pith. sign in

arxiv: 2607.02061 · v1 · pith:WZVHPTIAnew · submitted 2026-07-02 · 🌌 astro-ph.EP

NGTS-39 b: A 58 d transiting warm Jupiter in an eccentric orbit

Ioannis Apergis , Daniel Bayliss , Sol\`ene Ulmer-Moll , Samuel Gill , Toby Rodel , Matthew Battley , Paul Benni , Allyson Bieryla
show 48 more authors
James A. Blake Andrea Bonfanti Fran\c{c}ois Bouchy Edward M. Bryant Matthew R. Burleigh Samuel J. Carlier Sarah L. Casewell Hritam Chakraborty Alastair B. Claringbold Karen A. Collins Benjamin D. R. Davies Xavier Dumusque Troy A. Edkins Fintan Eeles-Nolle Jo Ann Egger Jorge Fern\'andez Fern\'andez Marcelo Aron Fetzner Keniger Pedro Figueira Michael R. Goad George Harvey Faith Hawthorn Melissa J. Hobson Mathilde Houelle Giovanni Isopi Timour Jestin Alicia Kendall Monika Lendl Daniel Lewis Isobel Lockley Franco Mallia James McCormac Morgan A. Mitchell Lucile Mignon Hugh Osborn Angelica Psaridi Alex Romanec Suman Saha Amber Sedgley S\'ergio Sousa Neil Thomas St\'ephane Udry Christopher Watson Richard G. West Thomas G. Wilson Peter J. Wheatley Jamie T. Williams Aldo Zapparata Krzysztof Sz. Zieli\'nski
This is my paper

Pith reviewed 2026-07-03 05:07 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanetstransiting planetswarm Jupiterseccentric orbitsradial velocitiesgas giants
0
0 comments X

The pith

A Jupiter-sized gas giant transits a Sun-like star every 58 days on an eccentric orbit with eccentricity 0.39.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper establishes the existence and detailed properties of a transiting warm Jupiter planet with an orbital period of 58 days. It uses combined transit photometry and radial velocity data to measure the planet's mass of 1.467 Jupiter masses, radius of 1.088 Jupiter radii, and eccentricity of 0.386. This adds an example in the intermediate-period range, which can test models of gas giant formation and migration.

Core claim

NGTS-39 b is a Jupiter-sized gas giant with a radius of 1.088 RJ and a mass of 1.467 MJ that transits a Sun-like star on a 58.2 day eccentric orbit with eccentricity 0.386. Its equilibrium temperature is 519 K. The radial velocity data show a linear trend of -17.75 m s^-1 yr^-1, which indicates the presence of an outer companion.

What carries the argument

The transiting gas giant planet with measured mass, radius, and orbital elements, which serves as the central object for studying warm Jupiters in the long-period regime.

If this is right

  • It provides a test case for formation and migration models of gas giants at intermediate orbital periods.
  • The measured eccentricity constrains possible dynamical histories or interactions with other bodies.
  • The linear trend in radial velocities indicates at least one additional outer companion in the system.
  • The bright host star allows further atmospheric or dynamical follow-up observations.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Similar single-transit events in survey data may be prioritized for radial velocity follow-up to find more such planets.
  • The system could be used to test predictions about how eccentricity correlates with orbital period in gas giants.
  • Detection of the outer companion would create a laboratory for studying planet-planet interactions over long timescales.

Load-bearing premise

The single transit signal, additional photometry, and radial velocity variations all come from the same planetary companion rather than stellar activity or a false positive.

What would settle it

A mismatch between the predicted transit timing from the radial velocity orbit and new photometric observations, or radial velocity data that cannot be fit by the derived orbital parameters.

Figures

Figures reproduced from arXiv: 2607.02061 by Alastair B. Claringbold, Aldo Zapparata, Alex Romanec, Alicia Kendall, Allyson Bieryla, Amber Sedgley, Andrea Bonfanti, Angelica Psaridi, Benjamin D. R. Davies, Christopher Watson, Daniel Bayliss, Daniel Lewis, Edward M. Bryant, Faith Hawthorn, Fintan Eeles-Nolle, Fran\c{c}ois Bouchy, Franco Mallia, George Harvey, Giovanni Isopi, Hritam Chakraborty, Hugh Osborn, Ioannis Apergis, Isobel Lockley, James A. Blake, James McCormac, Jamie T. Williams, Jo Ann Egger, Jorge Fern\'andez Fern\'andez, Karen A. Collins, Krzysztof Sz. Zieli\'nski, Lucile Mignon, Marcelo Aron Fetzner Keniger, Mathilde Houelle, Matthew Battley, Matthew R. Burleigh, Melissa J. Hobson, Michael R. Goad, Monika Lendl, Morgan A. Mitchell, Neil Thomas, Paul Benni, Pedro Figueira, Peter J. Wheatley, Richard G. West, Samuel Gill, Samuel J. Carlier, Sarah L. Casewell, S\'ergio Sousa, Sol\`ene Ulmer-Moll, St\'ephane Udry, Suman Saha, Thomas G. Wilson, Timour Jestin, Toby Rodel, Troy A. Edkins, Xavier Dumusque.

Figure 1
Figure 1. Figure 1: TESS Sector 7 Full-Frame Image cutout (11×11 pixels) of NGTS￾39 and the surrounding region, generated with tpfplotter (Aller et al. 2020). NGTS-39 is shown at the centre, labelled "1" and marked with the white x. The only additional source falling within our adopted aperture is approximately 6 magnitudes fainter than the target, and therefore its flux contribution is expected to be negligible. No significa… view at source ↗
Figure 2
Figure 2. Figure 2: TESS Sector detrended and normalised lightcurves zoomed-in for NGTS-39 from TESS full-frame images pipeline. The transit events are marked with red. Transits are detected in Sector 33 and Sector 87. The transit event in Sector 72 was just missed due to the orbit gap in the TESS data. All the data has been binned to 30-minutes for clarity and consistency [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: NGTS lightcurves from 2023/09/03 to 2024/02/04 for NGTS-39 from the bsproc pipeline, normalised and detrended. The transit event is visible in the lower-right panel and was observed on the night of 2024/01/21. For clarity, all data are binned to 5-minute cadence. resulting in a 17.1 ′ × 17.1 ′ full field of view (Mantovan et al. 2024). An egress event of NGTS-39 b was observed on 2025/10/22 using the 𝑟 ′ f… view at source ↗
Figure 4
Figure 4. Figure 4: Transit lightcurves of NGTS-39 from TESS. Each panel displays the transit data, depicted by square markers with errors. The data is binned to 10-minutes. The transit model is shown with the solid line. The left panel shows the data from TESS Sector 33 centered on BJD=2459225.7606 recorded with 10 minutes cadence and with the TESS filter. The right panel shows the data from TESS Sector 87 centered on BJD=24… view at source ↗
Figure 5
Figure 5. Figure 5: Transit lightcurves of NGTS-39 from NGTS. Each panel displays the transit data, shown as square markers with errors. The data are binned to 10-minutes. The transit model is shown with the solid line. The left panel shows the data from NGTS with 1 telescope unit, with 10 s exposure using the NGTS filter from the observing night of 2024/01/21 centered on BJD=2460331.6503. The right panel shows the data from … view at source ↗
Figure 6
Figure 6. Figure 6: Transit lightcurve of NGTS-39 normalised to the out-of-transit flux levels taken with LCO-CTIO, ULMT, Lookout, Acton Sky Portal, KeplerCam and OACC-CAO on 2025/10/22 centered on BJD=2460971.9023. The best fit model is shown in red. The data are binned to 10-minutes for clarity. The panel shows the six individual light curves, each vertically offset for clarity. RV signal rather than evidence for an indepen… view at source ↗
Figure 7
Figure 7. Figure 7: RV measurements of NGTS-39. CORALIE data from the first (CORALIE14) and second (CORALIE24) observing cycles are shown as yellow triangles and green squares, respectively, while HARPS measurements are represented by blue circles. The solid line indicates the best-fit RV model. The left panel presents the radial velocities over time along with the residuals from the fit, and the right panel shows the phase-f… view at source ↗
Figure 8
Figure 8. Figure 8: O-C diagram for transit NGTS-39 b using TESS data of Sector 33 and 87 (epochs -15 and 10 respectively), NGTS monitoring (epoch 4) and follow-up data from NGTS and the SG1 network (epoch 15). The mean value of the linear model is shown as a red dashed line and the 1-𝜎 RMS with the red shaded area. close-in, large- radius companions, they do not exclude lower-radius planets or giant companions on wider orbit… view at source ↗
Figure 11
Figure 11. Figure 11: Stellar effective temperature, Teff, is plotted against planetary equilibrium temperature, 𝑇eq. NGTS-39 b is highlighted as a star marker with a black outline and is colour-coded by its orbital eccentricity, consistent with the rest of the planetary sample. The horizontal dashed lines at 850 K and 500 K mark the expected CO–CH4 and N2–NH3 chemical transition boundaries, respectively, for a 1 MJ planet (Fo… view at source ↗
Figure 10
Figure 10. Figure 10: Population diagrams showing planetary radius (top) and orbital eccentricity (bottom) as a function of orbital period for exoplanets with period > 10 days and radius > 0.5 𝑅Jup. NGTS-39 b is highlighted as a star marker with a black outline and is colour-coded by its mass, consistent with the rest of the planetary sample. We note, however, that the N2-NH3 transition reported by Fortney et al. (2020) is cal… view at source ↗
read the original abstract

We report the discovery and characterisation of NGTS-39 b (TIC 453147896 b), a warm Jupiter transiting a Sun-like star on a 58.2 day, eccentric (e = 0.386 +/- 0.019) orbit. NGTS-39 b was first identified from a TESS single-transit event, and subsequently confirmed with NGTS photometry and radial-velocity measurements from CORALIE and HARPS. The host star is a bright (Tmag = 11.02) F9 dwarf with an effective temperature of Teff = 6053 +67/-30 K. NGTS-39 b is a Jupiter-sized gas giant with a radius of 1.088 +/- 0.012 RJ and a mass of 1.467 +/- 0.081 MJ. Its equilibrium temperature is 519 +6/-5 K, placing it between short-period hot Jupiters and cold, Jupiter-like giants. The high orbital eccentricity and intermediate equilibrium temperature of NGTS-39 b make it a valuable test case for formation and migration models, particularly in the poorly sampled regime of long-period gas giants. The RV data show a linear trend of gamma dot = -17.75 m s^-1 yr^-1, which indicates the presence of an outer companion. The discovery of NGTS-39 b contributes to the small but growing population of transiting warm Jupiters with P > 50 days orbiting bright stars.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The manuscript reports the discovery and characterization of NGTS-39 b, a warm Jupiter transiting a bright F9 dwarf (Tmag=11.02, Teff=6053+67/-30 K) on a 58.2-day eccentric (e=0.386±0.019) orbit. The planet was identified from a single TESS transit and confirmed with NGTS photometry plus CORALIE and HARPS radial velocities, yielding Rp=1.088±0.012 RJ, Mp=1.467±0.081 MJ, and Teq=519+6/-5 K. The RV data also show a linear trend (γ̇=-17.75 m s⁻¹ yr⁻¹) indicating an outer companion. The result is presented as adding to the population of long-period transiting gas giants around bright stars.

Significance. If robust, the detection supplies a rare, precisely characterized warm Jupiter in the P>50 d regime around a bright star, offering a test case for formation and migration models in a sparsely sampled period range. The combination of measured eccentricity and outer-companion trend adds dynamical interest beyond a simple period-radius-mass addition to the census.

major comments (2)
  1. [Analysis / confirmation section (likely §3–4)] The central claim that the TESS transit, NGTS photometry, and CORALIE/HARPS RVs arise from the same planetary companion requires explicit false-positive vetting (e.g., centroid motion, blend scenarios, activity indicators). No such section or quantitative assessment is described in the provided material, leaving the weakest assumption unaddressed and preventing full evaluation of the discovery.
  2. [§3 (Transit and RV analysis)] Transit and RV modeling details are absent: the abstract quotes final parameters and uncertainties but provides no information on data reduction pipelines, choice of transit model (e.g., Mandel–Agol vs. others, limb-darkening treatment), eccentricity priors, or joint fitting procedure. These choices directly affect the quoted Rp, Mp, and e values and must be documented for reproducibility.
minor comments (1)
  1. [Abstract / planet properties paragraph] The equilibrium temperature is reported with asymmetric uncertainties but the assumed Bond albedo and heat redistribution factor are not stated; this should be added for clarity even if standard values are used.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive report and positive assessment of the scientific value of NGTS-39 b. We agree that the two major comments identify areas where the manuscript can be strengthened for clarity and reproducibility. We address each point below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: The central claim that the TESS transit, NGTS photometry, and CORALIE/HARPS RVs arise from the same planetary companion requires explicit false-positive vetting (e.g., centroid motion, blend scenarios, activity indicators). No such section or quantitative assessment is described in the provided material, leaving the weakest assumption unaddressed and preventing full evaluation of the discovery.

    Authors: We acknowledge that a dedicated false-positive vetting section was not present in the submitted manuscript. In the revised version we will add a new subsection (likely in §3 or §4) that quantitatively addresses this. It will include: (i) TESS centroid motion analysis to check for shifts during transit; (ii) assessment of possible blend scenarios using available high-resolution imaging or archival data; and (iii) checks on activity indicators (e.g., BIS, FWHM, log R'HK from CORALIE/HARPS and photometric variability from NGTS/TESS) to rule out stellar activity or false positives. These additions will directly support the planetary interpretation. revision: yes

  2. Referee: Transit and RV modeling details are absent: the abstract quotes final parameters and uncertainties but provides no information on data reduction pipelines, choice of transit model (e.g., Mandel–Agol vs. others, limb-darkening treatment), eccentricity priors, or joint fitting procedure. These choices directly affect the quoted Rp, Mp, and e values and must be documented for reproducibility.

    Authors: We agree that the modeling and data-reduction procedures require explicit documentation. The revised manuscript will expand the relevant analysis section to describe: the TESS, NGTS, CORALIE and HARPS data-reduction pipelines; the transit model (Mandel–Agol with quadratic limb darkening, specifying how coefficients were handled); the eccentricity priors and other parameter priors; and the joint transit+RV fitting procedure (including the software package and any additional constraints such as the linear trend). This will allow full reproduction of the reported Rp, Mp and e values. revision: yes

Circularity Check

0 steps flagged

No significant circularity identified

full rationale

The paper is a standard observational discovery and characterization of an exoplanet. Orbital elements, mass, and radius are obtained by direct fitting of transit photometry (TESS + NGTS) and radial-velocity data (CORALIE + HARPS) to a Keplerian model; no derivation chain reduces any claimed result to its own inputs by construction, no self-citation is load-bearing for the existence or parameters of the planet, and no ansatz or uniqueness theorem is invoked. The central claim therefore remains self-contained against the external data.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The discovery rests on standard domain assumptions in exoplanet confirmation rather than new postulates or fitted constants beyond the usual orbital elements.

axioms (2)
  • domain assumption The photometric and spectroscopic signals are produced by a single transiting planet on a Keplerian orbit
    Invoked to combine TESS, NGTS and RV data into a single solution
  • domain assumption Stellar parameters derived from spectroscopy accurately reflect the host star's mass and radius
    Required to convert observed transit depth and RV amplitude into physical planet radius and mass

pith-pipeline@v0.9.1-grok · 6086 in / 1156 out tokens · 42249 ms · 2026-07-03T05:07:58.023363+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

299 extracted references · 190 canonical work pages · 12 internal anchors

  1. [1]

    Nominal thresholds for good astrometric fits, and prospects for binary detectability, for the full extended Gaia mission

    Nominal thresholds for good astrometric fits, and prospects for binary detectability, for the full extended Gaia mission. , keywords =. doi:10.1093/mnras/stag654 , archivePrefix =. 2511.02476 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stag654

  2. [2]

    , keywords =

    Gaia DR3 detectability of unresolved binary systems. , keywords =. doi:10.1051/0004-6361/202450172 , archivePrefix =. 2404.14127 , primaryClass =

    work page doi:10.1051/0004-6361/202450172

  3. [3]

    , keywords =

    A comprehensive study on radial velocity signals using ESPRESSO: Pushing precision to the 10 cm/s level. , keywords =. doi:10.1051/0004-6361/202553869 , archivePrefix =. 2507.07514 , primaryClass =

    work page doi:10.1051/0004-6361/202553869

  4. [5]

    New planetary systems around HD 87816, HD 94890, and HD 102888 and an update on HD 121056

    CORALIE radial-velocity search for companions around evolved stars (CASCADES): IV. New planetary systems around HD 87816, HD 94890, and HD 102888 and an update on HD 121056. , keywords =. doi:10.1051/0004-6361/202554137 , archivePrefix =. 2505.14317 , primaryClass =

    work page doi:10.1051/0004-6361/202554137

  5. [6]

    The CORALIE survey for southern extrasolar planets. XVI. Discovery of a planetary system around HD 147018 and of two long period and massive planets orbiting HD 171238 and HD 204313. , keywords =. doi:10.1051/0004-6361/200912136 , archivePrefix =. 0908.1479 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200912136

  6. [7]

    MNRAS , month = nov, number =

    Parviainen, Hannu and Aigrain, Suzanne , doi =. MNRAS , month = nov, number =

  7. [8]

    Analytical Chemistry , year = 1964, month = jan, volume =

    Smoothing and differentiation of data by simplified least squares procedures. Analytical Chemistry , year = 1964, month = jan, volume =. doi:10.1021/ac60214a047 , adsurl =

    work page doi:10.1021/ac60214a047 1964

  8. [9]

    Research Notes of the American Astronomical Society , keywords =

    TESS Science Processing Operations Center FFI Target List Products. Research Notes of the American Astronomical Society , keywords =. doi:10.3847/2515-5172/abc9b3 , archivePrefix =. 2011.05495 , primaryClass =

    work page doi:10.3847/2515-5172/abc9b3 2011

  9. [10]

    The CORALIE survey for southern extrasolar planets. XVIII. Three new massive planets and two low-mass brown dwarfs at greater than 5 AU separation. , keywords =. doi:10.1051/0004-6361/201935356 , archivePrefix =. 1904.01573 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201935356 1904

  10. [11]

    Lightkurve: Kepler and TESS time series analysis in Python

  11. [12]

    , volume = 167, number = 5, pages = 238, doi =

  12. [13]

    doi:10.1093/mnras/stx2836 , keywords =

    , volume = 475, number = 4, pages =. doi:10.1093/mnras/stx2836 , keywords =

    work page doi:10.1093/mnras/stx2836

  13. [14]

    doi:10.1038/378355a0 , adsurl =

    , volume = 378, number = 6555, pages =. doi:10.1038/378355a0 , adsurl =

    work page doi:10.1038/378355a0

  14. [15]

    Exoplanets , publisher =

  15. [16]

    doi:10.1051/0004-6361:20020802 , keywords =

    , volume = 391, pages =. doi:10.1051/0004-6361:20020802 , keywords =

    work page doi:10.1051/0004-6361:20020802

  16. [17]

    , volume = 210, number = 2, pages = 19, doi =

  17. [18]

    , volume = 254, number = 2, pages = 39, doi =

  18. [19]

    arXiv e-prints , pages =

  19. [20]

    , volume = 754, number = 2, pages = 129, doi =

  20. [21]

    , volume = 155, number = 2, pages = 57, doi =

  21. [22]

    , keywords =

    The NASA Exoplanet Archive and Exoplanet Follow-up Observing Program: Data, Tools, and Usage. , keywords =. doi:10.3847/PSJ/ade3c2 , archivePrefix =. 2506.03299 , primaryClass =

    work page doi:10.3847/psj/ade3c2

  22. [23]

    arXiv e-prints , keywords =

    An upgraded 0.4-meter telescope fleet for Las Cumbres Observatory's Educational and Science Programs. arXiv e-prints , keywords =. doi:10.48550/arXiv.2405.10408 , archivePrefix =. 2405.10408 , primaryClass =

    work page doi:10.48550/arxiv.2405.10408

  23. [24]

    Real-time processing of the imaging data from the network of Las Cumbres Observatory Telescopes using BANZAI

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1117/12.2314340 2018

  24. [25]

    doi:10.1111/j.1365-2966.2008.13689.x , keywords =

    , volume = 389, number = 3, pages =. doi:10.1111/j.1365-2966.2008.13689.x , keywords =

    work page doi:10.1111/j.1365-2966.2008.13689.x 2008

  25. [26]

    doi:10.1093/mnras/staa3739 , keywords =

    , volume = 501, number = 4, pages =. doi:10.1093/mnras/staa3739 , keywords =

    work page doi:10.1093/mnras/staa3739

  26. [27]

    , keywords =

    , volume = 419, number = 4, pages =. doi:10.1111/j.1365-2966.2011.19932.x , keywords =

    work page doi:10.1111/j.1365-2966.2011.19932.x 2011

  27. [28]

    Scientific Data , volume = 5, pages = 180124, doi =

    Time-lapse imagery and volunteer classifications from the Zooniverse Penguin Watch project , author =. Scientific Data , volume = 5, pages = 180124, doi =

  28. [29]

    doi:10.3847/2041-8213/aa7200 , keywords =

    , volume = 841, number = 2, pages =. doi:10.3847/2041-8213/aa7200 , keywords =

    work page doi:10.3847/2041-8213/aa7200 2041

  29. [30]

    doi:10.1016/j.icarus.2018.08.018 , keywords =

    , volume = 319, pages =. doi:10.1016/j.icarus.2018.08.018 , keywords =

    work page doi:10.1016/j.icarus.2018.08.018 2018

  30. [31]

    doi:10.31219/osf.io/z6exv , url =

    Describing vocalizations in young children: A big data approach through citizen science annotation , author =. doi:10.31219/osf.io/z6exv , url =

    work page doi:10.31219/osf.io/z6exv

  31. [32]

    Traffic , publisher =

    Deep learning for automatic segmentation of the nuclear envelope in electron microscopy data, trained with volunteer segmentations , author =. Traffic , publisher =. doi:10.1111/tra.12789 , issn =

    work page doi:10.1111/tra.12789

  32. [33]

    doi:10.46298/jdmdh.5759 , url =

    Blickhan, Samantha and Krawczyk, Coleman and Hanson, Daniel and Boyer, Amy and Simenstad, Andrea and Hyning, Victoria Van and Van Hyning, Victoria , year = 2019, month = Dec, journal =. doi:10.46298/jdmdh.5759 , url =

    work page doi:10.46298/jdmdh.5759 2019

  33. [34]

    , volume = 125, number = 930, pages = 989, doi =

  34. [35]

    Nature Astronomy , doi =

  35. [36]

    , keywords =

    , volume = 410, number = 1, pages =. doi:10.1111/j.1365-2966.2010.17432.x , keywords =

    work page doi:10.1111/j.1365-2966.2010.17432.x 2010

  36. [37]

    Advances in Machine Learning and Data Mining for Astronomy , publisher =

  37. [38]

    and Valenti, S

    , volume = 399, number = 1, pages =. doi:10.1111/j.1365-2966.2009.15299.x , keywords =

    work page doi:10.1111/j.1365-2966.2009.15299.x 2009

  38. [39]

    and Valenti, S

    , volume = 399, number = 3, pages =. doi:10.1111/j.1365-2966.2009.15383.x , keywords =

    work page doi:10.1111/j.1365-2966.2009.15383.x 2009

  39. [40]

    doi:10.1038/s41586-020-2421-7 , keywords =

    , volume = 583, number = 7814, pages =. doi:10.1038/s41586-020-2421-7 , keywords =

    work page doi:10.1038/s41586-020-2421-7

  40. [41]

    doi:10.1051/0004-6361/201527329 , keywords =

    , volume = 587, pages =. doi:10.1051/0004-6361/201527329 , keywords =

    work page doi:10.1051/0004-6361/201527329

  41. [42]

    doi:10.1111/j.1365-2966.2006.11074.x , keywords =

    , volume = 373, number = 2, pages =. doi:10.1111/j.1365-2966.2006.11074.x , keywords =

    work page doi:10.1111/j.1365-2966.2006.11074.x 2006

  42. [43]

    Science , volume = 327, number = 5968, pages = 977, doi =

  43. [44]

    doi:10.1117/1.JATIS.1.1.014003 , eid =

    Journal of Astronomical Telescopes, Instruments, and Systems , volume = 1, pages =. doi:10.1117/1.JATIS.1.1.014003 , eid =

    work page internal anchor Pith review doi:10.1117/1.jatis.1.1.014003

  44. [45]

    doi:10.1086/521346 , keywords =

    , volume = 669, number = 2, pages =. doi:10.1086/521346 , keywords =

    work page doi:10.1086/521346

  45. [46]

    , volume = 819, number = 2, pages = 127, doi =

  46. [47]

    The Deuterium-Burning Mass Limit for Brown Dwarfs and Giant Planets

    The Deuterium-burning Mass Limit for Brown Dwarfs and Giant Planets. , keywords =. doi:10.1088/0004-637X/727/1/57 , archivePrefix =. 1008.5150 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/727/1/57

  47. [48]

    doi:10.1073/pnas.1304206111 , keywords =

    Proceedings of the National Academy of Science , volume = 111, number = 35, pages =. doi:10.1073/pnas.1304206111 , keywords =

    work page doi:10.1073/pnas.1304206111

  48. [49]

    , volume = 59, doi =

  49. [50]

    The Optical Gravitational Lensing Experiment. Search for Planetary and Low-Luminosity Object Transits in the Galactic Disk. Results of 2001 Campaign

    , volume = 52, pages =. doi:10.48550/arXiv.astro-ph/0202320 , keywords =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0202320

  50. [51]

    doi:10.1086/429127 , keywords =

    , volume = 624, number = 1, pages =. doi:10.1086/429127 , keywords =

    work page doi:10.1086/429127

  51. [52]

    doi:10.1086/509874 , keywords =

    , volume = 656, number = 1, pages =. doi:10.1086/509874 , keywords =

    work page doi:10.1086/509874

  52. [53]

    doi:10.1051/0004-6361/201834853 , keywords =

    , volume = 623, pages =. doi:10.1051/0004-6361/201834853 , keywords =

    work page doi:10.1051/0004-6361/201834853

  53. [54]

    doi:10.1086/508556 , keywords =

    , volume = 118, number = 848, pages =. doi:10.1086/508556 , keywords =

    work page doi:10.1086/508556

  54. [55]

    Transiting Extrapolar Planets Workshop , series =

  55. [56]

    , keywords =

    , volume = 356, number = 4, pages =. doi:10.1111/j.1365-2966.2004.08585.x , keywords =

    work page doi:10.1111/j.1365-2966.2004.08585.x 2004

  56. [57]

    doi:10.1016/0019-1035(84)90102-7 , keywords =

    , volume = 58, number = 1, pages =. doi:10.1016/0019-1035(84)90102-7 , keywords =

    work page doi:10.1016/0019-1035(84)90102-7

  57. [58]

    doi:10.1086/382735 , keywords =

    , volume = 116, number = 817, pages =. doi:10.1086/382735 , keywords =

    work page doi:10.1086/382735

  58. [59]

    , volume = 222, number = 1, pages = 14, doi =

  59. [60]

    , volume = 126, number = 938, pages = 398, doi =

  60. [61]

    Next Generation Transit Survey Data Release Document , author =

  61. [62]

    Next Generation Transit Survey Second Data Release Document , author =

  62. [63]

    doi:10.1093/mnras/stz2064 , keywords =

    , volume = 488, number = 4, pages =. doi:10.1093/mnras/stz2064 , keywords =

    work page doi:10.1093/mnras/stz2064

  63. [64]

    , volume = 156, number = 5, pages = 234, doi =

  64. [65]

    , volume = 155, number = 3, pages = 136, doi =

  65. [66]

    doi:10.1146/annurev-astro-081811-125523 , keywords =

    , volume = 50, pages =. doi:10.1146/annurev-astro-081811-125523 , keywords =

    work page doi:10.1146/annurev-astro-081811-125523

  66. [67]

    , volume = 822, number = 2, pages = 86, doi =

  67. [68]

    , volume = 158, number = 4, pages = 138, doi =

  68. [69]

    doi:10.48550/arXiv.2108.04778 , keywords =

    arXiv e-prints , pages =. doi:10.48550/arXiv.2108.04778 , keywords =

    work page doi:10.48550/arxiv.2108.04778

  69. [70]

    doi:10.17909/FWDT-2X66 , url =

    TESS Input Catalog and Candidate Target List , author =. doi:10.17909/FWDT-2X66 , url =

    work page doi:10.17909/fwdt-2x66

  70. [71]

    , volume = 809, number = 1, pages = 25, doi =

  71. [72]

    , volume = 162, number = 2, pages = 75, doi =

  72. [73]

    , volume = 805, number = 1, pages = 16, doi =

  73. [74]

    doi:10.1086/309530 , keywords =

    , volume = 542, number = 1, pages =. doi:10.1086/309530 , keywords =

    work page doi:10.1086/309530

  74. [75]

    J. Sci. Commun. , volume = 18, number = 1, pages =. doi:10.22323/2.18010204 , url =

    work page doi:10.22323/2.18010204

  75. [76]

    doi:10.1093/mnras/stx2778 , keywords =

    , volume = 475, number = 4, pages =. doi:10.1093/mnras/stx2778 , keywords =

    work page doi:10.1093/mnras/stx2778

  76. [77]

    doi:10.1093/mnras/sty2581 , keywords =

    , volume = 481, number = 4, pages =. doi:10.1093/mnras/sty2581 , keywords =

    work page doi:10.1093/mnras/sty2581

  77. [78]

    doi:10.1093/mnras/sty1193 , keywords =

    , volume = 478, number = 4, pages =. doi:10.1093/mnras/sty1193 , keywords =

    work page doi:10.1093/mnras/sty1193

  78. [79]

    doi:10.1093/mnras/stz1084 , keywords =

    , volume = 486, number = 4, pages =. doi:10.1093/mnras/stz1084 , keywords =

    work page doi:10.1093/mnras/stz1084

  79. [80]

    doi:10.1051/0004-6361/201935206 , keywords =

    , volume = 625, pages =. doi:10.1051/0004-6361/201935206 , keywords =

    work page doi:10.1051/0004-6361/201935206

  80. [81]

    doi:10.1093/mnras/stz2349 , keywords =

    , volume = 489, number = 3, pages =. doi:10.1093/mnras/stz2349 , keywords =

    work page doi:10.1093/mnras/stz2349

Showing first 80 references.