Pith. sign in

REVIEW 4 major objections 4 minor 117 references

A Pair of Warm Saturn-mass Planets near the 2:1 Mean Motion Resonance around TOI-3850

T0 review · 4 major / 4 minor · reviewed 2026-08-15 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read TOI-3850 hosts two giant planets: a transiting warm Jupiter and a hidden Saturn-mass companion just wide of the 2:1 resonance.

desk verdict Two-planet detection is likely real and the paper is careful, but the headline masses and near-circular orbits are prior-influenced; needs robustness checks before I would quote them. read the letter →

arxiv 2608.11328 v1 pith:ESH6PCNC submitted 2026-08-11 astro-ph.EP

Sean Collins , Michelle Kunimoto , Nicolas B. Cowan , Keivan G. Stassun , Jack J. Lissauer , Ze'ev Vladimir , Teo Močnik , Ernesto Elenter
show 19 more authors
David W. Latham Karen A. Collins Jacob Bean Stephanie Striegel Khalid Barkaoui Ritvik Basant Tanya Das Raquel Forés-Toribio Akihiko Fukui Jose A. Muñoz Felipe Murgas Enric Palle Ivan A. Strakhov Richard P. Schwarz Avi Shporer Gregor Srdoc Chris Stockdale Neil B. Thomas Francis P. Wilkin
This is my paper · ORCID
classification astro-ph.EP
keywords exoplanetsystemswarmJupiterstransittimingvariationsmeanmotionresonanceradialvelocitySaturn-massplanetsplanetarymigrationTOI-3850
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

TOI-3850, a G0 dwarf observed by TESS in five sectors, showed a single transiting planet candidate whose arrival times wobbled by about an hour on a 513-day cycle. The paper argues that this wobble, combined with radial velocities from MAROON-X, requires a second planet: a transiting warm Jupiter, TOI-3850 b (period 14.484 days, mass $112\pm20\,M_\oplus$, radius $12.07\pm0.09\,R_\oplus$), and a non-transiting Saturn-mass companion, TOI-3850 c (period 29.85 days, mass $90\pm15\,M_\oplus$), on near-circular, nearly coplanar orbits just wide of the 2:1 mean motion resonance. If the interpretation is right, the system is one of only about eleven known compact two-giant architectures, and its location just outside resonance supports a formation history dominated by disk-driven migration rather than high-eccentricity migration. The same joint fit yields both masses as true dynamical masses rather than minimum masses, and N-body integrations predict that TOI-3850 c may begin transiting within roughly three decades.

What carries the argument

The central mechanism is the transit timing variation signal: the measured deviations of the inner planet's mid-transit times from a constant ephemeris, with an amplitude of about one hour and a super-period of 513 days. That super-period is the signature of a nearby companion near a first-order mean motion resonance, and it fixes the possible period branches through the relation $P_{\rm super}=|J/P_{\rm outer}-(J-1)/P_{\rm inner}|^{-1}$. The paper then fits the radial-velocity and TTV data simultaneously in a single N-body dynamical model, with the outer planet restricted to a non-transiting geometry. The joint fit is the load-bearing inference: it converts an observed timing wobble into the companion's mass and orbit.

What would settle it

Retake MAROON-X radial velocities at the phase of the excluded 5-sigma outlier (the epoch near BJD 2461103.95); if a velocity of similar magnitude repeats, the two-Saturn dynamical solution and the quoted masses are not uniquely supported.

Watch

Extended reading notes

Core claim

Working from TESS photometry, ground-based transit light curves, MAROON-X radial velocities, and transit timing variations, the paper identifies two giant planets around TOI-3850. The transiting inner planet has period $P_b=14.484$ days, radius $R_b=12.07\,R_\oplus$, and mass $M_b=112\pm20\,M_\oplus$; the unseen outer planet has period $P_c=29.85$ days and mass $M_c=90\pm15\,M_\oplus$, with eccentricity below 0.015 and a mutual inclination of about $4.6^\circ$ relative to the inner planet. The period ratio $P_c/P_b\approx2.06$ places the system just wide of the 2:1 mean motion resonance, and resonant-angle integrations indicate the planets are likely near, but not locked in, exact resonance. Because the joint RV+TTV fit constrains the outer planet's inclination, the paper concludes that both reported masses are dynamical masses, not minimum masses. Roughly half of the posterior samples have the outer planet reaching a transiting geometry within about 27 years.

Load-bearing premise

The result stands on the assumption that the one MAROON-X measurement flagged as a 5-$\sigma$ outlier is not real, and that the prior forcing the outer planet to be non-transiting (inclination $70^\circ<i<90^\circ$, impact parameter $b>1$) is not doing work the data cannot; if either is wrong, the claimed companion mass and the statement that both masses are true dynamical masses would no longer follow.

Editorial extensions

If this is right

  • The system becomes a rare benchmark: among more than 6000 confirmed exoplanets, only eleven systems are known with multiple giant planets inside 0.2 AU.
  • Both planets' masses are stated as true masses; for TOI-3850 c, the joint RV+TTV fit removes the usual $\sin i$ ambiguity, a step that works because the geometry is nearly coplanar.
  • The just-wide-of-resonance, low-eccentricity architecture is evidence for disk-driven migration and against high-eccentricity migration, providing a direct test for formation models.
  • About half of the posterior configurations predict that TOI-3850 c will reach a transiting geometry within about 27 years, so the hidden planet could become measurable from its transits.
  • TOI-3850 b has a transmission spectroscopy metric higher than 87% of warm Jupiters, making it a strong near-term target for atmospheric follow-up.

Reading between the lines

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

  • If the future-transit prediction holds, the system offers a rare natural experiment: the same two planets can be observed both as a TTV/RV pair and later as a double-transit system, so the mutual inclination and resonant state could be measured independently.
  • The stability of the reported masses could be tested immediately by taking more radial velocities at the phase of the one excluded 5-sigma observation; a repeating signal there would break the two-Saturn solution.
  • The super-period branch-selection method used here could be applied to other single-candidate systems with large TTVs, potentially turning lone-transiting-planet surveys into a population census of unseen companion architectures.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 4 minor

Summary. The paper reports the discovery of a compact two-planet system around the G0 dwarf TOI-3850, based on TESS photometry, ground-based transit follow-up, MAROON-X radial velocities, and TTV analysis. The authors identify a transiting warm Jupiter, TOI-3850 b (P_b = 14.484 days, M_b = 112 ± 20 M_Earth, R_b = 12.07 ± 0.09 R_Earth), and a non-transiting Saturn-mass companion, TOI-3850 c (P_c = 29.85 days, M_c = 90 ± 15 M_Earth, e_c < 0.015), on near-circular, nearly coplanar orbits just wide of the 2:1 mean motion resonance. The central claim is that the TTV and RV data jointly require the second planet and that both masses are true dynamical masses. The paper also presents dynamical stability tests, a prediction that TOI-3850 c may begin transiting on decadal timescales, and an assessment of the system's formation history and follow-up potential.

Significance. If correct, this is a valuable addition to a small sample of compact multi-giant-planet systems near a first-order resonance, and it provides a rare case where a non-transiting companion's mass is claimed to be dynamically determined rather than only an M_p sin i lower limit. The paper is thorough in its data collection and modeling: it uses five TESS sectors, extensive ground-based photometry, speckle imaging, MAROON-X RVs, and a joint RV+TTV fit with publicly available tools. The authors provide full prior tables, model comparison tables, convergence checks (R-hat < 1.01, emcee chains longer than 50 autocorrelation times), SPOCK stability classifications, and direct N-body integrations. The two-planet interpretation is independently supported by the large TTV amplitude and super-period and by the RV model comparison favoring a two-planet solution over a one-planet solution. The main weaknesses are that the reported masses and near-circular architecture rest on specific priors and on the exclusion of one RV point, with no sensitivity analysis demonstrating that the conclusions are robust to those choices.

major comments (4)
  1. [§4.3, Table A4] The Gaussian priors on (h,k) = (sqrt(e) cos(omega), sqrt(e) sin(omega)) with standard deviation 0.1 restrict eccentricities to roughly e < 0.06 at 95% confidence, so the reported e_b = 0.018 ± 0.008 and e_c < 0.015 may be prior-dominated rather than measured. Because the TTV signal near the 2:1 commensurability can trade mass against eccentricity, the reported M_c = 90 ± 15 M_Earth and the 'near-circular' architecture are not demonstrated to be robust to this choice. I request a sensitivity test with broader priors (for example, uniform in e up to 0.3, or N(0,0.3) on the eccentricity components) and a report of how the posterior masses and eccentricities shift.
  2. [§2.4.2] A single MAROON-X spectrum is excluded because it lies 5-sigma from the posterior solution, but no fit that includes this point is presented. With only 14 RVs and a companion semi-amplitude K_c = 17.5 ± 2.9 m/s, the outlier could plausibly influence K_b and K_c. Please provide a joint RV+TTV fit that includes the excluded point, or at least quantify the change in the fitted parameters and BIC when it is included, and describe an a priori criterion for outlier rejection rather than a post-hoc one.
  3. [§4.3, Table A4] The companion inclination is constrained by the prior U(70,90) and the hard cut b > 1, rather than by a fit that marginalizes over the full allowed parameter space. Although the reported i_c = 87.18 ± 1.29 deg lies inside the prior, the paper shows no test of whether the TTV data alone constrain this angle; without such a test, the statement at the end of §4.3 that both masses are 'true dynamical masses rather than the usual RV minimum mass' is not supported. A fit with a broader inclination prior (or a prior derived from the non-transit constraint) should be reported.
  4. [§4.2, Table A3] The choice of the wide-of-resonance exterior 2:1 branch over the shortward branch is based on a BIC difference of only 1.7 in the RV-only comparison, which is not statistically significant. The subsequent joint RV+TTV fit assumes this branch without re-testing the branch assignment. Since the system's location wide of the 2:1 MMR is a central claim, the joint fit should either compare the two branches or demonstrate that the TTV phases break the degeneracy.
minor comments (4)
  1. [Title, §1] The phrase 'W arm Saturn-mass Planets' in the title and in the first line of the draft appears to be a typo for 'Warm Saturn-mass Planets'.
  2. [Table A3] The BIC values in Table A3 are not accompanied by the number of free parameters or the number of data points for each model; adding these would allow readers to verify the quoted BIC values and assess the model comparison.
  3. [§4.2] The RV-only model comparison uses Gaussian priors on the companion period that are seeded by the TTV super-period; the text should state more explicitly that the detection of a second Keplerian signal is nonetheless independent of the TTV amplitude, since the one-planet versus two-planet comparison does not use the TTV data directly.
  4. [§5.2.2] The prediction that '50% of samples reach a transiting geometry for TOI-3850 c within the next ~27 years' should be accompanied by a statement of how the assumed inclination prior affects this fraction, since the U(70,90) prior with b > 1 shapes the distribution of first transit epochs.

Circularity Check

1 steps flagged · score 2.0 of 10

Derivation chain is self-contained; only mild self-referential RV outlier rejection.

  1. other [Section 2.4.2 (MAROON-X) and Section 4.3 (Joint RV+TTV Fit)]
    "We excluded one observation from the RV analysis since it was a significant outlier relative to the remaining measurements and lies 5σ away from the posterior median solution presented in §4.3."

    The posterior median solution used to judge the outlier is itself computed from the fit to the 13 retained RVs, so the 5σ distance is measured against a model built without the excluded point. The exclusion criterion is therefore partly self-referential: any point strongly disfavored by the retained-RV model will, by construction, lie far from that model. This is a data-selection loop rather than an independent outlier test, and it could shift K_b and K_c. It is disclosed by the authors and is not load-bearing for the existence of the second planet, which is independently supported by the large TTVs and by the two-Keplerian RV fit to the retained data.

full rationale

The paper is an observational measurement, not a claimed first-principles derivation, and its central claim—that TOI-3850 hosts two giant planets—does not reduce to its inputs. The TTV super-period and Equations (1)-(2) are used to set period priors for the RV-only model comparison, but the RV data are independent of the TTVs, and the preferred 2:1 exterior-wide architecture is selected by BIC rather than imposed by the prior. The joint TTV+RV fit then estimates all orbital and mass parameters from the data, with the eccentricity and inclination priors stated explicitly in Table A4; a tight prior on (h,k) may influence the reported near-zero eccentricities and deserves a sensitivity check, but this is a modeling assumption, not a circular reduction. The system's near-coplanarity is supported by a general empirical citation (Lissauer et al. 2011) that is contextual rather than load-bearing, and no self-citation is used to forbid alternative architectures or to supply a uniqueness theorem. The only flagged circular-adjacent element is the exclusion of one MAROON-X point based on the posterior of the fit that already excludes it; this is a disclosed data-selection loop and could modestly affect the RV semi-amplitudes, but the discovery of the non-transiting companion and the broad mass range are robust to it. Overall, the derivation is self-contained, with one minor self-referential step that does not drive the central result.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

No new physical entities are introduced; the planets are the measured result. The claims rest on standard orbital mechanics plus a set of priors and data-selection choices, the most consequential being the companion inclination prior and the RV outlier exclusion.

free parameters (4)
  • Companion inclination prior range = U(70,90) deg; posterior i_c=87.18±1.29 deg
    The non-transiting companion's inclination is only weakly constrained; the posterior and hence the true dynamical mass claim depend on this prior and the b>1 visibility constraint (Table A4).
  • Eccentricity vector prior width = N(0,0.1) on sqrt(e)cos(omega) and sqrt(e)sin(omega)
    Imposed to mitigate the TTV mass-eccentricity degeneracy; it drives the low eccentricities (e_c<0.015) central to the near-circular architecture claim.
  • MAROON-X jitter = 23.6±6.6 m/s
    Fitted RV jitter added in quadrature; comparable in size to the two Keplerian semi-amplitudes, so the RV mass measurements are sensitive to this term.
  • RV outlier exclusion threshold = One point at BJD 2461103.95 excluded
    The excluded spectrum has RV_red=109 m/s and RV_blue=129 m/s; the decision to exclude it is based on its 5-sigma distance from the posterior solution, affecting the RV fit.
assumptions (5)
  • standard math TTV super-period formula relating period ratio to super-period for first-order MMR (Equations 1-2)
    Used to set Gaussian priors on the companion period; standard TTV theory from Hadden and Lithwick 2016.
  • domain assumption System is nearly coplanar, with companion inclination in U(70,90) and b>1
    The joint fit assumes coplanarity as commonly observed and enforces a non-transiting geometry; the mass and future-transit predictions depend on this.
  • domain assumption The exterior companion wide of 2:1 is the correct architecture
    Selected by BIC among a fixed set of MMR configurations; the TTV posterior for non-transiting companions is degenerate, so this selection is necessary.
  • ad hoc to paper The excluded MAROON-X spectrum is an outlier, not a signal
    The paper excludes one spectrum because it is 5-sigma from the posterior solution, rather than demonstrating it is instrumental or activity-induced.
  • domain assumption Stellar activity does not mimic the planet RVs
    Supported by GLS periodograms of activity indicators and rotation period, but residual jitter is 23.6 m/s.

how reviews work

0 comments
Cite this review

Pith. "Pith review of A Pair of Warm Saturn-mass Planets near the 2:1 Mean Motion Resonance around TOI-3850." pith.science (2026). https://pith.science/paper/ESH6PCNC

@misc{pith2026260811328,
  author       = {Pith},
  title        = {Pith review of: A Pair of Warm Saturn-mass Planets near the 2:1 Mean Motion Resonance around TOI-3850},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ESH6PCNC}},
  note         = {Machine review of arXiv:2608.11328}
}
abstract

Warm Jupiters, with orbital periods of $10$--$200~\rm{days}$ and radii exceeding $8~R_{\oplus}$, are a relatively understudied class of exoplanets occupying the parameter space between hot Jupiters and more widely separated, colder Jupiter analogs. In this work, we report the detection of a multi-planet warm Jupiter system around TOI-3850 (TIC-143008050), a moderately active, near-solar metallicity G0 dwarf star observed by TESS in Sectors 15, 21, 41, 48 and 75. Initially, a single candidate planet was discovered by TESS, displaying transit timing variations (TTVs) with an amplitude of $\sim 1~\rm hr$ and a super-period of $513~\rm days$. Through a combination of transit photometry, radial velocity observations with MAROON-X, and TTV modeling, we identify two planets: TOI-3850 b $(P_b=14.484\pm0.002~\mathrm{days},~ M_b =112\pm20~M_{\oplus},~e_b = 0.018\pm0.008, R_b = 12.07\pm0.09~R_{\oplus}, ~T_{\rm{eq}}=841\pm10~\rm{K})$, a transiting warm Jupiter, and TOI-3850 c $(P_c=29.85\pm0.01~\mathrm{days},~ M_c =90\pm15~M_{\oplus},~e_c < 0.015, ~T_{\rm{eq}}=661\pm7~\rm{K})$, a non-transiting, Saturn-mass companion. The two planets lie wide of the 2:1 mean motion resonance $(P_c/P_b \approx 2.06)$, consistent with a formation history involving disk-driven migration. $N$-body integrations indicate that TOI-3850 c may begin to transit on decadal timescales, while TOI-3850 b remains a promising target for follow-up atmospheric characterization.

Figures

Figures reproduced from arXiv: 2608.11328 by the authors.

Figure 1
Figure 1. Left: Difference image of TOI-3850.01. The top panel was produced using a 20 × 20 pixel grid of Sector 48 FFIs. The bottom panel zooms in on the central 5 × 5 pix￾els. Right: Average of out-of-transit images, representing a direct image of the sky near TOI-3850. All colour bars show the flux in units of electrons per second. Nearby stars with ∆Tmag ≤ 10 are depicted as white circles with sizes scaled by their flux. … view at source ↗
Figure 2
Figure 2. High-resolution contrast curve for TOI-3850, derived from speckle observations in the I-band with the SAI-2.5 m telescope. The curve shows the limiting difference in apparent magnitude between the target and a detectable companion as a function of angular distance from TOI-3850. The increasing contrast toward larger separations indicates sensitivity to fainter companions farther from the target. No nearby companion … view at source ↗
Figure 3
Figure 3. Spectral energy distribution of TOI-3850. 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 gray swathe represents the Gaia spectrophotometry (also in the inset). As inputs, we use the observed photometric mag￾nitudes (J, H, K, W1, W2, W3, G, GR… view at source ↗
Figures from the paper (9 more)
Figure 4
Figure 4. Figure 4: Left: Time series of stellar activity indicators determined by the SERVAL reduction pipeline. Indicators include the differential line width (dLW) and the Hα, Ca II IRT, Na, and chromatic (CRX) indices. Right: Generalized Lomb Scargle (GLS) periodogram of stellar activ…
Figure 5
Figure 5. Figure 5: Panel (a). Generalized Lomb Scargle (GLS) pe￾riodogram of the out-of-transit TESS light curve in Sectors 15, 21, 41, 48, and 75. The peak periodic component at Ppeak = 5.89 days suggests TOI-3850 has a rotation period P ∼ 6 days. Since this does not overlap with the or…
Figure 6
Figure 6. Figure 6: Median light curve models and transit data for all TESS, LCO, and FLWO observations used in the global transit fit. Each night of ground-based photometry is shown separately while the TESS observations have been phase-folded at the median orbital period. For clarity, w…
Figure 7
Figure 7. Figure 7: Radial velocity (RV) models and residuals fit to our MAROON-X observations. Here, we explore models consisting of (a) zero, (b) one, and (c) two planets to assess which configuration best explains the observed RV signal. The zero planet model consists exclusively of an…
Figure 8
Figure 8. Figure 8: Best-fit joint radial velocity (left) and transit timing variation (right) model for the TOI-3850 system, suggesting the presence of two planets: TOI-3850 b and TOI-3850 c. TOI-3850 b is a Saturn-mass planet with Mb ≈ 112 M⊕ at an orbital period of Pb ≈ 14.5 days, whil…
Figure 9
Figure 9. Figure 9: Depiction of the orbits of TOI-3850 b and TOI-3850 c based on the median values in the joint RV + TTV fit. Warm Jupiters may represent a heterogeneous popu￾lation with multiple formation and migration pathways. Several warm Jupiters have been found in single planet sys…
Figure 10
Figure 10. Figure 10: Cumulative distribution function (CDF) of the first time TOI-3850 c reaches a transit-permitting geometry, defined as bc < 1, measured from t0 = 4010 TBJD (2025 November 30). The dashed line marks the median (26.6 yr) and the shaded region shows the 16th–84th percenti…
Figure 11
Figure 11. Figure 11: Time evolution of the best-fit dynamical configuration of the TOI-3850 system from a 1 Myr integration with REBOUND. The osculating period ratio, eccentricities, and impact parameters are shown for the first 1000 years while the resonant angles are shown for the first…
Figure 12
Figure 12. Figure 12: , we show all confirmed warm Jupiters on a radius-mass diagram, with the colour scale denoting TSM. 10 1 10 2 10 3 Planet Mass [M ] 8 10 12 14 16 Pla n e t R a diu s [ R ] TOI 3850 b Lone WJs Multi-planet WJs 10 100 TSM [PITH_FULL_IMAGE:figures/full_fig_p018_12.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

117 extracted references · 12 canonical work pages

  1. [1]

    On detecting terrestrial planets with timing of giant planet transits , url =

    Agol, Eric and Steffen, Jason and Sari, Re'em and Clarkson, Will , journal =. On detecting terrestrial planets with timing of giant planet transits , url =. 2005 , month = May, volume =

    2005

  2. [2]

    Monthly Notices of the Royal Astronomical Society , author =

    Moderately eccentric warm. Monthly Notices of the Royal Astronomical Society , author =. 2017 , pages =. doi:10.1093/mnras/stx2250 , number =

    doi:10.1093/mnras/stx2250 2017

  3. [3]

    and Agol, Eric and Holman, Matthew J

    Deck, Katherine M. and Agol, Eric and Holman, Matthew J. and Nesvorný, David , month = may, year =. The Astrophysical Journal , publisher =. doi:10.1088/0004-637X/787/2/132 , language =

    doi:10.1088/0004-637x/787/2/132

  4. [4]

    The Astrophysical Journal Letters , publisher =

    Dong, Subo and Katz, Boaz and Socrates, Aristotle , month = dec, year =. The Astrophysical Journal Letters , publisher =. doi:10.1088/2041-8205/781/1/L5 , language =

    doi:10.1088/2041-8205/781/1/l5

  5. [5]

    and Lang, Dustin and Goodman, Jonathan , month = feb, year =

    Foreman-Mackey, Daniel and Hogg, David W. and Lang, Dustin and Goodman, Jonathan , month = feb, year =. emcee:. Publications of the Astronomical Society of the Pacific , publisher =. doi:10.1086/670067 , language =

    doi:10.1086/670067

  6. [6]

    Journal of Open Source Software , author =

    `exoplanet`:. Journal of Open Source Software , author =. 2021 , pages =. doi:10.21105/joss.03285 , language =

    doi:10.21105/joss.03285 2021

  7. [7]

    Journal of Geophysical Research: Planets , author =

    Hot. Journal of Geophysical Research: Planets , author =. doi:10.1029/2020JE006629 , language =

    doi:10.1029/2020je006629

  8. [8]

    The Astrophysical Journal , publisher =

    Hadden, Sam and Lithwick, Yoram , month = aug, year =. The Astrophysical Journal , publisher =. doi:10.3847/0004-637X/828/1/44 , language =

    doi:10.3847/0004-637x/828/1/44

Show all 117 references
  1. [9]

    Formation of hot

    Heller, René , month = aug, year =. Formation of hot. Astronomy & Astrophysics , publisher =. doi:10.1051/0004-6361/201833486 , language =

    doi

  2. [10]

    Huang, Chelsea and Wu, Yanqin and Triaud, Amaury H. M. J. , month = jul, year =. The Astrophysical Journal , publisher =. doi:10.3847/0004-637X/825/2/98 , language =

    doi

  3. [11]

    and Winn, Joshua N

    Sullivan, Peter W. and Winn, Joshua N. and Berta-Thompson, Zachory K. and Charbonneau, David and Deming, Drake and Dressing, Courtney D. and Latham, David W. and Levine, Alan M. and McCullough, Peter R. and Morton, Timothy and Ricker, George R. and Vanderspek, Roland and Woods...

    2015

  4. [12]

    and Bakos, G

    Zhou, G. and Bakos, G. HAT-P-67b: An Extremely Low Density Saturn Transiting an F-subgiant Confirmed via Doppler Tomography , journal =. 2017 , doi =

    2017

  5. [13]

    and Henry, Todd J

    Raghavan, Deepak and McAlister, Harold A. and Henry, Todd J. and Latham, David W. and Marcy, Geoffrey W. and et al. , title =. The Astrophysical Journal Supplement Series , volume =. 2010 , doi =

    2010

  6. [14]

    and Seager, S

    Guerrero, Natalia M. and Seager, S. and Huang, Chelsea X. and Vanderburg, Andrew and et al. , title =. The Astrophysical Journal Supplement Series , volume =. 2021 , doi =

    2021

  7. [15]

    and Liu, S.-F

    Rein, H. and Liu, S.-F. , title =. Astronomy & Astrophysics , volume =. 2012 , doi =

    2012

  8. [16]

    The Astronomical Journal , volume =

    Saha, Prasenjit and Tremaine, Scott , title =. The Astronomical Journal , volume =. 1992 , doi =

    1992

  9. [17]

    and Kratter, Kaitlin M

    Morrison, Sarah J. and Kratter, Kaitlin M. , title =. The Astrophysical Journal , volume =. 2016 , doi =

    2016

  10. [18]

    Brown, T. M. and Baliber, N. and Bianco, F. B. and et al. , title =. Publications of the Astronomical Society of the Pacific , volume =. 2013 , doi =

    2013

  11. [19]

    and Harbeck, Daniel-Rolf and et al

    McCully, Curtis and Volgenau, Nikolaus H. and Harbeck, Daniel-Rolf and et al. , title =. Software and Cyberinfrastructure for Astronomy V , volume =. 2018 , doi =

    2018

  12. [20]

    and Kielkopf, John F

    Collins, Karen A. and Kielkopf, John F. and Stassun, Keivan G. and Hessman, Frederic V. , title =. The Astronomical Journal , volume =. 2017 , doi =

    2017

  13. [21]

    Strakhov, I. A. and Safonov, B. S. and Cheryasov, D. V. , month = jun, year =. Speckle. Astrophysical Bulletin , publisher =. doi:10.1134/S1990341323020104 , urldate =

    doi

  14. [22]

    and Milisavljevic, Dan and Crabtree, Kyle N

    Law, Charles J. and Milisavljevic, Dan and Crabtree, Kyle N. and et al. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2017 , doi =

    2017

  15. [23]

    and Reiners, A

    Zechmeister, M. and Reiners, A. and Amado, P. J. and et al. , title =. Astronomy & Astrophysics , volume =. 2018 , doi =

    2018

  16. [24]

    and Schwab, Christian , title =

    Seifahrt, Andreas and Stürmer, Julian and Bean, Jacob L. and Schwab, Christian , title =. Ground-based and Airborne Instrumentation for Astronomy VII , volume =. 2018 , doi =

    2018

  17. [25]

    and Cloutier, Ryan and Medina, Amber A

    Winters, Jennifer G. and Cloutier, Ryan and Medina, Amber A. and et al. , title =. The Astronomical Journal , volume =. 2022 , doi =

    2022

  18. [26]

    and Caballero, J

    Trifonov, T. and Caballero, J. A. and Morales, J. C. and et al. , title =. Science , volume =. 2021 , doi =

    2021

  19. [27]

    , title =

    Kunimoto, Michelle and Daylan, Tansu and Guerrero, Natalia and et al. , title =. The Astrophysical Journal Supplement Series , volume =. 2022 , doi =

    2022

  20. [28]

    and Jenkins, Jon M

    Bryson, Stephen T. and Jenkins, Jon M. and Gilliland, Ronald L. and et al. , title =. Publications of the Astronomical Society of the Pacific , volume =. 2013 , doi =

    2013

  21. [29]

    and Oelkers, Ryan J

    Stassun, Keivan G. and Oelkers, Ryan J. and Paegert, Martin and et al. , title =. The Astronomical Journal , volume =. 2019 , doi =

    2019

  22. [30]

    and Bizzarro, Martin and Latham, David W

    Buchhave, Lars A. and Bizzarro, Martin and Latham, David W. and et al. , title =. Nature , volume =. 2014 , doi =

    2014

  23. [31]

    and Latham, David W

    Buchhave, Lars A. and Latham, David W. and Johansen, Anders and et al. , title =. Nature , volume =. 2012 , doi =

    2012

  24. [32]

    , title =

    Choi, Jieun and Dotter, Aaron and Conroy, Charlie and et al. , title =. The Astrophysical Journal , volume =. 2016 , doi =

    2016

  25. [33]

    Lomb, N. R. , title =. Astrophysics and Space Science , volume =. 1976 , doi =

    1976

  26. [34]

    Scargle, J. D. , title =. The Astrophysical Journal , volume =. 1982 , doi =

    1982

  27. [35]

    2022 , doi =

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project , journal =. 2022 , doi =

    2022

  28. [36]

    and Kürster, M

    Zechmeister, M. and Kürster, M. , title =. Astronomy & Astrophysics , volume =. 2009 , doi =

    2009

  29. [37]

    and Donahue, Robert A

    Saar, Steven H. and Donahue, Robert A. , title =. The Astrophysical Journal , volume =. 1997 , doi =

    1997

  30. [38]

    and Mulders, Gijs D

    Hippke, Michael and David, Trevor J. and Mulders, Gijs D. and Heller, René , title =. The Astronomical Journal , volume =. 2019 , doi =

    2019

  31. [39]

    Publications of the Astronomical Society of the Pacific , volume =

    Kreidberg, Laura , title =. Publications of the Astronomical Society of the Pacific , volume =. 2015 , doi =

    2015

  32. [40]

    , title =

    Abril-Pla, Oriol and Andreani, Virgile and Carroll, Colin and et al. , title =. PeerJ Computer Science , volume =. 2023 , doi =

    2023

  33. [41]

    The Astrophysical Journal Letters , volume =

    Lithwick, Yoram and Wu, Yanqin , title =. The Astrophysical Journal Letters , volume =. 2012 , doi =

    2012

  34. [42]

    The Astronomical Journal , volume =

    Batygin, Konstantin and Morbidelli, Alessandro , title =. The Astronomical Journal , volume =. 2012 , doi =

    2012

  35. [43]

    and Eberhardt, Jan and Trifonov, Trifon and et al

    Mihaylov, Deyan P. and Eberhardt, Jan and Trifonov, Trifon and et al. , title =. The Astronomical Journal , volume =. 2026 , doi =

    2026

  36. [44]

    and Fabrycky, Daniel C

    Mills, Sean M. and Fabrycky, Daniel C. , title =. The Astronomical Journal , volume =. 2017 , doi =

    2017

  37. [45]

    , year =

    Winn, Joshua N. , year =. The. Handbook of. doi:10.1007/978-3-319-30648-3_83-1 , pages =

    doi

  38. [46]

    2018 , archivePrefix =

    Lightkurve: Kepler and TESS time series analysis in Python , howpublished =. 2018 , archivePrefix =. 1812.013 , adsurl =

    2018

  39. [47]

    , title =

    Morton, Timothy D. , title =. 2015 , archivePrefix =. 1503.010 , adsurl =

    2015

  40. [48]

    and Davis, M

    Kunimoto, Michelle and Vanderburg, Andrew and Huang, Chelsea X. and Davis, M. Ryleigh and Affer, Laura and Cameron, Andrew Collier and Charbonneau, David and Cosentino, Rosario and Damasso, Mario and Dumusque, Xavier and Fiorenzano, A. F. Martnez and Ghedina, Adriano and Haywo...

  41. [49]

    2017 , archivePrefix =

    Eastman, Jason , title =. 2017 , archivePrefix =. 1710.003 , adsurl =

    2017

  42. [50]

    doi:10.5281/zenodo.16175987 , urldate =

    Newville, Matthew and Otten, Renee and Nelson, Andrew and Stensitzki, Till and Ingargiola, Antonino and Allan, Daniel and Fox, Austin and Carter, Faustin and Rawlik, Michal , month = jul, year =. doi:10.5281/zenodo.16175987 , urldate =

    doi

  43. [51]

    and Petigura, Erik A

    Fulton, Benjamin J. and Petigura, Erik A. and Blunt, Sarah and Sinukoff, Evan , month = apr, year =. doi:10.1088/1538-3873/aaaaa8 , journal =

    doi

  44. [52]

    and Ragozzine, Darin and Fabrycky, Daniel C

    Lissauer, Jack J. and Ragozzine, Darin and Fabrycky, Daniel C. and Steffen, Jason H. and Ford, Eric B. and Jenkins, Jon M. and Shporer, Avi and Holman, Matthew J. and Rowe, Jason F. and Quintana, Elisa V. and Batalha, Natalie M. and Borucki, William J. and Bryson, Stephen T. a...

  45. [53]

    Howard, A. W. and Bakos, G. 2012 , pages =. doi:10.1088/0004-637X/749/2/134 , journal =

    2012 doi

  46. [54]

    Almenara, J. M. and Leleu, A. and Guillot, T. and Mardling, R. and Bouchy, F. and Forveille, T. and Winn, J. and Abe, L. and Beltrame, M. and Bendjoya, P. and Bonfils, X. and Deline, A. and Delisle, J.-B. and Díaz, R. F. and Fridén, E. and Hobson, M. and Hoogenboom, R. M. and ...

  47. [55]

    Proceedings of the National Academy of Sciences of the United States of America , author =

    Architectures of planetary systems and implications for their formation , volume =. Proceedings of the National Academy of Sciences of the United States of America , author =. 2014 , pages =. doi:10.1073/pnas.1304219111 , number =

    2014 doi

  48. [56]

    and Laughlin, Gregory P

    Batygin, Konstantin and Bodenheimer, Peter H. and Laughlin, Gregory P. , month = sep, year =. The Astrophysical Journal , publisher =. doi:10.3847/0004-637X/829/2/114 , language =

    doi

  49. [57]

    and Davies, Melvyn B

    Mustill, Alexander J. and Davies, Melvyn B. and Johansen, Anders , month = jul, year =. The Astrophysical Journal , publisher =. doi:10.1088/0004-637X/808/1/14 , language =

    doi

  50. [58]

    Lee, Man Hoi and Peale, S. J. , month = mar, year =. Dynamics and. The Astrophysical Journal , publisher =. doi:10.1086/338504 , language =

    doi

  51. [59]

    Resonance capture and stability analysis for planet pairs under

    Lin, Linghong and Liu, Beibei and Zheng, Zekai , month = oct, year =. Resonance capture and stability analysis for planet pairs under. Astronomy & Astrophysics , publisher =. doi:10.1051/0004-6361/202453589 , urldate =

    doi

  52. [60]

    Tamayo, Daniel and Murray, Norman and Tremaine, Scott and Winn, Joshua , month = oct, year =. A. The Astronomical Journal , publisher =. doi:10.3847/1538-3881/ac1c6a , language =

    doi

  53. [61]

    and Ho, Shirley and Spergel, David N

    Tamayo, Daniel and Cranmer, Miles and Hadden, Samuel and Rein, Hanno and Battaglia, Peter and Obertas, Alysa and Armitage, Philip J. and Ho, Shirley and Spergel, David N. and Gilbertson, Christian and Hussain, Naireen and Silburt, Ari and Jontof-Hutter, Daniel and Menou, Krist...

    doi

  54. [62]

    , month = apr, year =

    Gratia, Pierre and Lissauer, Jack J. , month = apr, year =. Eccentricities and the stability of closely-spaced five-planet systems , volume =. doi:10.1016/j.icarus.2020.114038 , journal =

    2020

  55. [63]

    Icarus , author =

    Dynamics of. Icarus , author =. 1993 , pages =. doi:10.1006/icar.1993.1169 , urldate =

    1993

  56. [64]

    , month = aug, year =

    Marzari, F. , month = aug, year =. Dynamical behaviour of multiplanet systems close to their stability limit , volume =. doi:10.1093/mnras/stu929 , journal =

    doi

  57. [65]

    Cincotta, P. M. and Simó, C. , month = dec, year =. Simple tools to study global dynamics in non-axisymmetric galactic potentials -. doi:10.1051/aas:2000108 , journal =

    doi

  58. [66]

    Exoplanet

    Seager, Sara and Deming, Drake , month = sep, year =. Exoplanet. Annual Review of Astronomy and Astrophysics , publisher =. doi:10.1146/annurev-astro-081309-130837 , language =

    doi

  59. [67]

    Exoplanetary

    Madhusudhan, Nikku , month = aug, year =. Exoplanetary. Annual Review of Astronomy and Astrophysics , publisher =. doi:10.1146/annurev-astro-081817-051846 , number =

    doi

  60. [68]

    and Bean, Jacob L

    Kempton, Eliza M.-R. and Bean, Jacob L. and Louie, Dana R. and Deming, Drake and Koll, Daniel D. B. and Mansfield, Megan and Christiansen, Jessie L. and López-Morales, Mercedes and Swain, Mark R. and Zellem, Robert T. and Ballard, Sarah and Barclay, Thomas and Barstow, Joanna ...

  61. [69]

    Tinetti, Giovanna and Eccleston, Paul and Lueftinger, Theresa and Salvignol, Jean-Christophe and Fahmy, Salma and Alves de Oliveira, Caterina , month = sep, year =. Ariel:. doi:10.5194/epsc2022-1114 , urldate =

    doi

  62. [70]

    and Johnson, John Asher , month = sep, year =

    Dawson, Rebekah I. and Johnson, John Asher , month = sep, year =. Origins of. Annual Review of Astronomy and Astrophysics , publisher =. doi:10.1146/annurev-astro-081817-051853 , language =

    doi

  63. [71]

    and Cowan, Nicolas B

    D’Aoust, Lina and Coull-Neveu, Ben and Lee, Eve J. and Cowan, Nicolas B. , month = dec, year =. Testing the. The Astrophysical Journal , publisher =. doi:10.3847/1538-4357/ae10ac , language =

    doi

  64. [72]

    and Vanderburg, Andrew and Adams, Fred C

    Becker, Juliette C. and Vanderburg, Andrew and Adams, Fred C. and Rappaport, Saul A. and Schwengeler, Hans Martin , month = oct, year =. The Astrophysical Journal Letters , publisher =. doi:10.1088/2041-8205/812/2/L18 , number =

    doi

  65. [73]

    Models of

    Rauscher, Emily , month = aug, year =. Models of. The Astrophysical Journal , publisher =. doi:10.3847/1538-4357/aa81c3 , number =

    doi

  66. [74]

    and Millholland, Sarah C

    Gupta, Arvind F. and Millholland, Sarah C. and Im, Haedam and Dong, Jiayin and Jackson, Jonathan M. and Carleo, Ilaria and Libby-Roberts, Jessica and Delamer, Megan and Giovinazzi, Mark R. and Lin, Andrea S. J. and Kanodia, Shubham and Wang, Xian-Yu and Stassun, Keivan and Mas...

  67. [75]

    The Astrophysical Journal , publisher =

    Petrovich, Cristobal and Tremaine, Scott , month = sep, year =. The Astrophysical Journal , publisher =. doi:10.3847/0004-637X/829/2/132 , number =

    doi

  68. [76]

    In situ scattering of warm

    Anderson, Kassandra R and Lai, Dong and Pu, Bonan , month = jan, year =. In situ scattering of warm. doi:10.1093/mnras/stz3119 , journal =

    doi

  69. [77]

    , month = nov, year =

    Gelman, Andrew and Rubin, Donald B. , month = nov, year =. Inference from. Statistical Science , publisher =. doi:10.1214/ss/1177011136 , language =

  70. [78]

    2022 , pages =

    Journal of Open Source Software , author =. 2022 , pages =. doi:10.21105/joss.04304 , language =

    2022 doi

  71. [79]

    Monthly Notices of the Royal Astronomical Society: Letters , author =

    Degeneracy in the characterization of non-transiting planets from transit timing variations , volume =. Monthly Notices of the Royal Astronomical Society: Letters , author =. 2012 , pages =. doi:10.1111/j.1745-3933.2012.01236.x , number =

    2012

  72. [80]

    , month = may, year =

    Lammers, Caleb and Winn, Joshua N. , month = may, year =. The Astronomical Journal , publisher =. doi:10.3847/1538-3881/ae61a3 , number =

    doi

  73. [81]

    , year = 2026, month = jun, pages =

    TOI-2147 b and TOI-6019 b: Two eccentric warm Jupiters detected and characterized with TESS and MaHPS. , year = 2026, month = jun, pages =

    2026

  74. [82]

    2017 , pages =

    Monthly Notices of the Royal Astronomical Society , author =. 2017 , pages =. doi:10.1093/mnras/stw3005 , urldate =

    2017 doi

  75. [83]

    and Watkins, Cristilyn N

    Pinto, Marcelo Tala and Jordán, Andrés and Acuña, Lorena and Jones, Matías and Brahm, Rafael and Reinarz, Yared and Eberhardt, Jan and Espinoza, Néstor and Henning, Thomas and Hobson, Melissa and Rojas, Felipe and Schlecker, Martin and Trifonov, Trifon and Bakos, Gaspar and Bo...

  76. [84]

    Monthly Notices of the Royal Astronomical Society , author =

    A general model of resonance capture in planetary systems: first- and second-order resonances , volume =. Monthly Notices of the Royal Astronomical Society , author =. 2011 , pages =. doi:10.1111/j.1365-2966.2011.18201.x , number =

    2011

  77. [85]

    , keywords =

    Parallax Systematics and Photocenter Motions of Benchmark Eclipsing Binaries in Gaia EDR3. , keywords =. doi:10.3847/2041-8213/abdaad , archivePrefix =. 2101.03425 , primaryClass =

    arXiv

  78. [86]

    , keywords =

    Evidence for a Systematic Offset of -80 as in the Gaia DR2 Parallaxes. , keywords =. doi:10.3847/1538-4357/aacafc , archivePrefix =. 1805.03526 , primaryClass =

    arXiv

  79. [87]

    , keywords =

    Empirical Accurate Masses and Radii of Single Stars with TESS and Gaia. , keywords =. doi:10.3847/1538-3881/aa998a , archivePrefix =. 1710.01460 , primaryClass =

    arXiv

  80. [88]

    , keywords =

    Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes. , keywords =. doi:10.3847/1538-3881/aa5df3 , archivePrefix =. 1609.04389 , primaryClass =

    arXiv

  81. [89]

    , keywords =

    Eclipsing Binaries as Benchmarks for Trigonometric Parallaxes in the Gaia Era. , keywords =. doi:10.3847/0004-6256/152/6/180 , archivePrefix =. 1609.02579 , primaryClass =

    arXiv

  82. [90]

    , keywords =

    Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds. , keywords =. doi:10.1086/305772 , archivePrefix =. astro-ph/9710327 , primaryClass =

    arXiv

  83. [91]

    , keywords =

    Accurate masses and radii of normal stars: modern results and applications. , keywords =. doi:10.1007/s00159-009-0025-1 , archivePrefix =. 0908.2624 , primaryClass =

    arXiv

  84. [92]

    , keywords =

    Stellar Activity in the Broadband Ultraviolet. , keywords =. doi:10.1088/0004-6256/142/1/23 , archivePrefix =. 1105.1377 , primaryClass =

  85. [93]

    The rotation-activity relationship for very low-mass stars through R' _ HK

    Magnetic activity in the HARPS M dwarf sample. The rotation-activity relationship for very low-mass stars through R' _ HK. , keywords =. doi:10.1051/0004-6361/201527078 , archivePrefix =. 1610.09007 , primaryClass =

    arXiv

  86. [94]

    Research Notes of the American Astronomical Society , year = 2018, month = feb, volume =

    The Rotation-Age Relationship of M Dwarfs: A Progress Report of the Living with a Red Dwarf Program. Research Notes of the American Astronomical Society , year = 2018, month = feb, volume =. doi:10.3847/2515-5172/aab1f8 , adsurl =

    2018 doi

  87. [95]

    VizieR Online Data Catalog , keywords =

    VizieR Online Data Catalog: Homogeneous Means in the UBV System (Mermilliod 1991). VizieR Online Data Catalog , keywords =

    1991

  88. [96]

    How to Constrain Your M Dwarf. II. The Mass-Luminosity-Metallicity Relation from 0.075 to 0.70 Solar Masses. , keywords =. doi:10.3847/1538-4357/aaf3bc , archivePrefix =. 1811.06938 , primaryClass =

    arXiv

  89. [97]

    , keywords =

    Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics. , keywords =. doi:10.1086/591785 , archivePrefix =. 0807.1686 , primaryClass =

    arXiv

  90. [98]

    , keywords =

    A new catalogue of Str \"o mgren-Crawford uvby photometry. , keywords =. doi:10.1051/0004-6361/201526413 , archivePrefix =. 1506.04568 , primaryClass =

    arXiv

  91. [99]

    , keywords =

    Y ^ 2 Isochrones with an Improved Core Overshoot Treatment. , keywords =. doi:10.1086/424966 , adsurl =

    doi

  92. [100]

    , keywords =

    The NextGen Model Atmosphere Grid for 3000<=T _ eff <=10,000 K. , keywords =. doi:10.1086/306745 , archivePrefix =. astro-ph/9807286 , primaryClass =

    arXiv

  93. [101]

    , keywords =

    Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors. , keywords =. doi:10.1086/519295 , archivePrefix =. 0704.3068 , primaryClass =

    arXiv

  94. [102]

    IAU Colloq

    A New Opacity-Sampling Model Atmosphere Program for Arbitrary Abundances. IAU Colloq. 138: Peculiar versus Normal Phenomena in A-type and Related Stars , year = 1993, editor =

    1993

  95. [103]

    , keywords =

    A new extensive library of PHOENIX stellar atmospheres and synthetic spectra. , keywords =. doi:10.1051/0004-6361/201219058 , archivePrefix =. 1303.5632 , primaryClass =

    arXiv

  96. [104]

    , keywords =

    White dwarf spectra and atmosphere models. , keywords =

  97. [105]

    and Polania Vivas, Michael S

    MacDonald, Mariah G. and Polania Vivas, Michael S. and D’Angiolillo, Skylar and Fernandez, Ashley N. and Quinn, Tyler , month = aug, year =. The Astronomical Journal , publisher =. doi:10.3847/1538-3881/ace69d , language =

    doi

  98. [106]

    , month = jan, year =

    Goldreich, Peter and Schlichting, Hilke E. , month = jan, year =. The Astronomical Journal , publisher =. doi:10.1088/0004-6256/147/2/32 , number =

    doi

  99. [107]

    doi:10.5281/zenodo.21003741 , url =

    pandas-dev/pandas: Pandas , month = jun, year =. doi:10.5281/zenodo.21003741 , url =

    doi

  100. [108]

    Computing in Science & Engineering , author =

    Matplotlib:. Computing in Science & Engineering , author =. 2007 , pages =. doi:10.1109/MCSE.2007.55 , number =

    2007 doi

  101. [109]

    and Millman, K

    Harris, Charles R. and Millman, K. Jarrod and van der Walt, Stéfan J. and Gommers, Ralf and Virtanen, Pauli and Cournapeau, David and Wieser, Eric and Taylor, Julian and Berg, Sebastian and Smith, Nathaniel J. and Kern, Robert and Picus, Matti and Hoyer, Stephan and van Kerkwi...

  102. [110]

    and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and van der Walt, Stéfan J

    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 van der Walt, Stéfan J. and Brett, Matthew and Wilson, Joshua and Millma...

  103. [111]

    Software and Cyberinfrastructure for Astronomy IV , year = 2016, series =

    The TESS science processing operations center. Software and Cyberinfrastructure for Astronomy IV , year = 2016, series =. doi:10.1117/12.2233418 , adsurl =

    2016 doi

  104. [112]

    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 =

    2011 arXiv

  105. [113]

    The Astrophysical Journal , publisher =

    Perryman, Michael and Hartman, Joel and Bakos, G. The Astrophysical Journal , publisher =. 2014 , pages =. doi:10.1088/0004-637X/797/1/14 , language =

    2014 doi

  106. [114]

    and Lattanzi, M

    Casertano, S. and Lattanzi, M. G. and Sozzetti, A. and Spagna, A. and Jancart, S. and Morbidelli, R. and Pannunzio, R. and Pourbaix, D. and Queloz, D. , month = may, year =. Double-blind test program for astrometric planet detection with. Astronomy & Astrophysics , publisher =...

    doi

  107. [115]

    and Brown, A

    Vallenari, A. and Brown, A. G. A. and Prusti, T. and Bruijne, J. H. J. de and Arenou, F. and Babusiaux, C. and Biermann, M. and Creevey, O. L. and Ducourant, C. and Evans, D. W. and Eyer, L. and Guerra, R. and Hutton, A. and Jordi, C. and Klioner, S. A. and Lammers, U. L. and ...

  108. [116]

    ChatGPT v5.6 , year =

  109. [117]

    doi:10.26134/EXOFOP5 , url =

    Exoplanet Follow-up Observing Program Web Service , publisher =. doi:10.26134/EXOFOP5 , url =

    doi

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.