellar companions or background eclipsing binaries produce the observed dips (TRICERATOPS + RUWE + SPHERE).
invented entities (1)
-
Planet c (TOI-6697.02)
independent evidence
Cite this review
Pith. "Pith review of The Longest-period Young Transiting Exoplanets. A Duo of Puffy Giants inside a Debris Disk." pith.science (2026). https://pith.science/paper/N3FTM3VT
@misc{pith2026260702685,
author = {Pith},
title = {Pith review of: The Longest-period Young Transiting Exoplanets. A Duo of Puffy Giants inside a Debris Disk},
year = {2026},
howpublished = {\url{https://pith.science/paper/N3FTM3VT}},
note = {Machine review of arXiv:2607.02685}
}
abstract
We identify two large-radius planets around the F-type star HD 114082 as the longest-period young transiting exoplanets known. From the first transit, detected by NASA's Transiting Exoplanet Survey Satellite (TESS), and a second dip, spotted by the Next-Generation Transit Survey (NGTS), we predicted mid-transit times for HD 114082 b (planet b). We pinpoint its orbit (period Pb= 225.5504$\pm$0.0004 days) from a third transit captured with the ESA's CHaracterising ExOplanet Satellite and the upgraded Antarctic Search for Transiting ExoPlanets telescope (ASTEP+), alongside orbit-discriminating observations. Another dimming partly covered by ASTEP+ completes the four-transit series. We support with dynamical evidence the planetary nature of a deeper transit detected with TESS and NGTS, identifying planet c. Additionally, we reexamine the debris disk, fitting its excess emission with two dust components. Fundamental stellar parameters are inferred from stellar evolution models, while a joint modeling of photometric and radial-velocity time series yields the planetary parameters, with masses further constrained using an N-body code. For planet b, the semimajor axis a$_b$= 0.791$\pm$0.008 au, eccentricity eb$\approx$ 0, inclination ib= 89.791$\pm$0.014 degrees, radius Rb= 1.046$\pm$0.014 R$_J$, and 95 % confidence upper limit on its mass M$_{95\%,b}$= 1.6 M$_J$. For planet c, a$_c$= 0.99$^{+0.03}_{-0.04}$ au, ec$\approx$ 0, i$_c$= 89.701$\pm$0.011 degrees, R$_c$= 1.36$\pm$0.03 R$_J$, and M$_{95\%,c}$= 2.0 M$_J$ (0.24 M$_J$ if adding transit timing variation constrains). They seem to be moderate-to-low-mass giants in nearly resonant, coplanar, circular orbits that formed in situ, or beyond the snowline, and migrated inwards, shaping the disk.
Figures
Figures from the paper (3 more)
Reference graph
Works this paper leans on
-
[1]
HARPS reduced data obtained by standard ESO pipeline processing , publisher =. 2014 , copyright =. doi:10.18727/ARCHIVE/33 , url =
-
[3]
Composite Planet Data Table , publisher =. doi:10.26133/NEA2 , url =
-
[4]
The NASA Exoplanet Archive and Exoplanet Follow-up Observing Program: Data, Tools, and Usage. , keywords =. doi:10.3847/PSJ/ade3c2 , archivePrefix =. 2506.03299 , primaryClass =
-
[5]
TESS Light Curves - Sectors. 2021, 2026 , publisher =. doi:10.17909/t9-nmc8-f686 , url =
-
[6]
Separating Super-Puffs vs. Hot Jupiters Among Young Puffy Planets
Separating Super-puffs versus Hot Jupiters among Young Puffy Planets. , keywords =. doi:10.3847/1538-4357/ad946c , archivePrefix =. 2408.16793 , primaryClass =
-
[7]
Understanding the Origins of Super-Puff Planets: A New Mass-Loss Regime Coupled to Planetary Evolution. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.02201 , archivePrefix =. 2510.02201 , primaryClass =
-
[8]
, year = 1969, month = may, volume =
Collisional Model of Asteroids and Their Debris. , year = 1969, month = may, volume =. doi:10.1029/JB074i010p02531 , adsurl =
-
[9]
Software and Cyberinfrastructure for Astronomy V , year = 2018, editor =
Real-time processing of the imaging data from the network of Las Cumbres Observatory Telescopes using BANZAI. Software and Cyberinfrastructure for Astronomy V , year = 2018, editor =. doi:10.1117/12.2314340 , archivePrefix =. 1811.04163 , primaryClass =
Show all 175 references
-
[10]
, keywords =
A survey of the motions of asteroids in the commensurabilities with Jupiter. , keywords =
- [11]
- [12]
-
[13]
Ground-based and Airborne Telescopes III , year = 2010, editor =
ASTEP 400: a telescope designed for exoplanet transit detection from Dome C, Antarctica. Ground-based and Airborne Telescopes III , year = 2010, editor =. doi:10.1117/12.854946 , adsurl =
2010 doi
-
[14]
Observatory Operations: Strategies, Processes, and Systems IX , year = 2022, editor =
Observation scheduling and automatic data reduction for the Antarctic Telescope, ASTEP+. Observatory Operations: Strategies, Processes, and Systems IX , year = 2022, editor =. doi:10.1117/12.2629920 , archivePrefix =. 2208.04501 , primaryClass =
-
[15]
Motivation, sample, data reduction, and results overview
The ALMA survey to Resolve exoKuiper belt Substructures (ARKS): I. Motivation, sample, data reduction, and results overview. , keywords =. doi:10.1051/0004-6361/202556489 , archivePrefix =. 2601.11708 , primaryClass =
- [16]
- [17]
- [18]
-
[19]
Astronomische Nachrichten , keywords =
A new algorithm for differential photometry: computing an optimum artificial comparison star. Astronomische Nachrichten , keywords =. doi:10.1002/asna.200410350 , adsurl =
- [20]
- [21]
- [22]
- [23]
- [24]
- [25]
- [26]
- [27]
- [28]
- [29]
-
[30]
, year = 1993, month = jan, volume =
Habitable Zones around Main Sequence Stars. , year = 1993, month = jan, volume =. doi:10.1006/icar.1993.1010 , adsurl =
1993 doi
- [31]
- [32]
- [33]
- [34]
- [35]
-
[36]
EPSC-DPS Joint Meeting 2025 (EPSC-DPS2025 , year = 2025, month = sep, eid =
Tidal Effects on Planetary Migration in Systems Hosting a Hot Jupiter and an Inner Companion. EPSC-DPS Joint Meeting 2025 (EPSC-DPS2025 , year = 2025, month = sep, eid =. doi:10.5194/epsc-dps2025-1120 , adsurl =
2025 doi
- [37]
- [38]
-
[39]
Handbook of Exoplanets , year = 2025, eid =
Dynamical Evolution of Planetary Systems. Handbook of Exoplanets , year = 2025, eid =. doi:10.1007/978-3-319-55333-7_145 , adsurl =
2025 doi
- [40]
-
[41]
Studies of Stellar Rotation. V. The Dependence of Rotation on Age among Solar-Type Stars. , year = 1967, month = nov, volume =. doi:10.1086/149359 , adsurl =
1967 doi
- [42]
- [43]
-
[44]
, keywords =
The Tycho-2 catalogue of the 2.5 million brightest stars. , keywords =
- [45]
- [46]
- [47]
- [48]
-
[49]
, keywords =
Correcting systematic effects in a large set of photometric light curves. , keywords =. doi:10.1111/j.1365-2966.2004.08585.x , archivePrefix =. astro-ph/0502056 , primaryClass =
2004 doi
- [50]
- [51]
- [52]
- [53]
- [54]
- [55]
-
[56]
doi:10.1117/12.2233418 , adsurl =
Software and Cyberinfrastructure for Astronomy IV , year = 2016, editor =. doi:10.1117/12.2233418 , adsurl =
2016 doi
- [57]
- [58]
-
[59]
doi:10.1086/674989 , adsurl =
, year = 2014, month = jan, volume = 126, pages =. doi:10.1086/674989 , adsurl =
2014 doi
-
[60]
doi:10.1080/713820996 , adsurl =
Optica Acta , year = 1955, month = apr, volume =. doi:10.1080/713820996 , adsurl =
1955 doi
-
[61]
Optical and IR Telescope Instrumentation and Detectors , year = 2000, editor =
HARPS: a new high-resolution spectrograph for the search of extrasolar planets. Optical and IR Telescope Instrumentation and Detectors , year = 2000, editor =. doi:10.1117/12.395516 , adsurl =
-
[62]
Rasmussen and C.K.I
Gaussian Processes for Machine Learning, by C.E. Rasmussen and C.K.I. Williams. ISBN-13 978-0-262-18253-9 , year = 2006, adsurl =
2006
- [63]
- [64]
- [65]
-
[66]
doi:10.1063/1.1835238 , adsurl =
Bayesian Inference and Maximum Entropy Methods in Science and Engineering: 24th International Workshop on Bayesian Inference and Maximum Entropy Methods in Science and Engineering , year = 2004, editor =. doi:10.1063/1.1835238 , adsurl =
2004 doi
-
[67]
Bayesian Analysis , number =
John Skilling , title =. Bayesian Analysis , number =. 2006 , doi =
2006
- [68]
-
[69]
doi:10.5281/zenodo.7832419 , version =
joshspeagle/dynesty: v2.1.1. doi:10.5281/zenodo.7832419 , version =
- [70]
-
[71]
The Messenger , keywords =
Commissioning FEROS, the new high-resolution spectrograph at La-Silla. The Messenger , keywords =
-
[72]
The Messenger , year = 2003, month = dec, volume =
Setting New Standards with HARPS. The Messenger , year = 2003, month = dec, volume =
2003
- [73]
-
[74]
The Spitzer Infrared Spectrograph Debris Disk Catalog. I. Continuum Analysis of Unresolved Targets. , keywords =. doi:10.1088/0067-0049/211/2/25 , adsurl =
-
[75]
The Spitzer Infrared Spectrograph Debris Disk Catalog. II. Silicate Feature Analysis of Unresolved Targets. , keywords =. doi:10.1088/0004-637X/798/2/87 , adsurl =
- [76]
- [77]
- [78]
- [79]
- [80]
- [81]
- [82]
- [83]
- [84]
- [85]
-
[86]
, keywords =
Effects of Outer Giant Planets on In Situ Formation of Inner Super-Earths. , keywords =. doi:10.3847/1538-4357/adf1a6 , adsurl =
- [87]
- [88]
- [89]
- [90]
- [91]
- [92]
- [93]
- [94]
- [95]
-
[96]
A uniform re-analysis of 400 stars from the GPIES survey
The COBREX archival survey: Improved constraints on the occurrence rate of wide-orbit substellar companions: I. A uniform re-analysis of 400 stars from the GPIES survey. , keywords =. doi:10.1051/0004-6361/202452310 , archivePrefix =. 2411.06157 , primaryClass =
- [97]
- [98]
- [99]
- [100]
-
[101]
Astronomy Letters , keywords =
Activity of the Young Solar Analog HD 109833 and Estimates of the Mass Loss Rate from the Atmospheres of Its Two Planets. Astronomy Letters , keywords =. doi:10.1134/S1063773723090049 , adsurl =
- [102]
- [103]
- [104]
- [105]
- [106]
- [107]
-
[108]
, keywords =
PARSEC: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code. , keywords =. doi:10.1111/j.1365-2966.2012.21948.x , archivePrefix =. 1208.4498 , primaryClass =
2012 doi
- [109]
- [110]
-
[111]
Comparison with detached eclipsing binaries
Testing models of stellar structure and evolution - I. Comparison with detached eclipsing binaries. , keywords =. doi:10.1093/mnras/sty1371 , adsurl =
- [112]
- [113]
- [114]
-
[115]
Handbook of Exoplanets , year = 2018, editor =
CHEOPS: CHaracterizing ExOPlanets Satellite. Handbook of Exoplanets , year = 2018, editor =. doi:10.1007/978-3-319-55333-7_84 , adsurl =
2018 doi
- [116]
- [117]
-
[118]
Ground-based and Airborne Instrumentation for Astronomy VIII , year = 2020, editor =
Towards ASTEP+, a two-color photometric telescope at Dome C, Antarctica. Ground-based and Airborne Instrumentation for Astronomy VIII , year = 2020, editor =. doi:10.1117/12.2562550 , adsurl =
2020 doi
-
[119]
AAS/Division for Planetary Sciences Meeting Abstracts \#48 , year = 2016, series =
A Neptune-sized transiting planet closely orbiting a 5-10-million-year-old star. AAS/Division for Planetary Sciences Meeting Abstracts \#48 , year = 2016, series =
2016
- [120]
-
[121]
Constraints from VLT/SPHERE completed with TESS, Gaia, and radial velocities
The high-albedo, low polarization disk around HD 114082 that harbors a Jupiter-sized transiting planet. Constraints from VLT/SPHERE completed with TESS, Gaia, and radial velocities. , keywords =. doi:10.1051/0004-6361/202244380 , archivePrefix =. 2211.11767 , primaryClass =
- [122]
- [123]
- [124]
- [125]
-
[126]
Architecture of Kepler confirmed single-exoplanet systems compared to star-planet evolution models
Stellar spectral-type (mass) dependence of the dearth of close-in planets around fast-rotating stars. Architecture of Kepler confirmed single-exoplanet systems compared to star-planet evolution models. , keywords =. doi:10.1051/0004-6361/202346933 , archivePrefix =. 2311.00108...
- [127]
- [128]
- [129]
- [130]
-
[131]
, year = 1962, month = jun, volume =
Secular Perturbations of Asteroids with High Inclination and Eccentricity. , year = 1962, month = jun, volume =. doi:10.1086/108876 , adsurl =
1962 doi
- [132]
- [133]
-
[134]
, year = 1962, month = oct, volume =
The evolution of orbits of artificial satellites of planets under the action of gravitational perturbations of external bodies. , year = 1962, month = oct, volume =. doi:10.1016/0032-0633(62)90129-0 , adsurl =
1962 doi
-
[135]
, year = 1995, month = nov, volume =
A Jupiter-mass companion to a solar-type star. , year = 1995, month = nov, volume =. doi:10.1038/378355a0 , adsurl =
1995 doi
- [136]
- [137]
-
[138]
Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave , year = 2020, editor =
CHEOPS, the ESA mission for exo-planets characterization: early operations and commissioning results. Space Telescopes and Instrumentation 2020: Optical, Infrared, and Millimeter Wave , year = 2020, editor =. doi:10.1117/12.2567296 , adsurl =
2020 doi
- [139]
-
[140]
Space Telescopes and Instrumentation 2014: Optical, Infrared, and Millimeter Wave , year = 2014, editor =
Transiting Exoplanet Survey Satellite (TESS). Space Telescopes and Instrumentation 2014: Optical, Infrared, and Millimeter Wave , year = 2014, editor =. doi:10.1117/12.2063489 , archivePrefix =. 1406.0151 , primaryClass =
- [141]
- [142]
- [143]
- [144]
- [145]
- [146]
- [147]
- [148]
- [149]
- [150]
- [151]
-
[152]
A transiting warm super-Jovian planet around HD 114082, a young star with a debris disk
Radial velocity survey for planets around young stars (RVSPY). A transiting warm super-Jovian planet around HD 114082, a young star with a debris disk. , keywords =. doi:10.1051/0004-6361/202244747 , archivePrefix =. 2211.08294 , primaryClass =
- [153]
- [154]
- [155]
- [156]
- [157]
-
[158]
Insights from 178 debris systems in the ISPY, LEECH, and LIStEN planet-hunting surveys
Planet populations inferred from debris discs. Insights from 178 debris systems in the ISPY, LEECH, and LIStEN planet-hunting surveys. , keywords =. doi:10.1051/0004-6361/202142720 , archivePrefix =. 2201.08369 , primaryClass =
- [159]
- [160]
-
[161]
, keywords =
Debris disc stirring by secular perturbations from giant planets. , keywords =. doi:10.1111/j.1365-2966.2009.15360.x , archivePrefix =. 0907.1389 , primaryClass =
2009 doi
- [162]
-
[163]
, keywords =
Testing the impact of planet-stirring, self-stirring, and mixed-stirring on debris disc architecture: a case study of HD 16743. , keywords =. doi:10.1093/mnras/staf1990 , archivePrefix =. 2509.22822 , primaryClass =
-
[164]
arXiv e-prints , keywords =
The vertical structure of debris discs and the role of disc gravity. arXiv e-prints , keywords =
- [165]
- [166]
-
[167]
, archivePrefix = "arXiv", eprint =
The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , archivePrefix = "arXiv", eprint =. doi:10.3847/1538-3881/aabc4f , adsurl =
- [168]
- [169]
-
[170]
and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and
Virtanen, Pauli and Gommers, Ralf and Oliphant, Travis E. and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and. Nature Methods , year =
-
[171]
Computing in Science and Engineering , keywords =
Matplotlib: A 2D Graphics Environment. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2007.55 , adsurl =
2007 doi
-
[172]
Harris and K
Charles R. Harris and K. Jarrod Millman and St. Array programming with. 2020 , month = sep, journal =. doi:10.1038/s41586-020-2649-2 , publisher =
2020 doi
-
[173]
The Journal of Open Source Software , year = 2016, month = jun, volume =
corner.py: Scatterplot matrices in Python. The Journal of Open Source Software , year = 2016, month = jun, volume =. doi:10.21105/joss.00024 , adsurl =
2016 doi
- [174]
- [175]
-
[176]
Spearman , journal =
C. Spearman , journal =. The Proof and Measurement of Association between Two Things , urldate =
Reviewed July 12, 2026 · model on record in the stance chip above.
Discussion (0). Sign in to comment.