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Giant Outer Transiting Exoplanet Mass (GOT 'EM) Survey. VI: Confirmation of a Long-Period Giant Planet Discovered with a Single TESS Transit

T0 review · 1 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read TOI-4465 b is a confirmed massive, dense, temperate giant planet on a 101.94-day eccentric orbit, established from a single TESS transit plus radial velocities and a globally observed second transit.

desk verdict Solid incremental confirmation of a new long-period giant planet; the main issue is the unexplained exclusion of CORALIE RVs, which a referee should ask to see quantified. read the letter →

arxiv 2506.20019 v1 pith:FXA4G3XQ submitted 2025-06-24 astro-ph.EP

Zahra Essack , Diana Dragomir , Paul A. Dalba , Matthew P. Battley , David R. Ciardi , Karen A. Collins , Steve B. Howell , Matias I. Jones
show 76 more authors
Stephen R. Kane Eric E. Mamajek Christopher R. Mann Ismael Mireles Dominic Oddo Lauren A. Sgro Keivan G. Stassun Solene Ulmer-Moll Cristilyn N. Watkins Samuel W. Yee Carl Ziegler Allyson Bieryla Ioannis Apergis Khalid Barkaoui Rafael Brahm Edward M. Bryant Thomas M. Esposito Pedro Figueira Benjamin J. Fulton Samuel Gill Andrew W. Howard Howard Isaacson Alicia Kendall Nicholas Law Michael B. Lund Andrew W. Mann Rachel A. Matson Felipe Murgas Enric Palle Samuel N. Quinn Alexandre Revol Suman Saha Richard P. Schwarz Ramotholo Sefako Avi Shporer Ivan A. Strakhov Steven Villanueva Jr. George R. Ricker Roland Vanderspek David W. Latham Sara Seager Joshua N. Winn Pau Bosch-Cabot Kevin I. Collins Raquel Forés-Toribio Fabian Rodriguez Frustagia Eric Girardin Ian J. Helm Pablo Lewin Jose A. Muñoz Patrick Newman Peter Plavchan Gregor Srdoc Chris Stockdale Anaël Wünsche Mario Billiani Martin Davy Alex Douvas Keiichi Fukui Bruno Guillet Cory Ostrem Michael Rushton Angsar Schmidt Andrea Finardi Patrice Girard Tateki Goto Julien S. de Lambilly Liouba Leroux Fabrice Mortecrette John W. Pickering Michael Primm Marc Ribot Ethan Teng Aad Verveen Stefan Will Mark Ziegler
This is my paper · ORCID
classification astro-ph.EP
keywords exoplanetssingle-transiteventslong-periodgiantplanetswarmJupitersradialvelocitytransitphotometryplanetarysystemformationTOI-4465b
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 establishes that TOI-4465 b is a real transiting giant planet: a $5.89 \pm 0.26$ Jupiter-mass, $1.25^{+0.08}_{-0.07}$ Jupiter-radius world on a $101.94054$ day, mildly eccentric orbit around a G dwarf at about 122 pc. The case matters because the planet was uncovered as a single transit in TESS data, and long-period planets leave very few such events; the paper shows that radial velocities can solve the orbit and a coordinated ground-based campaign can catch the next transit, turning a one-off detection into a fully characterized system. The result adds a relatively dense ($3.73 \pm 0.53$ g/cm$^3$) and temperate (375--478 K) giant to a sparse region of mass--radius--period space, and identifies it as one of the best long-period planets for atmospheric emission spectroscopy.

What carries the argument

The load-bearing mechanism is the pairing of a single space-based transit with dense radial-velocity monitoring: the RVs set the orbital period, eccentricity, and mass, and that timing prediction then guided a global photometric campaign to catch the next transit, confirming the ephemeris. The machinery includes a joint fit of all photometry and RVs, with the stellar density left free and the planet radius and semimajor axis tied to Kepler's third law, plus stellar limb-darkening coefficients computed from model atmospheres. The long transit duration (about 12 hours) is what makes worldwide longitudinal coverage essential and practical, and the lack of detected stellar companions from high-resolution imaging validates the single-star dilution assumption.

What would settle it

Measure the stellar radius independently, for example with asteroseismology or long-baseline interferometry, and compare it with $1.014 \pm 0.041\,R_\odot$; a disagreement larger than about 8% (roughly 2 $\sigma$) would rescale the planetary radius, density, and heavy-element mass enough to shift several of the paper's conclusions.

Watch

Extended reading notes

Core claim

The central claim is that TOI-4465 b is a confirmed transiting giant with orbital period $P = 101.94054^{+0.00040}_{-0.00036}$ d, radial-velocity semi-amplitude $K = 277.19^{+2.37}_{-1.90}$ m/s, eccentricity $e = 0.24 \pm 0.01$, radius $R_p = 1.25^{+0.08}_{-0.07}\,R_J$, and mass $M_p = 5.89 \pm 0.26\,M_J$. A single TESS transit in Sector 40 triggered the search; radial velocities from three spectrographs determined the period and amplitude, and a worldwide photometric campaign caught the roughly 12-hour second transit, confirming the ephemeris. From the joint fit the paper derives a bulk density of $3.73 \pm 0.53$ g/cm$^3$ and equilibrium temperatures of 375 K at apastron and 478 K at periastron. Comparing the planet to giant-planet structure models, it finds a heavy-element mass fraction $Z_p = 0.091 \pm 0.017$, or about $171 \pm 32$ Earth masses of heavy elements, roughly $7.5 \pm 1.4$ times the host star's heavy-element fraction. The paper further argues that TOI-4465 b is the largest-radius giant with $P > 100$ days, one of the most massive such planets, and a strong target for emission spectroscopy and obliquity measurement.

Load-bearing premise

The adopted stellar radius and mass—$R_* = 1.014 \pm 0.041\,R_\odot$ and $M_* = 0.93 \pm 0.06\,M_\odot$, from the spectral-energy-distribution plus Gaia analysis—must be correct, because every derived planetary radius, mass, density, and heavy-element mass rescales directly from those values even though the transit and radial-velocity detection themselves would survive.

Editorial extensions

If this is right

  • Single-transit TESS candidates can be promoted to precisely characterized planets when the RV-anchored ephemeris is followed by a coordinated second-transit campaign, so the confirmation path demonstrated here should be reusable for many similar candidates.
  • TOI-4465 b becomes a benchmark giant planet at $P > 100$ days with radius, mass, and density all measured to better than 10%, sharpening the mass--radius relation for non-inflated, temperate giants.
  • With the third-highest emission spectroscopy metric among confirmed long-period giants, TOI-4465 b is one of the best available targets for probing cool-giant chemistry such as CO/CH$_4$ and N$_2$/NH$_3$ disequilibrium.
  • Its heavy-element enrichment of $Z_p/Z_* = 7.5 \pm 1.4$ is consistent with late-stage accretion of icy planetesimals, adding a high-mass, low-host-metallicity data point to tests of core-accretion versus disk-instability formation.
  • The predicted Rossiter--McLaughlin amplitude of up to about 42 m/s makes TOI-4465 b a viable candidate for measuring the obliquity of a long-period planet, which would test disk versus dynamical migration histories.

Reading between the lines

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

  • Extension: If the same single-transit-plus-RV-plus-second-transit recipe works at scale, the census of planets beyond 100-day periods could grow quickly, and population comparisons between hot, warm, and cold giants would become statistically meaningful.
  • Extension: The unusually high density for a 5.9-Jupiter-mass planet at this period suggests modest envelope inflation; measuring the planet's infrared emission could test whether tidal or stellar irradiation effects are truly negligible at these separations.
  • Extension: A third transit observed at the predicted time would shrink the period uncertainty further and open a search for transit-timing variations that could reveal an outer companion in the system.
  • Extension: The host star's apparently super-solar magnesium abundance, if confirmed by higher-resolution abundance work, could point to a chemical environment that favored efficient solid accretion, offering a testable link to the planet's heavy-element content.
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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

1 major / 5 minor

Summary. The manuscript reports the discovery and confirmation of TOI-4465 b, a transiting giant planet first detected as a single TESS Sector 40 transit. The authors combine TESS and ground-based photometry (LCOGT, NGTS, Unistellar/eVscope, and NEOSSat) with radial velocities from APF, CHIRON, and TRES in a joint juliet fit, yielding P = 101.94054 d, K = 277.19 m/s, e = 0.24, Rp = 1.25 RJ, Mp = 5.89 MJ, and a bulk density of 3.73 g/cm^3. The RV-determined period was used to predict and then observe a second transit from multiple sites, providing an independent confirmation of the ephemeris. The paper also discusses the planet's population context, atmospheric characterization prospects, heavy-element enrichment, and obliquity measurement.

Significance. If accepted, this is a valuable addition to the small sample of long-period transiting giant planets: TOI-4465 b is claimed to have the largest radius among transiting giants with P > 100 days and is among the best long-period targets for emission spectroscopy. The detection strategy is strong in an important respect: the RV period was fit independently of the later ground-based transit, and that transit was predicted from the RV period and then observed, rather than being used circularly in the period solution. The detailed data tables and the use of published structure models for the heavy-element interpretation are additional strengths. The main caveats are that the derived planetary properties scale directly with the SED-based stellar radius and mass, and the exclusion of the CORALIE RVs from the final fit is not yet demonstrated to be innocuous.

major comments (1)
  1. [Sections 3.2.4 and 4.2; Tables 6 and 7] The exclusion of the six CORALIE RVs from the final fit is not adequately justified, and because the final orbital parameters are load-bearing for the paper's central claim, this needs to be fixed. The text in Sections 3.2.4 and 4.2 states that the CORALIE data have 'large errorbars' and 'added noise without enhancing model precision,' but Table 7 lists quoted uncertainties of 6.5-14.7 m/s, which are comparable to APF and CHIRON and smaller than most TRES uncertainties (17.5-29.4 m/s; Table 6). The manuscript reports that the data were modeled with and without CORALIE, but gives no quantitative comparison of the two fits. If the six points are consistent with the adopted solution, they should be retained or their removal should be justified by a numerical model comparison; if they are in tension, the tension must be diagnosed rather than hidden by exclusion. Please report the CORALIE-inclusive values of P, K, e, and omega (with a fitted CORALIE offset), the change in log evidence or chi-square, and a brief residual analysis for the six points.
minor comments (5)
  1. [Section 3.2.1, Table 4] Three APF epochs (2459817.77572, 2459835.70532, and 2459850.70414) appear twice with identical RVs and uncertainties; please clarify whether these are genuine duplicate exposures or a copying error in the table.
  2. [Table 8] The final Hazelwood Observatory row lists start and end times of 10414.1959-10414.2601, which is inconsistent with the BTJD-2450000 convention used for the other rows and with the 2022 campaign dates; this is presumably a typo and should be corrected.
  3. [Section 5.3] The heavy-element enrichment calculation follows Thorngren et al. (2016), a framework noted to be calibrated for planets with P < 100 days, while TOI-4465 b has P = 101.94 days; the text should add a sentence quantifying the expected extrapolation uncertainty.
  4. [Section 2.1] The reduced chi-squared of 1.5 for the SED fit would be more informative with the number of degrees of freedom, since a reduced chi-squared near 1.5 can indicate either an acceptable fit or underestimated photometric uncertainties depending on the number of constraints.
  5. [Section A1 / Figure A1] The corner plot of the posterior distribution is not referenced in the main text; please add a pointer in Section 4 so that readers know the full posterior covariances are available.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the discovery chain is empirically self-contained.

full rationale

The paper's central claim—a confirmed transiting giant planet with P ≈ 101.94 d—rests on three independent data sets joined in one juliet fit: the TESS single transit, the APF/CHIRON/TRES radial velocities, and a ground-based second transit. The ground-based campaign was scheduled from an ephemeris predicted from the TESS transit epoch and the RV period (Section 3.3), and the later detection of the transit at the predicted time is independent confirmation, not a constructed output; had the RV period been wrong, the transit would have been missed. The final period is jointly re-fit, not defined by the prior prediction. The adopted stellar radius and mass (Section 2.1) come from SED and Gaia analysis using the published Stassun & Torres and Stassun et al. procedures; one co-author of those method papers appears here, but the method is external, standard, and validated, so the citation is not load-bearing. The heavy-element enrichment (Section 5.3) is computed with Thorngren et al. (2016) models and then compared with that same paper's empirical mass-metallicity correlation; this is a consistency comparison, not a derivation of the correlation from this planet's fit. No equation in the paper defines a fitted parameter as its own predicted quantity. The exclusion of the six CORALIE RVs (Sections 3.2.4 and 4.2) on the grounds that they 'added noise without enhancing model precision' is a data-selection/auditability concern rather than a circular step, and it does not make the central derivation self-referential.

Assumptions & free parameters 9 free parameters · 6 assumptions · 0 invented entities

The central discovery claim is empirical and rests on standard observational fitting. The free parameters are the fitted orbital and planetary parameters plus instrument nuisances; no ad hoc physical entities are introduced. The heavy-element enrichment is a model-dependent interpretation, not a new entity.

free parameters (9)
  • Orbital period P = 101.94054(+0.00040,-0.00036) d
    Fitted jointly to RV and transit photometry (Table 9); central to scheduling and confirmation.
  • Transit epoch T0 = 2459395.1256 ± 0.0006 BJD_TDB
    Fitted in the juliet joint model; anchors the ephemeris.
  • Planet-to-star radius ratio p = Rp/R* = 0.1268 ± 0.0004
    Fitted to TESS and ground-based transit photometry; yields the planet radius.
  • RV semi-amplitude K = 277.19(+2.37,-1.90) m/s
    Fitted to APF, CHIRON and TRES radial velocities; yields the planet mass.
  • Orbital eccentricity e = 0.24 ± 0.01
    Fitted jointly with omega; important for the interpretation and temperature range.
  • Argument of periastron omega = 279.74(+0.58,-0.57) deg
    Fitted jointly with eccentricity in the RV model.
  • Stellar density rho* = 1.30(+0.41,-0.44) g/cm3
    Fitted in the transit model and combined with adopted stellar mass and radius.
  • TESS limb darkening q1, q2 = 0.31 ± 0.02, 0.39 ± 0.01
    Fitted with normal priors; non-TESS limb darkening coefficients are fixed from PyLDTK.
  • Per-instrument offsets and jitter (RV and photometry) = Tables 9 and A2
    Nuisance parameters for APF, CHIRON, TRES, TESS, LCOGT, NGTS, NEOSSat, and 13 Unistellar datasets; not central to the planet claim.
assumptions (6)
  • domain assumption The TESS single transit and ground-based transits are caused by a planet transiting TOI-4465, not by a blended eclipsing binary.
    High-resolution imaging from Gemini, SOAR, SAI, Palomar and Lick rules out companions, and the RV signal is consistent with the planet. See Sections 2.2 and 4.
  • domain assumption The host star's radius and mass from SED fitting, R* = 1.014 ± 0.041 Rsun and M* = 0.93 ± 0.06 Msun, are correct.
    Derived in Section 2.1 using PHOENIX model fits, Gaia parallax, and empirical relations; adopted in all planet parameter calculations.
  • domain assumption The radial velocities are dominated by a single planet.
    The model in Section 4.2 fits one Keplerian; the paper notes the eccentricity could indicate an unseen outer planet but does not perform a systematic multi-planet search.
  • domain assumption Limb darkening coefficients for LCOGT, NGTS, NEOSSat and Unistellar, computed from PHOENIX and PyLDTK, are fixed and correct.
    Section 4.1 fixes these coefficients; their uncertainties are not propagated into the final planet parameters.
  • domain assumption Giant-planet structure models from Thorngren et al. (2016) are applicable for inferring the heavy-element content.
    Section 5.3 uses these models to derive Zp = 0.091 ± 0.017 and Mz = 171 ± 32 Earth masses.
  • domain assumption The equilibrium temperature range assumes zero albedo and full heat redistribution.
    The 375-478 K range in Section 5 and Table 10 is explicitly computed under these assumptions.

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Cite this review

Pith. "Pith review of Giant Outer Transiting Exoplanet Mass (GOT 'EM) Survey. VI: Confirmation of a Long-Period Giant Planet Discovered with a Single TESS Transit." pith.science (2026). https://pith.science/paper/FXA4G3XQ

@misc{pith2026250620019,
  author       = {Pith},
  title        = {Pith review of: Giant Outer Transiting Exoplanet Mass (GOT 'EM) Survey. VI: Confirmation of a Long-Period Giant Planet Discovered with a Single TESS Transit},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/FXA4G3XQ}},
  note         = {Machine review of arXiv:2506.20019}
}
abstract

We report the discovery and confirmation of TOI-4465 b, a $1.25^{+0.08}_{-0.07}~R_{J}$, $5.89\pm0.26~M_{J}$ giant planet orbiting a G dwarf star at $d\simeq$ 122 pc. The planet was detected as a single-transit event in data from Sector 40 of the Transiting Exoplanet Survey Satellite (TESS) mission. Radial velocity (RV) observations of TOI-4465 showed a planetary signal with an orbital period of $\sim$102 days, and an orbital eccentricity of $e=0.24\pm0.01$. TESS re-observed TOI-4465 in Sector 53 and Sector 80, but did not detect another transit of TOI-4465 b, as the planet was not expected to transit during these observations based on the RV period. A global ground-based photometry campaign was initiated to observe another transit of TOI-4465 b after the RV period determination. The $\sim$12 hour-long transit event was captured from multiple sites around the world, and included observations from 24 citizen scientists, confirming the orbital period as $\sim$102 days. TOI-4465 b is a relatively dense ($3.73\pm0.53~\rm{g/cm^3}$), temperate (375-478 K) giant planet. Based on giant planet structure models, TOI-4465 b appears to be enriched in heavy elements at a level consistent with late-stage accretion of icy planetesimals. Additionally, we explore TOI-4465 b's potential for atmospheric characterization, and obliquity measurement. Increasing the number of long-period planets by confirming single-transit events is crucial for understanding the frequency and demographics of planet populations in the outer regions of planetary systems.

Figures

Figures reproduced from arXiv: 2506.20019 by the authors.

Figure 1
Figure 1. Spectral energy distribution of TOI-4465. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best￾fit PHOENIX atmosphere model (black). The inset shows the absolute flux-calibrated Gaia spectrophotometry as a gray swathe overlaid on the model (black). AAVSO Photometric All-Sky Survey (APASS) … view at source ↗
Figure 2
Figure 2. Gemini-North ‘Alopeke 5σ speckle imaging con￾trast curves in 562 nm filter (blue line) and 832 nm filter (red line) as a function of the angular separation out to 1.2”. The inset shows the reconstructed 832 nm image of TOI-4465 with a 1” scale bar. TOI-4465 was found to have no close companions from the diffraction limit out to 1.2” to within the contrast levels achieved. imaging provides crucial information toward … view at source ↗
Figure 4
Figure 4. SAI speckle-imaging observations of TOI￾4465. The contrast curve (5σ sensitivity limits), and auto￾correlation functions (inset) are shown. was estimated from 4000 frames with 30 ms exposure. The detector has a pixel scale of 20.6 mas/pixel, and the angular resolution was 89 mas. Long-exposure see￾ing was 0.92′′. We did not detect any stellar compan￾ions brighter than ∆IC = 5.0 and 6.5 at ρ = 0.25′′ and 1 ′′, respec… view at source ↗
Figures from the paper (8 more)
Figure 5
Figure 5. Figure 5: NIR AO imaging and sensitivity curves for the Palomar Observations. Insets: Image of the central portion of the image. the Palomar Hale (5 m) telescope behind the P3K nat￾ural guide star AO system (Dekany et al. 2013) in the narrowband Br-γ filter (λo = 2.1686; ∆λ = 0.…
Figure 6
Figure 6. Figure 6: TESS light curves of TOI-4465. Top: Detrended, normalized and flattened Sector 40 FFI light curve. Lighter gray points are the TESS 10-minute cadence flux measurements; darker points are the same data binned into 2.5-hour intervals. The single-transit occurred at 24593…
Figure 7
Figure 7. Figure 7: Results of the juliet joint fit to the APF, CHIRON and TRES radial velocities. Top: APF (blue points), CHIRON (green points) and TRES (orange points) RVs over time, and full best-fit juliet model (black curve). Middle: Phase-folded RV measurements from APF, CHIRON and …
Figure 8
Figure 8. Figure 8: Results of the juliet joint fit to LCOGT, NGTS and NEOSSat photometry. Top: Transit observations of the respective instruments phase-folded to the period of TOI-4465 b. The black curve is the best-fit juliet transit model, and the 68% confidence interval is represented…
Figure 9
Figure 9. Figure 9: Results of the juliet joint fit to the Unistellar photometry. Top: Photometric data from the 13 eVscopes phase￾folded to the period of TOI-4465 b. The gray band is the best-fit juliet transit model with 1σ uncertainty. The binned data (red points) with errorbars are sh…
Figure 10
Figure 10. Figure 10: Mass-radius diagram for confirmed giant planets (Rp > 0.2 RJ, Mp < 13 MJ) with measured mass and radius uncertainties below 20%. Planets are colored according to their average equilibrium temperature (calculated assuming zero albedo and efficient heat redistribution).…
Figure 11
Figure 11. Figure 11: Period-radius plot for confirmed giant planets (Rp > 0.2 RJ, Mp < 13 MJ) with measured mass and radius uncertainties below 20%. Planets are colored according to their mass. TOI-4465 b has the largest radius among giant planets with P > 100 days, and the second most ma…
Figure 12
Figure 12. Figure 12: Period-mass plot for confirmed giant planets (Rp > 0.2 RJ, Mp < 13 MJ) with measured mass and radius uncertainties below 20%. Planets are colored according to their orbital eccentricity. Planets at longer orbital periods generally trend towards higher eccentricities. …

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Works this paper leans on

147 extracted references · 3 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    g7FKmjU1ff S(@( @R

    thebibliography [1] 20pt to REFERENCES 6pt =0pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command E...

    2021

  4. [4]

    2019, Geosciences, 9, 105

    Adibekyan, V. 2019, Geosciences, 9, 105

    2019

  5. [5]

    N., Johnson, J

    Albrecht, S., Winn, J. N., Johnson, J. A., et al. 2012, The Astrophysical Journal, 757, 18

    2012

  6. [6]

    2019, , 628, A94, 10.1051/0004-6361/201935765

    Anders , F., Khalatyan , A., Chiappini , C., et al. 2019, , 628, A94, 10.1051/0004-6361/201935765

    doi:10.1051/0004-6361/201935765 2019

  7. [7]

    Anders , F., Khalatyan , A., Queiroz , A. B. A., et al. 2022, , 658, A91, 10.1051/0004-6361/202142369

    doi:10.1051/0004-6361/202142369 2022

  8. [8]

    Bailer-Jones , C. A. L., Rybizki , J., Fouesneau , M., Demleitner , M., & Andrae , R. 2021, , 161, 147, 10.3847/1538-3881/abd806

    doi:10.3847/1538-3881/abd806 2021

Show all 147 references
  1. [9]

    Bensby , T., Feltzing , S., & Oey , M. S. 2014, , 562, A71, 10.1051/0004-6361/201322631

    2014 doi

  2. [10]

    Boss, A. P. 1997, Science, 276, 1836

    1997

  3. [11]

    2019, , 158, 45, 10.3847/1538-3881/ab279a

    Brahm , R., Espinoza , N., Jord \'a n , A., et al. 2019, , 158, 45, 10.3847/1538-3881/ab279a

    2019 doi

  4. [12]

    M., Baliber , N., Bianco , F

    Brown , T. M., Baliber , N., Bianco , F. B., et al. 2013, , 125, 1031, 10.1086/673168

    2013 doi

  5. [13]

    M., Bayliss, D., McCormac, J., et al

    Bryant, E. M., Bayliss, D., McCormac, J., et al. 2020, Monthly Notices of the Royal Astronomical Society, 494, 5872

    2020

  6. [14]

    A., Bakos , G

    Buchhave , L. A., Bakos , G. \'A ., Hartman , J. D., et al. 2010, , 720, 1118, 10.1088/0004-637X/720/2/1118

    2010 doi

  7. [15]

    A., Latham, D., Johansen, A., et al

    Buchhave, L. A., Latham, D., Johansen, A., et al. 2012, Nature, 486, 375

    2012

  8. [16]

    P., Marcy, G

    Butler, R. P., Marcy, G. W., Williams, E., et al. 1996, Publications of the Astronomical Society of the Pacific, 108, 500

    1996

  9. [17]

    A., Tenenbaum , P., Twicken , J

    Caldwell , D. A., Tenenbaum , P., Twicken , J. D., et al. 2020, Research Notes of the American Astronomical Society, 4, 201, 10.3847/2515-5172/abc9b3

    2020 doi

  10. [18]

    N., & Davies , M

    Carrera , D., Raymond , S. N., & Davies , M. B. 2019, , 629, L7, 10.1051/0004-6361/201935744

    2019 doi

  11. [19]

    R., Beichman , C

    Ciardi , D. R., Beichman , C. A., Horch , E. P., & Howell , S. B. 2015, , 805, 16, 10.1088/0004-637X/805/1/16

    2015 doi

  12. [20]

    S., Raymond , S

    Clement , M. S., Raymond , S. N., Kaib , N. A., et al. 2021, , 355, 114122, 10.1016/j.icarus.2020.114122

    2021

  13. [21]

    2019, in American Astronomical Society Meeting Abstracts, Vol

    Collins , K. 2019, in American Astronomical Society Meeting Abstracts, Vol. 233, American Astronomical Society Meeting Abstracts \#233, 140.05

    2019

  14. [22]

    A., Kielkopf , J

    Collins , K. A., Kielkopf , J. F., Stassun , K. G., & Hessman , F. V. 2017, , 153, 77, 10.3847/1538-3881/153/2/77

    2017 doi

  15. [23]

    F., Pollacco, D., Anderson, D

    Cooke, B. F., Pollacco, D., Anderson, D. R., et al. 2021, Monthly Notices of the Royal Astronomical Society, 500, 5088

    2021

  16. [24]

    2003, The IRSA 2MASS All-Sky Point Source Catalog

    Cutri, R., Skrutskie, M., Van Dyk, S., et al. 2003, The IRSA 2MASS All-Sky Point Source Catalog

    2003

  17. [25]

    M., & et al

    Cutri , R. M., & et al. 2012, VizieR Online Data Catalog, II/311

    2012

  18. [26]

    D., et al

    Cziranka-Crooks , N., Hrynyk , T., Balam , D. D., et al. 2023, in 2nd NEO and Debris Detection Conference, 60

    2023

  19. [27]

    A., & Muirhead , P

    Dalba , P. A., & Muirhead , P. S. 2016, , 826, L7, 10.3847/2041-8205/826/1/L7

    2016 doi

  20. [28]

    A., Muirhead , P

    Dalba , P. A., Muirhead , P. S., Croll , B., & Kempton , E. M.-R. 2017, , 153, 59, 10.1088/1361-6528/aa5278

    2017 doi

  21. [29]

    A., Kane, S

    Dalba, P. A., Kane, S. R., Dragomir, D., et al. 2022, The Astronomical Journal, 163, 61

    2022

  22. [30]

    2013, , 776, 130, 10.1088/0004-637X/776/2/130

    Dekany , R., Roberts , J., Burruss , R., et al. 2013, , 776, 130, 10.1088/0004-637X/776/2/130

    2013 doi

  23. [31]

    2018, Research Notes of the AAS, 2, 209, 10.3847/2515-5172/aaef38

    Espinoza, N. 2018, Research Notes of the AAS, 2, 209, 10.3847/2515-5172/aaef38

    2018 doi

  24. [32]

    2019, Monthly Notices of the Royal Astronomical Society, 490, 2262

    Espinoza, N., Kossakowski, D., & Brahm, R. 2019, Monthly Notices of the Royal Astronomical Society, 490, 2262

    2019

  25. [33]

    2007, The Astrophysical Journal, 669, 1298

    Fabrycky, D., & Tremaine, S. 2007, The Astrophysical Journal, 669, 1298

    2007

  26. [34]

    2008, PhD thesis, University of Szeged, Hungary

    F u r\'esz, G. 2008, PhD thesis, University of Szeged, Hungary

    2008

  27. [35]

    J., Marley, M

    Fortney, J. J., Marley, M. S., & Barnes, J. W. 2007, The Astrophysical Journal, 659, 1661

    2007

  28. [36]

    J., & Nettelmann, N

    Fortney, J. J., & Nettelmann, N. 2010, Space Science Reviews, 152, 423

    2010

  29. [37]

    J., Visscher, C., Marley, M

    Fortney, J. J., Visscher, C., Marley, M. S., et al. 2020, The Astronomical Journal, 160, 288

    2020

  30. [38]

    2022, in AAS/Division for Planetary Sciences Meeting Abstracts, Vol

    Fox , C., & Wiegert , P. 2022, in AAS/Division for Planetary Sciences Meeting Abstracts, Vol. 54, AAS/Division for Planetary Sciences Meeting Abstracts, 215.03

    2022

  31. [39]

    J., Petigura, E

    Fulton, B. J., Petigura, E. A., Blunt, S., & Sinukoff, E. 2018, Publications of the Astronomical Society of the Pacific, 130, 044504

    2018

  32. [40]

    J., Collins, K

    Fulton, B. J., Collins, K. A., Gaudi, B. S., et al. 2015, The Astrophysical Journal, 810, 30

    2015

  33. [41]

    2017, The Astronomical Journal, 154, 66

    Furlan, E., & Howell, S. 2017, The Astronomical Journal, 154, 66

    2017

  34. [42]

    2020, The Astrophysical Journal, 898, 47

    ---. 2020, The Astrophysical Journal, 898, 47

    2020

  35. [43]

    R., Everett , M

    Furlan , E., Ciardi , D. R., Everett , M. E., et al. 2017, , 153, 71, 10.3847/1538-3881/153/2/71

    2017 doi

  36. [44]

    Gaia Collaboration , Brown , A. G. A., Vallenari , A., et al. 2018, , 616, A1, 10.1051/0004-6361/201833051

    2018 doi

  37. [45]

    2021 a , , 649, A1, 10.1051/0004-6361/202039657

    ---. 2021 a , , 649, A1, 10.1051/0004-6361/202039657

    2021 doi

  38. [46]

    L., Sarro , L

    Gaia Collaboration , Smart , R. L., Sarro , L. M., et al. 2021 b , , 649, A6, 10.1051/0004-6361/202039498

    2021 doi

  39. [47]

    S., Zahnle, K., Robinson, T

    Gao, P., Marley, M. S., Zahnle, K., Robinson, T. D., & Lewis, N. K. 2017, The Astronomical Journal, 153, 139

    2017

  40. [48]

    2019, The Astrophysical Journal, 876, 23

    Goda, S., & Matsuo, T. 2019, The Astrophysical Journal, 876, 23

    2019

  41. [49]

    1980, Astrophysical Journal, Part 1, vol

    Goldreich, P., & Tremaine, S. 1980, Astrophysical Journal, Part 1, vol. 241, Oct. 1, 1980, p. 425-441., 241, 425

    1980

  42. [50]

    M., Seager, S., Huang, C

    Guerrero, N. M., Seager, S., Huang, C. X., et al. 2021, The Astrophysical Journal Supplement Series, 254, 39

    2021

  43. [51]

    Guillot, T., & Showman, A. P. 2002, Astronomy & Astrophysics, 385, 156

    2002

  44. [52]

    F., Millholland, S

    Gupta, A. F., Millholland, S. C., Im, H., et al. 2024, Nature, 1

    2024

  45. [53]

    L., Brandl , B., Pirger , B., et al

    Hayward , T. L., Brandl , B., Pirger , B., et al. 2001, , 113, 105, 10.1086/317969

    2001 doi

  46. [54]

    2006, Icarus, 185, 64

    Helled, R., Podolak, M., & Kovetz, A. 2006, Icarus, 185, 64

    2006

  47. [55]

    A., Levine , S

    Henden , A. A., Levine , S. E., Terrell , D., Smith , T. C., & Welch , D. 2012, , 40, 430

    2012

  48. [56]

    B., Everett, M

    Howell, S. B., Everett, M. E., Sherry, W., Horch, E., & Ciardi, D. R. 2011, The Astronomical Journal, 142, 19

    2011

  49. [57]

    B., Scott, N

    Howell, S. B., Scott, N. J., Matson, R. A., et al. 2021, Frontiers in Astronomy and Space Sciences, 8, 635864

    2021

  50. [58]

    Huang, C., Wu, Y., & Triaud, A. H. 2016, The Astrophysical Journal, 825, 98

    2016

  51. [59]

    X., Vanderburg, A., P \'a l, A., et al

    Huang, C. X., Vanderburg, A., P \'a l, A., et al. 2020, Research Notes of the AAS, 4, 204

    2020

  52. [61]

    2013 b , , 553, A6, 10.1051/0004-6361/201219058

    ---. 2013 b , , 553, A6, 10.1051/0004-6361/201219058

    2013 doi

  53. [62]

    M., Twicken , J

    Jenkins , J. M., Twicken , J. D., McCauliff , S., et al. 2016, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9913, The TESS science processing operations center , 99133E, 10.1117/12.2233418

    2016 doi

  54. [63]

    2013, Tapir: A web interface for transit/eclipse observability , Astrophysics Source Code Library

    Jensen , E. 2013, Tapir: A web interface for transit/eclipse observability , Astrophysics Source Code Library. 1306.007

    2013

  55. [64]

    I., Brahm , R., Espinoza , N., et al

    Jones , M. I., Brahm , R., Espinoza , N., et al. 2019, , 625, A16, 10.1051/0004-6361/201834640

    2019 doi

  56. [65]

    I., Reinarz , Y., Brahm , R., et al

    Jones , M. I., Reinarz , Y., Brahm , R., et al. 2024, , 683, A192, 10.1051/0004-6361/202348147

    2024 doi

  57. [66]

    R., Ciardi , D

    Kane , S. R., Ciardi , D. R., Gelino , D. M., & von Braun , K. 2012, , 425, 757, 10.1111/j.1365-2966.2012.21627.x

    2012

  58. [67]

    R., & Raymond , S

    Kane , S. R., & Raymond , S. N. 2014, , 784, 104, 10.1088/0004-637X/784/2/104

    2014 doi

  59. [68]

    R., & Wittenmyer , R

    Kane , S. R., & Wittenmyer , R. A. 2024, , 962, L21, 10.3847/2041-8213/ad2463

    2024 doi

  60. [69]

    R., Hill , M

    Kane , S. R., Hill , M. L., Dalba , P. A., et al. 2023, , 165, 252, 10.3847/1538-3881/acd17a

    2023 doi

  61. [70]

    M.-R., Bean, J

    Kempton, E. M.-R., Bean, J. L., Louie, D. R., et al. 2018, Publications of the Astronomical Society of the Pacific, 130, 114401

    2018

  62. [71]

    Kipping, D. M. 2013, Monthly Notices of the Royal Astronomical Society, 435, 2152

    2013

  63. [72]

    J., et al

    Kordopatis , G., Schultheis , M., McMillan , P. J., et al. 2023, , 669, A104, 10.1051/0004-6361/202244283

    2023 doi

  64. [73]

    2015, Publications of the Astronomical Society of the Pacific, 127, 1161

    Kreidberg, L. 2015, Publications of the Astronomical Society of the Pacific, 127, 1161

    2015

  65. [74]

    2019, Astronomy & Astrophysics, 632, A65

    Kubyshkina, D., Fossati, L., Mustill, A., et al. 2019, Astronomy & Astrophysics, 632, A65

    2019

  66. [75]

    2022, Research Notes of the AAS, 6, 236

    Kunimoto, M., Tey, E., Fong, W., et al. 2022, Research Notes of the AAS, 6, 236

    2022

  67. [76]

    2021, Research Notes of the AAS, 5, 234

    Kunimoto, M., Huang, C., Tey, E., et al. 2021, Research Notes of the AAS, 5, 234

    2021

  68. [77]

    Kurucz , R. L. 1992, in The Stellar Populations of Galaxies, ed. B. Barbuy & A. Renzini , Vol. 149, 225

    1992

  69. [78]

    2018, , 616, A132, 10.1051/0004-6361/201832832

    Lallement , R., Capitanio , L., Ruiz-Dern , L., et al. 2018, , 616, A132, 10.1051/0004-6361/201832832

    2018 doi

  70. [79]

    V., Matson, R

    Lester, K. V., Matson, R. A., Howell, S. B., et al. 2021, The Astronomical Journal, 162, 75

    2021

  71. [80]

    Lightkurve Collaboration , Cardoso , J. V. d. M., Hedges , C., et al. 2018, Lightkurve: Kepler and TESS time series analysis in Python , Astrophysics Source Code Library. 1812.013

    2018

  72. [81]

    L., Zhao , Y

    Luo , A. L., Zhao , Y. H., Zhao , G., & et al. 2019, VizieR Online Data Catalog

    2019

  73. [82]

    2022, VizieR Online Data Catalog

    ---. 2022, VizieR Online Data Catalog

    2022

  74. [83]

    L., Zhao , Y

    Luo , A. L., Zhao , Y. H., Zhao , G., et al. 2016, VizieR Online Data Catalog

    2016

  75. [84]

    2019, Astronomy & Astrophysics, 624, A94

    Maldonado, J., Villaver, E., Eiroa, C., & Micela, G. 2019, Astronomy & Astrophysics, 624, A94

    2019

  76. [85]

    E., & Hillenbrand , L

    Mamajek , E. E., & Hillenbrand , L. A. 2008, , 687, 1264, 10.1086/591785

    2008 doi

  77. [86]

    2024, in TESS Science Conference III, 24, 10.5281/zenodo.13387460

    Mann , C. 2024, in TESS Science Conference III, 24, 10.5281/zenodo.13387460

    2024 doi

  78. [87]

    R., Dalba, P

    Mann, C. R., Dalba, P. A., Lafreni \`e re, D., et al. 2023, The Astronomical Journal, 166, 239

    2023

  79. [88]

    2020, Acta Astronautica, 166, 23, 10.1016/j.actaastro.2019.09.028

    Marchis , F., Malvache , A., Marfisi , L., Borot , A., & Arbouch , E. 2020, Acta Astronautica, 166, 23, 10.1016/j.actaastro.2019.09.028

    2020 doi

  80. [89]

    Y., & Ipatov , S

    Marov , M. Y., & Ipatov , S. I. 2018, Solar System Research, 52, 392, 10.1134/S0038094618050052

    2018 doi

  81. [90]

    A., Howell, S

    Matson, R. A., Howell, S. B., Horch, E. P., & Everett, M. E. 2018, The Astronomical Journal, 156, 31

    2018

  82. [91]

    McCall , M. L. 2004, , 128, 2144, 10.1086/424933

    2004 doi

  83. [92]

    H., Harbeck , D.-R., et al

    McCully , C., Volgenau , N. H., Harbeck , D.-R., et al. 2018, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 10707, , 107070K, 10.1117/12.2314340

    2018 doi

  84. [93]

    McLaughlin , D. B. 1924, , 60, 22, 10.1086/142826

    1924 doi

  85. [94]

    2016, The Astrophysical Journal, 832, 41

    Mordasini, C., van Boekel, R., Molli \`e re, P., Henning, T., & Benneke, B. 2016, The Astrophysical Journal, 832, 41

    2016

  86. [95]

    Ohno, K., & Fortney, J. J. 2023, The Astrophysical Journal, 956, 125

    2023

  87. [96]

    2020, Monthly Notices of the Royal Astronomical Society, 491, 4481

    Osborn, A., & Bayliss, D. 2020, Monthly Notices of the Royal Astronomical Society, 491, 4481

    2020

  88. [97]

    A., Henry , T

    Paredes , L. A., Henry , T. J., Quinn , S. N., et al. 2021, , 162, 176, 10.3847/1538-3881/ac082a

    2021 doi

  89. [98]

    Parviainen , H. 2015, PyLDTk: Python toolkit for calculating stellar limb darkening profiles and model-specific coefficients for arbitrary filters, Astrophysics Source Code Library, record ascl:1510.003. 1510.003

    2015

  90. [99]

    2015, , 453, 3821, 10.1093/mnras/stv1857

    Parviainen , H., & Aigrain , S. 2015, , 453, 3821, 10.1093/mnras/stv1857

    2015 doi

  91. [100]

    O., Esposito, T

    Peluso, D. O., Esposito, T. M., Marchis, F., et al. 2023, Publications of the Astronomical Society of the Pacific, 135, 015001

    2023

  92. [101]

    O., Dalba, P

    Peluso, D. O., Dalba, P. A., Wright, D., et al. 2024, The Astronomical Journal, 167, 170

    2024

  93. [102]

    2002, Messenger, 110, 9

    Pepe, F., Mayor, M., Rupprecht, G., et al. 2002, Messenger, 110, 9

    2002

  94. [103]

    A., Marcy, G

    Petigura, E. A., Marcy, G. W., Winn, J. N., et al. 2018, The Astronomical Journal, 155, 89

    2018

  95. [104]

    B., Hubickyj, O., Bodenheimer, P., et al

    Pollack, J. B., Hubickyj, O., Bodenheimer, P., et al. 1996, icarus, 124, 62

    1996

  96. [105]

    Queiroz , A. B. A., Anders , F., Chiappini , C., et al. 2020, , 638, A76, 10.1051/0004-6361/201937364

    2020 doi

  97. [106]

    2000, arXiv preprint astro-ph/0006213

    Queloz, D., Eggenberger, A., Mayor, M., et al. 2000, arXiv preprint astro-ph/0006213

    2000 arXiv

  98. [107]

    2001, The Messenger, No

    Queloz, D., Mayor, M., Udry, S., et al. 2001, The Messenger, No. 105, p. 1-7 (September 2001), 105, 1

    2001

  99. [108]

    V., Cabak, G

    Radovan, M. V., Cabak, G. F., Laiterman, L. H., Lockwood, C. T., & Vogt, S. S. 2010, in Ground-based and Airborne Instrumentation for Astronomy III, Vol. 7735, SPIE, 1736--1748

    2010

  100. [109]

    V., Lanclos, K., Holden, B

    Radovan, M. V., Lanclos, K., Holden, B. P., et al. 2014, in Ground-based and Airborne Telescopes V, Vol. 9145, SPIE, 842--853

    2014

  101. [110]

    A., & Ford, E

    Rasio, F. A., & Ford, E. B. 1996, Science, 274, 954

    1996

  102. [111]

    N., Armitage , P

    Raymond , S. N., Armitage , P. J., & Gorelick , N. 2010, , 711, 772, 10.1088/0004-637X/711/2/772

    2010 doi

  103. [112]

    N., & Izidoro , A

    Raymond , S. N., & Izidoro , A. 2017, , 297, 134, 10.1016/j.icarus.2017.06.030

    2017 doi

  104. [113]

    2022, The Astronomical Journal, 164, 104

    Rice, M., Wang, S., Wang, X.-Y., et al. 2022, The Astronomical Journal, 164, 104

    2022

  105. [114]

    R., Winn, J

    Ricker, G. R., Winn, J. N., Vanderspek, R., et al. 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003

    2015

  106. [115]

    J., Fulton, B

    Rosenthal, L. J., Fulton, B. J., Hirsch, L. A., et al. 2021, The Astrophysical Journal Supplement Series, 255, 8

    2021

  107. [116]

    Rossiter , R. A. 1924, , 60, 15, 10.1086/142825

    1924 doi

  108. [117]

    S., Lysenko , P

    Safonov , B. S., Lysenko , P. A., & Dodin , A. V. 2017, Astronomy Letters, 43, 344, 10.1134/S1063773717050036

    2017 doi

  109. [118]

    2017, Astronomy & Astrophysics, 603, A30

    Santos, N., Adibekyan, V., Figueira, P., et al. 2017, Astronomy & Astrophysics, 603, A30

    2017

  110. [119]

    J., Finkbeiner , D

    Schlegel , D. J., Finkbeiner , D. P., & Davis , M. 1998, , 500, 525, 10.1086/305772

    1998 doi

  111. [120]

    J., Howell, S

    Scott, N. J., Howell, S. B., Gnilka, C. L., et al. 2021, Frontiers in Astronomy and Space Sciences, 8, 716560

    2021

  112. [121]

    A., Dalba, P

    Sgro, L. A., Dalba, P. A., Esposito, T. M., et al. 2024, The Astronomical Journal, 168, 26

    2024

  113. [122]

    2022, , 663, A4, 10.1051/0004-6361/202142409

    Soubiran , C., Brouillet , N., & Casamiquela , L. 2022, , 663, A4, 10.1051/0004-6361/202142409

    2022 doi

  114. [123]

    Speagle, J. S. 2020, Monthly Notices of the Royal Astronomical Society, 493, 3132

    2020

  115. [124]

    G., Collins , K

    Stassun , K. G., Collins , K. A., & Gaudi , B. S. 2017, , 153, 136, 10.3847/1538-3881/aa5df3

    2017 doi

  116. [125]

    G., Corsaro , E., Pepper , J

    Stassun , K. G., Corsaro , E., Pepper , J. A., & Gaudi , B. S. 2018, , 155, 22, 10.3847/1538-3881/aa998a

    2018 doi

  117. [126]

    G., & Torres , G

    Stassun , K. G., & Torres , G. 2016, , 152, 180, 10.3847/0004-6256/152/6/180

    2016 doi

  118. [127]

    2021, , 907, L33, 10.3847/2041-8213/abdaad

    ---. 2021, , 907, L33, 10.3847/2041-8213/abdaad

    2021 doi

  119. [128]

    G., Oelkers , R

    Stassun , K. G., Oelkers , R. J., Paegert , M., et al. 2019, , 158, 138, 10.3847/1538-3881/ab3467

    2019 doi

  120. [129]

    P., Fortney, J

    Thorngren, D. P., Fortney, J. J., Murray-Clay, R. A., & Lopez, E. D. 2016, The Astrophysical Journal, 831, 64

    2016

  121. [130]

    2018, , 130, 035002, 10.1088/1538-3873/aaa7d9

    Tokovinin , A. 2018, , 130, 035002, 10.1088/1538-3873/aaa7d9

    2018 doi

  122. [131]

    A., Bonati , M., et al

    Tokovinin , A., Fischer , D. A., Bonati , M., et al. 2013, , 125, 1336, 10.1086/674012

    2013 doi

  123. [132]

    2010, , 18, 67, 10.1007/s00159-009-0025-1

    Torres , G., Andersen , J., & Gim \'e nez , A. 2010, , 18, 67, 10.1007/s00159-009-0025-1

    2010 doi

  124. [133]

    H., Cameron, A

    Triaud, A. H., Cameron, A. C., Queloz, D., et al. 2010, Astronomy & Astrophysics, 524, A25

    2010

  125. [134]

    Triaud , A. H. M. J. 2018, in Handbook of Exoplanets, ed. H. J. Deeg & J. A. Belmonte , 2, 10.1007/978-3-319-55333-7_2

    2018 doi

  126. [135]

    D., Catanzarite , J

    Twicken , J. D., Catanzarite , J. H., Clarke , B. D., et al. 2018, , 130, 064502, 10.1088/1538-3873/aab694

    2018 doi

  127. [136]

    Villanueva, S., Dragomir, D., & Gaudi, B. S. 2019, The Astronomical Journal, 157, 84

    2019

  128. [137]

    S., Radovan, M., Kibrick, R., et al

    Vogt, S. S., Radovan, M., Kibrick, R., et al. 2014, Publications of the Astronomical Society of the Pacific, 126, 359

    2014

  129. [138]

    L., Bedard , D., Matthews , J., & Grocott , S

    Wallace , B., Scott , R. L., Bedard , D., Matthews , J., & Grocott , S. 2006, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 6265, Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, ed. J. C. Mather , H. A. MacEwen ...

    2006 doi

  130. [139]

    Ward, W. R. 1997, Icarus, 126, 261

    1997

  131. [140]

    J., West, R

    Wheatley, P. J., West, R. G., Goad, M. R., et al. 2018, Monthly Notices of the Royal Astronomical Society, 475, 4476

    2018

  132. [141]

    Winn, J. N. 2010, Exoplanet transits and occultations, Vol. 55 (University of Arizona Press Tucson)

    2010

  133. [142]

    N., Fabrycky, D., Albrecht, S., & Johnson, J

    Winn, J. N., Fabrycky, D., Albrecht, S., & Johnson, J. A. 2010, The Astrophysical Journal Letters, 718, L145

    2010

  134. [143]

    A., Wang , S., Horner , J., et al

    Wittenmyer , R. A., Wang , S., Horner , J., et al. 2020, , 492, 377, 10.1093/mnras/stz3436

    2020 doi

  135. [144]

    2011, The Astrophysical Journal, 735, 109

    Wu, Y., & Lithwick, Y. 2011, The Astrophysical Journal, 735, 109

    2011

  136. [145]

    2019, , 245, 34, 10.3847/1538-4365/ab5364

    Xiang , M., Ting , Y.-S., Rix , H.-W., et al. 2019, , 245, 34, 10.3847/1538-4365/ab5364

    2019 doi

  137. [146]

    W., Petigura, E

    Yee, S. W., Petigura, E. A., & von Braun , K. 2017, , 836, 77, 10.3847/1538-4357/836/1/77

    2017 doi

  138. [147]

    2023, , 264, 14, 10.3847/1538-4365/ac9dfa

    Zhang , R., & Yuan , H. 2023, , 264, 14, 10.3847/1538-4365/ac9dfa

    2023 doi

  139. [148]

    2020, , 159, 19, 10.3847/1538-3881/ab55e9

    Ziegler , C., Tokovinin , A., Brice \ n o , C., et al. 2020, , 159, 19, 10.3847/1538-3881/ab55e9

    2020 doi

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