Pith. sign in

REVIEW 2 major objections 5 minor 129 references

A transiting giant planet in orbit around a 0.2-solar-mass host star

T0 review · 2 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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

Pith's one-line read TOI-6894b, a 0.168-Jupiter-mass giant planet transiting a 0.207-solar-mass M dwarf, makes its host the lowest-mass star known to host a transiting giant planet.

desk verdict TOI-6894b is a real, well-vetted benchmark discovery—the lowest-mass star hosting a transiting giant planet—with only minor model-dependence in the stellar mass that doesn't threaten the headline claim. read the letter →

arxiv 2506.07931 v2 pith:75XEXWD3 submitted 2025-06-09 astro-ph.EP astro-ph.SR

Edward M. Bryant , Andrés Jordán , Joel D. Hartman , Daniel Bayliss , Elyar Sedaghati , Khalid Barkaoui , Jamila Chouqar , Francisco J. Pozuelos
show 51 more authors
Daniel P. Thorngren Mathilde Timmermans Jose Manuel Almenara Igor V. Chilingarian Karen A. Collins Tianjun Gan Steve B. Howell Norio Narita Enric Palle Benjamin V. Rackham Amaury H.M.J. Triaud Gaspar Á. Bakos Rafael Brahm Melissa J. Hobson Vincent Van Eylen Pedro J. Amado Luc Arnold Xavier Bonfils Artem Burdanov Charles Cadieux Douglas A. Caldwell Victor Casanova David Charbonneau Catherine A. Clark Kevin I. Collins Tansu Daylan Georgina Dransfield Brice-Oliver Demory Elsa Ducrot Gareb Fernández-Rodríguez Izuru Fukuda Akihiko Fukui Michaël Gillon Rebecca Gore Matthew J. Hooton Kai Ikuta Emmanuel Jehin Jon M. Jenkins Alan M. Levine Colin Littlefield Felipe Murgas Kendra Nguyen Hannu Parviainen Didier Queloz S. Seager Daniel Sebastian Gregor Srdoc R. Vanderspek Joshua N. Winn Julien de Wit Sebastián Zúñiga-Fernández
This is my paper
classification astro-ph.EPastro-ph.SR
keywords exoplanetsMdwarfstarsgiantplanetstransitingplanetformationatmosphericcharacterizationinteriorstructureTOI-6894
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

This paper reports the discovery and characterization of TOI-6894b, a transiting giant planet with mass $0.168 \pm 0.022\,M_{\rm J}$ and radius $0.855 \pm 0.022\,R_{\rm J}$ around the $0.207 \pm 0.011\,M_\odot$ star TOI-6894. If the derived stellar mass is right, TOI-6894 is the lowest-mass star known to host a transiting giant planet, and the very existence of the planet contradicts the simplest core-accretion predictions that very low-mass stars cannot form gas giants. The paper also shows the planet probably contains $12 \pm 2\,M_\oplus$ of metals and has exceptionally deep 17% transits, making it a leading target for transmission spectroscopy that could reveal a methane-dominated atmosphere and constrain the formation pathway.

What carries the argument

The argument is carried by the planet-to-star radius ratio: TOI-6894b's deep transits set $R_P/R_* = 0.3860 \pm 0.0029$, and a Keplerian fit to the radial-velocity measurements gives $K = 65.5 \pm 8.3$ m/s. A joint Markov-chain fit of all photometric, radial-velocity, astrometric, and broadband-flux data, with the star constrained to be consistent with stellar-evolution models for low-mass M dwarfs, converts these into stellar and planetary masses and radii. A separate blend analysis, comparing the data against models of a faint eclipsing binary blended with a brighter M dwarf, rules out those false-positive scenarios with large chi-squared differences.

What would settle it

Re-fit the photometry, parallax, and radial velocities with the stellar-evolution model constraint removed and the stellar mass and radius drawn from an empirical mass-radius relation for 0.1-0.3 solar-mass M dwarfs based on eclipsing binaries; if the resulting stellar mass exceeds 0.3 solar masses, or the radius differs by more than about 3 percent, the lowest-mass-star claim and the absolute planet parameters would collapse.

Watch

Extended reading notes

Core claim

On the authors' own terms, the central claim is that the system is a single M5 dwarf of $0.207 \pm 0.011\,M_\odot$ and $0.2276 \pm 0.0057\,R_\odot$ transited every $3.37077196 \pm 0.00000059$ days by a low-density giant planet of $M_P = 0.168 \pm 0.022\,M_J$ ($53.4 \pm 7.1\,M_\oplus$) and $R_P = 0.855 \pm 0.022\,R_J$. The planet's radius is about 1.9 times the star's, giving a 17% transit depth; the radial-velocity semi-amplitude is $65.5 \pm 8.3$ m/s; and an interior retrieval gives a metal mass fraction $Z_P = 0.23 \pm 0.02$, corresponding to $12 \pm 2\,M_\oplus$ of metals. This makes TOI-6894 the lowest-mass star known to date to host a transiting giant planet, and the fourth lowest-mass to host any transiting planet.

Load-bearing premise

The host star's mass and radius come from a joint fit that requires consistency with stellar-evolution models for low-mass M dwarfs; if those models are systematically off for a star near 0.2 solar masses, the 'lowest-mass' record and the absolute planet parameters shift.

Editorial extensions

If this is right

  • TOI-6894b becomes a benchmark for giant-planet formation around very low-mass stars, joining the radial-velocity systems LHS 3154 b, GJ 3512 b/c, and TZ Ari b that already strain formation models.
  • The planet's $12 \pm 2\,M_\oplus$ metal content implies, at a 10% formation efficiency, a disc solid budget near $120\,M_\oplus$, exceeding the most massive known Class II disc around a $0.15$-$0.25\,M_\odot$ star; the mismatch sharpens if disc masses are underestimated or formation happens in the Class 0/I phase.
  • With a transmission spectroscopy metric of $356 \pm 58$, the highest among giant planets with $T_{\rm eq} \le 900$ K or $M_* \le 0.7\,M_\odot$, a single transit observation could deliver signal-to-noise above 100 for methane, water, and carbon dioxide.
  • The equilibrium temperature of $417.9 \pm 8.6$ K places TOI-6894b between hot Jupiters and Jupiter itself, in the regime where methane chemistry should dominate; measuring its atmosphere tests cloud and chemistry models for temperate H/He giants.

Reading between the lines

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

  • Editorial inference: if the stellar-evolution models used to anchor the host-star parameters carry a systematic offset for very low-mass M dwarfs, the 'lowest-mass star' claim and the absolute planet mass and radius would move together; an empirical mass-radius relation from eclipsing binaries would provide a model-free check.
  • Editorial inference: the deep 17% transits also make TOI-6894b a candidate for high-resolution ground-based transmission spectroscopy at near-infrared wavelengths, where methane features should be strong even with a cloud deck near 1 mbar.
  • Editorial inference: a direct atmospheric metallicity measurement would separate two formation routes — planetesimal or pebble accretion delivering metals versus gravitational-instability fragments that later capture solids — because the interior-retrieval estimate of the metal mass is degenerate with atmospheric metallicity.
  • Editorial inference: if formation efficiency around very low-mass stars is lower than the assumed 10%, the required disc solid mass grows, implying either that the known disc sample misses the massive and pebble-rich discs that produce rare giants like this, or that an alternative formation channel is required.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. The paper reports the discovery and characterization of TOI-6894 b, a transiting sub-Saturn-mass giant planet (M_P = 0.168 ± 0.022 M_J, R_P = 0.855 ± 0.022 R_J) orbiting the very low-mass M dwarf TOI-6894 (M_* = 0.207 ± 0.011 M_sun, R_* = 0.2276 ± 0.0057 R_sun). The analysis combines TESS photometry from multiple sectors, an extensive ground-based follow-up campaign, ESPRESSO and SPIRou radial velocities, archival and speckle imaging, a chromaticity analysis, a secondary-eclipse search, and a quantitative blend analysis. The authors conclude that TOI-6894 is the lowest-mass star known to host a transiting giant planet, and they argue that the system challenges core-accretion formation models. They also present interior-structure modeling and forward atmospheric simulations, identifying TOI-6894 b as a high-priority target for transmission spectroscopy with a TSM of 356 ± 58.

Significance. The discovery is significant. If the stellar mass is correct, TOI-6894 b extends the population of transiting giant planets to host stars of only ~0.2 M_sun, a regime where core-accretion models predict that giant planet formation is strongly suppressed. The paper is unusually thorough in its validation: it uses multiple independent transit detections, ground-based and space-based photometry, two independent RV instruments, a blend analysis with Δχ² = 1600 against eclipsing-binary scenarios, archival imaging spanning decades, high-resolution speckle imaging, chromaticity checks, and injection-recovery limits on additional planets. The data and reduction pipelines are publicly available, and the authors disclose the limited blind-detection significance of the ESPRESSO-only RVs. The atmospheric characterization prospects are quantified with both TSM and PANDEXO simulations. These strengths make the paper a valuable contribution to the discovery literature on giant planets around M dwarfs.

major comments (2)
  1. [Methods, Global Analysis; Supplementary Table 2] The headline claim that TOI-6894 is the lowest-mass star known to host a transiting giant planet rests on M_* = 0.207 ± 0.011 M_sun, which is derived from a joint fit that enforces consistency with MIST evolutionary tracks and includes an adopted 5% systematic mass uncertainty. For very low-mass M dwarfs, systematic offsets between model-based and empirical masses can be of comparable or larger size, and the 5% prior does not by itself validate the model scale. I request an explicit robustness test: recompute the stellar and planetary parameters using an independent empirical mass-luminosity or mass-radius relation (e.g., Mann et al. 2019) or a second set of stellar models, and state whether the record claim survives at the 1σ level. If the ranking changes, the claim should be correspondingly softened or rephrased.
  2. [Figure 2 and Section 1.2.2] The 'lowest-mass star' claim is time-sensitive and depends on the comparison sample. Figure 2 and the associated text use the NASA Exoplanet Archive as accessed on 16 May 2024, but the manuscript draft is dated September 2025. Please rerun the comparison against the current archive at the time of submission and, for transparency, tabulate the host-star masses and 1σ uncertainties for the closest transiting-giant-planet competitors (for example TOI-3235 b, TOI-5205 b, TOI-4860 b, and TOI-3884 b). This will allow readers to verify the record claim directly.
minor comments (5)
  1. [Abstract and Table 2] The abstract states that the transits are '17% deep,' but Table 2 gives R_P/R_* = 0.3860 ± 0.0029, which corresponds to a transit depth of approximately 14.9%. Please reconcile this discrepancy or correct the value in the abstract.
  2. [Section 1.2.2 (Main Text)] The sentence 'this analysis confidently confirms the nature of a the TOI-6894 system' contains a typo ('a the'); please correct it.
  3. [Extended Data Figure 1 caption] The caption begins 'The the gray shaded regions' and should read 'The gray shaded regions.'
  4. [Methods, Stellar Atmospheric Parameter Determination and Global Analysis] The paper reports a FIRE-based metallicity of [Fe/H] = +0.240 ± 0.081 and an ODUSSEAS-based value of [Fe/H] = −0.01 ± 0.10, then adopts the FIRE value as the prior but reports a posterior [Fe/H] = 0.142 ± 0.087 in Table 1. Please clarify why the FIRE value is preferred and discuss the role of the SED/photometric constraints in moving the posterior away from the adopted prior.
  5. [Methods, Planet Composition Analysis] The quoted metal mass fraction Z_P = 0.23 ± 0.02 and metal mass 12 ± 2 M_earth are described as statistical uncertainties only. Please state explicitly that systematic uncertainties from the interior model or atmospheric metallicity degeneracy are not included in these numbers, or provide an estimate of their magnitude.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the planet and stellar parameters are derived from independent photometric, radial-velocity, astrometric, and spectroscopic inputs, with no target quantity defined from itself.

full rationale

The characterization chain is self-contained and non-circular. The transiting signal is measured directly in TESS and ground-based photometry, with a consistent ~17% depth and flat-bottom shape modeled by Mandel-Agol transit models; limb-darkening coefficients are assigned independent Gaussian priors from theoretical stellar-atmosphere grids. The radial-velocity semi-amplitude K = 65.5 ± 8.3 m/s is measured from ESPRESSO and SPIRou data, with the orbital period and phase anchored by the photometric ephemeris, and the planet mass follows from K together with the stellar mass. The stellar mass and radius come from a joint fit to broadband photometry, Gaia parallax, and atmospheric priors (Teff = 2960 ± 66 K, [Fe/H] = +0.240 ± 0.081) while enforcing consistency with MIST stellar evolution models; the planet parameters are not fed back as priors on the star, so the star is not defined in terms of the planet. The headline claim that TOI-6894 is the lowest-mass known host of a transiting giant planet is an empirical comparison against the NASA Exoplanet Archive sample, not a predicted quantity derived from the model inputs. The overlapping-author citations (Bryant et al. 2023 for the candidate search, Hartman et al. for the joint-fit methodology, Thorngren et al. for interior forward models) are context or external machinery, and the decisive validation steps—centroid analysis, speckle imaging, archival imaging, chromaticity checks, occultation non-detection, and the blend analysis with Δχ² = 1600 against eclipsing-binary scenarios—use independent data. The authors also explicitly disclose the low blind-detection significance of the ESPRESSO-only RVs, which is a stated limitation rather than a circular step. No equation in the paper sets a reported quantity equal to its own input, and no fitted parameter is renamed as a prediction.

Assumptions & free parameters 2 free parameters · 4 assumptions · 0 invented entities

The central detection does not depend on hand-tuned constants; the planet's mass, radius, and period come from direct fits to data. The only hand-chosen inputs are the Bond albedo and heat redistribution efficiency used for the equilibrium temperature and transmission spectroscopy metric, which are secondary claims. The analysis does rely on several external model assumptions, which are listed as axioms.

free parameters (2)
  • Bond albedo A = 0.1 (assumed)
    Assumed to compute T_eq = 417.9±8.6 K and the transmission spectroscopy metric TSM = 356±58. This is a hand-chosen value that affects secondary atmospheric characterization claims, not the central detection.
  • Heat redistribution efficiency = efficient (100%)
    Assumed efficient heat redistribution in the equilibrium temperature calculation, stated in the text alongside the albedo. Affects the same secondary claims as the albedo.
assumptions (4)
  • domain assumption MIST stellar evolution models accurately predict the mass-radius-luminosity relation for very low-mass M dwarf stars
    The stellar parameters are derived by requiring consistency with MIST models at every MCMC step (Methods, Global Analysis). A systematic failure of these models for M dwarfs would bias the stellar mass and radius used in the central claim.
  • domain assumption The radial velocity variations arise from a Keplerian orbit rather than stellar activity or an unseen companion
    A Keplerian orbit is assumed in the RV fit (Methods, Global Analysis). Activity indicators (bisector span, H alpha, log R'HK) show no significant correlation, supporting the assumption, but it is not independently proven.
  • domain assumption The interior retrieval models of Thorngren et al. (2016, 2019) reliably convert mass and radius into a metal mass fraction
    The reported metal content (12±2 M_earth) is derived from the warm-giant retrieval framework of Thorngren & Fortney (2019). The quoted uncertainty is statistical only and does not include systematic model uncertainty.
  • domain assumption The many vetting observations are sufficient to rule out any blended eclipsing binary scenario
    The blend analysis yields Delta chi^2 = 1600 against blended binaries, but it relies on MIST models for hypothetical companions and on the completeness of archival and speckle searches (Methods, Blend Analysis, Archival Imaging, High Contrast Imaging).

how reviews work

0 comments
Cite this review

Pith. "Pith review of A transiting giant planet in orbit around a 0.2-solar-mass host star." pith.science (2026). https://pith.science/paper/75XEXWD3

@misc{pith2026250607931,
  author       = {Pith},
  title        = {Pith review of: A transiting giant planet in orbit around a 0.2-solar-mass host star},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/75XEXWD3}},
  note         = {Machine review of arXiv:2506.07931}
}
abstract

Planet formation models suggest that the formation of giant planets is significantly harder around low-mass stars, due to the scaling of protoplanetary disc masses with stellar mass. The discovery of giant planets orbiting such low-mass stars thus imposes strong constraints on giant planet formation processes. Here, we report the discovery of a transiting giant planet orbiting a $0.207 \pm 0.011 M_{\odot}$ star. The planet, TOI-6894 b, has a mass and radius of $M_P = 0.168 \pm 0.022 M_J (53.4 \pm 7.1 M_{\oplus})$ and $R_P = 0.855 \pm 0.022 R_J$, and likely includes $12 \pm 2 M_{\oplus}$ of metals. The discovery of TOI-6894 b highlights the need for a better understanding of giant planet formation mechanisms and the protoplanetary disc environments in which they occur. The extremely deep transits (17% depth) make TOI-6894 b one of the most accessible exoplanetary giants for atmospheric characterisation observations, which will be key for fully interpreting the formation history of this remarkable system and for the study of atmospheric methane chemistry.

Figures

Figures reproduced from arXiv: 2506.07931 by the authors.

Figure 1
Figure 1. Observational data and best-fitting models (black line in all panels). a. Phase-folded TESS photometric data at a cadence of 30-min (left), 10-min (middle), and 2-min (right) (blue points). b. Phase￾folded RV data from ESPRESSO (orange triangles) and SPIRou (cyan squares). c. Selected ground-based follow-up photometric data. The panel annotations give the night on which the observations were taken, the facility that… view at source ↗
Figure 2
Figure 2. Placing TOI-6894 b in the context of known transiting planets. a Masses or minimum masses of the known population of planets discovered through the transit or radial velocity method as a function of mass of the host star (data taken from the NASA Exoplanet Archive, accessed 16 May 2024). We plot transiting planets for which we have an absolute mass measurement as the blue circles and the non-transiting RV planets fo… view at source ↗
Figure 3
Figure 3. Atmospheric characterisation potential of TOI-6894 b. We plot the Transmission Spectroscopy Metric (TSM; see 61, for more details) – a metric which provides an estimate of the expected signal-to-noise for transmission spectroscopy observations – of known giant planets as a function of the planetary equilibrium temperature. The colour of the points denotes the effective temperature of the host star and the star symbo… view at source ↗
Figures from the paper (12 more)
Figure 1
Figure 1. Figure 1: TESS candidate detection TOI-6894 was included in a systematic transit search for giant planets with low-mass host stars in the TESS primary mission FFI data (13). In short, this search detected periodic transit-like signals [PITH_FULL_IMAGE:figures/full_fig_p015_1.png]
Figure 4
Figure 4. Figure 4: Extended Data Figure 1 [PITH_FULL_IMAGE:figures/full_fig_p029_4.png]
Figure 5
Figure 5. Figure 5: Extended Data Figure 2 [PITH_FULL_IMAGE:figures/full_fig_p030_5.png]
Figure 6
Figure 6. Figure 6: Extended Data Figure 3 [PITH_FULL_IMAGE:figures/full_fig_p031_6.png]
Figure 7
Figure 7. Figure 7: Extended Data Figure 4 [PITH_FULL_IMAGE:figures/full_fig_p031_7.png]
Figure 8
Figure 8. Figure 8: Extended Data Figure 5 [PITH_FULL_IMAGE:figures/full_fig_p032_8.png]
Figure 9
Figure 9. Figure 9: Extended data Figure 6 [PITH_FULL_IMAGE:figures/full_fig_p032_9.png]
Figure 10
Figure 10. Figure 10: Extended Data Figure 7 [PITH_FULL_IMAGE:figures/full_fig_p033_10.png]
Figure 11
Figure 11. Figure 11: Extended Data Figure 8 [PITH_FULL_IMAGE:figures/full_fig_p033_11.png]
Figure 12
Figure 12. Figure 12: Supplementary Figure 1 [PITH_FULL_IMAGE:figures/full_fig_p036_12.png]
Figure 13
Figure 13. Figure 13: Supplementary Figure 2 [PITH_FULL_IMAGE:figures/full_fig_p037_13.png]
Figure 14
Figure 14. Figure 14: Supplementary Figure 3 [PITH_FULL_IMAGE:figures/full_fig_p038_14.png]

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

129 extracted references · 10 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]

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

    ENTRY address archive author booktitle chapter doi edition editor eid eprint howpublished institution journal key keywords month note number organization pages publisher school series title type url volume year archivePrefix primaryClass adsurl adsnote version label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sent...

  4. [4]

    write newline

    " write newline "" before.all 'output.state := FUNCTION add.period duplicate empty 'skip "." * add.blank if FUNCTION if.digit duplicate "0" = swap duplicate "1" = swap duplicate "2" = swap duplicate "3" = swap duplicate "4" = swap duplicate "5" = swap duplicate "6" = swap duplicate "7" = swap duplicate "8" = swap "9" = or or or or or or or or or FUNCTION ...

  5. [5]

    635:A128

    Aller A, Lillo-Box J, Jones D, et al (2020) Planetary nebulae seen with TESS: Discovery of new binary central star candidates from Cycle 1 . 635:A128. doi:10.1051/0004-6361/201937118 [astro-ph.SR]

    doi:10.1051/0004-6361/201937118 2020

  6. [6]

    Antoniadis-Karnavas A, Sousa SG, Delgado-Mena E, et al (2020) ODUSSEAS: a machine learning tool to derive effective temperature and metallicity for M dwarf stars . 636:A9. doi:10.1051/0004-6361/201937194 [astro-ph.SR]

    doi:10.1051/0004-6361/201937194 2020

  7. [7]

    164(3):84

    Artigau \'E , Cadieux C, Cook NJ, et al (2022) Line-by-line Velocity Measurements: an Outlier-resistant Method for Precision Velocimetry . 164(3):84. doi:10.3847/1538-3881/ac7ce6 [astro-ph.IM]

    doi:10.3847/1538-3881/ac7ce6 2022

  8. [8]

    935(2):167

    Astropy Collaboration , Price-Whelan AM, Lim PL, et al (2022) The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package . 935(2):167. doi:10.3847/1538-4357/ac7c74 [astro-ph.IM]

    doi:10.3847/1538-4357/ac7c74 2022

Show all 129 references
  1. [9]

    159(6):267

    Bakos G \'A , Bayliss D, Bento J, et al (2020) HATS-71b: A Giant Planet Transiting an M3 Dwarf Star in TESS Sector 1 . 159(6):267. doi:10.3847/1538-3881/ab8ad1

    2020 doi

  2. [10]

    623(7988):709--712

    Bell TJ, Welbanks L, Schlawin E, et al (2023) Methane throughout the atmosphere of the warm exoplanet WASP-80b . 623(7988):709--712. doi:10.1038/s41586-023-06687-0 [astro-ph.EP]

    2023 doi

  3. [11]

    523(4):6282--6292

    Bloot S, Miguel Y, Bazot M, et al (2023) Exoplanet interior retrievals: core masses and metallicities from atmospheric abundances . 523(4):6282--6292. doi:10.1093/mnras/stad1873 [astro-ph.EP]

    2023 doi

  4. [12]

    In: Shaklan S (ed) Techniques and Instrumentation for Detection of Exoplanets VII, p 96051L, doi:10.1117/12.2186999

    Bonfils X, Almenara JM, Jocou L, et al (2015) ExTrA: Exoplanets in transit and their atmospheres . In: Shaklan S (ed) Techniques and Instrumentation for Detection of Exoplanets VII, p 96051L, doi:10.1117/12.2186999

    2015 doi

  5. [13]

    Borisov SB, Chilingarian IV, Rubtsov EV, et al (2023) New generation stellar spectral libraries in the optical and near-infrared. i. the recalibrated uves-pop library for stellar population synthesis. 266(1):11. doi:10.3847/1538-4365/acc321 [astro-ph.IM]

    2023 doi

  6. [14]

    Science 276:1836--1839

    Boss AP (1997) Giant planet formation by gravitational instability. Science 276:1836--1839. doi:10.1126/science.276.5320.1836

    1997

  7. [15]

    956(1):4

    Boss AP, Kanodia S (2023) Forming Gas Giants around a Range of Protostellar M-dwarfs by Gas Disk Gravitational Instability . 956(1):4. doi:10.3847/1538-4357/acf373 [astro-ph.EP]

    2023 doi

  8. [16]

    125:1031

    Brown TM, Baliber N, Bianco FB, et al (2013) Las Cumbres Observatory Global Telescope Network . 125:1031. doi:10.1086/673168 [astro-ph.IM]

    2013 doi

  9. [17]

    doi:10.1093/mnras/stad626 [astro-ph.EP]

    Bryant EM, Bayliss D, Van Eylen V (2023) The occurrence rate of giant planets orbiting low-mass stars with TESS . doi:10.1093/mnras/stad626 [astro-ph.EP]

    2023 doi

  10. [18]

    134(1040):105001

    Burdanov AY, de Wit J, Gillon M, et al (2022) SPECULOOS Northern Observatory: Searching for Red Worlds in the Northern Skies . 134(1040):105001. doi:10.1088/1538-3873/ac92a6 [astro-ph.IM]

    2022 doi

  11. [19]

    In: Astronomical Society of India Conference Series, pp 7--12

    Burgasser AJ, Splat Development Team (2017) The SpeX Prism Library Analysis Toolkit (SPLAT): A Data Curation Model . In: Astronomical Society of India Conference Series, pp 7--12

    2017

  12. [20]

    Burn R, Schlecker M, Mordasini C, et al (2021) The New Generation Planetary Population Synthesis (NGPPS). IV. Planetary systems around low-mass stars . 656:A72. doi:10.1051/0004-6361/202140390 [astro-ph.EP]

    2021 doi

  13. [21]

    164(3):96

    Cadieux C, Doyon R, Plotnykov M, et al (2022) TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf . 164(3):96. doi:10.3847/1538-3881/ac7cea [astro-ph.EP]

    2022 doi

  14. [22]

    Mikulski Archive for Space Telescopes doi:10.17909/t9-wpz1-8s54

    Caldwell DA, Jenkins JM, Ting EB (2020 a ) TESS Light Curves From Full Frame Images (TESS-SPOC) . Mikulski Archive for Space Telescopes doi:10.17909/t9-wpz1-8s54

    2020 doi

  15. [23]

    Research Notes of the American Astronomical Society 4(11):201

    Caldwell DA, Tenenbaum P, Twicken JD, et al (2020 b ) TESS Science Processing Operations Center FFI Target List Products . Research Notes of the American Astronomical Society 4(11):201. doi:10.3847/2515-5172/abc9b3 [astro-ph.EP]

    2020 doi

  16. [24]

    952(1):L20

    Chachan Y, Lee EJ (2023) Small Planets around Cool Dwarfs: Enhanced Formation Efficiency of Super-Earths around M Dwarfs . 952(1):L20. doi:10.3847/2041-8213/ace257 [astro-ph.EP]

    2023 doi

  17. [25]

    In: Ballester P, Ibsen J, Solar M, et al (eds) Astronomical Data Analysis Software and Systems XXVII, p 623

    Chilingarian I (2020) Quick and accurate data reduction for intermediate-resolution echelle spectrographs at magellan. In: Ballester P, Ibsen J, Solar M, et al (eds) Astronomical Data Analysis Software and Systems XXVII, p 623

    2020

  18. [26]

    Choi J, Dotter A, Conroy C, et al (2016) Mesa Isochrones and Stellar Tracks (MIST). I. Solar-scaled Models . 823(2):102. doi:10.3847/0004-637X/823/2/102 [astro-ph.SR]

    2016 doi

  19. [27]

    495(1):962--970

    Chouqar J, Benkhaldoun Z, Jabiri A, et al (2020) Properties of sub-neptune atmospheres: Toi-270 system. 495(1):962--970

    2020

  20. [28]

    Claret A (2018) A new method to compute limb-darkening coefficients for stellar atmosphere models with spherical symmetry: the space missions TESS, Kepler, CoRoT, and MOST . 618:A20. doi:10.1051/0004-6361/201833060 [astro-ph.SR]

    2018 doi

  21. [29]

    Claret A, Hauschildt PH, Witte S (2012) New limb-darkening coefficients for PHOENIX/1D model atmospheres. I. Calculations for 1500 K T _ eff 4800 K Kepler, CoRot, Spitzer, uvby, UBVRIJHK, Sloan, and 2MASS photometric systems . 546:A14. doi:10.1051/0004-6361/201219849

    2012 doi

  22. [30]

    Claret A, Hauschildt PH, Witte S (2013) New limb-darkening coefficients for Phoenix/1d model atmospheres. II. Calculations for 5000 K T _ eff 10 000 K Kepler, CoRot, Spitzer, uvby, UBVRIJHK, Sloan, and 2MASS photometric systems . 552:A16. doi:10.1051/0004-6361/201220942

    2013 doi

  23. [31]

    Collins KA, Kielkopf JF, Stassun KG, et al (2017) AstroImageJ: Image Processing and Photometric Extraction for Ultra-precise Astronomical Light Curves . 153:77. doi:10.3847/1538-3881/153/2/77 [astro-ph.IM]

    2017 doi

  24. [32]

    134(1041):114509

    Cook NJ, Artigau \'E , Doyon R, et al (2022) APERO: A PipelinE to Reduce Observations-Demonstration with SPIRou . 134(1041):114509. doi:10.1088/1538-3873/ac9e74 [astro-ph.IM]

    2022 doi

  25. [33]

    623(2):1115--1140

    Cushing MC, Rayner JT, Vacca WD (2005) An Infrared Spectroscopic Sequence of M, L, and T Dwarfs . 623(2):1115--1140. doi:10.1086/428040 [astro-ph]

    2005 doi

  26. [34]

    In: Marshall HK, Spyromilio J (eds) Ground-based and Airborne Telescopes VII, International Society for Optics and Photonics, vol 10700

    Delrez L, Gillon M, Queloz D, et al (2018) SPECULOOS: a network of robotic telescopes to hunt for terrestrial planets around the nearest ultracool dwarfs . In: Marshall HK, Spyromilio J (eds) Ground-based and Airborne Telescopes VII, International Society for Optics and Photon...

    2018 doi

  27. [35]

    Delrez L, Murray CA, Pozuelos FJ, et al (2022) Two temperate super-Earths transiting a nearby late-type M dwarf . 667:A59. doi:10.1051/0004-6361/202244041 [astro-ph.EP]

    2022 doi

  28. [36]

    Demory BO, Pozuelos FJ, G \'o mez Maqueo Chew Y, et al (2020) A super-Earth and a sub-Neptune orbiting the bright, quiet M3 dwarf TOI-1266 . 642:A49. doi:10.1051/0004-6361/202038616 [astro-ph.EP]

    2020 doi

  29. [37]

    Astrophysics Source Code Library, record ascl:2309.007

    D \'e vora-Pajares M, Pozuelos FJ (2023) MATRIX: Multi-phAse Transits Recovery from Injected eXoplanets toolkit . Astrophysics Source Code Library, record ascl:2309.007

    2023

  30. [38]

    532(4):4752--4773

    D \'e vora-Pajares M, Pozuelos FJ, Thuillier A, et al (2024) The SHERLOCK pipeline: new exoplanet candidates in the WASP-16, HAT-P-27, HAT-P-26, and TOI-2411 systems . 532(4):4752--4773. doi:10.1093/mnras/stae1740 [astro-ph.EP]

    2024 doi

  31. [39]

    498(4):5684--5703

    Donati JF, Kouach D, Moutou C, et al (2020) SPIRou: NIR velocimetry and spectropolarimetry at the CFHT . 498(4):5684--5703. doi:10.1093/mnras/staa2569 [astro-ph.IM]

    2020 doi

  32. [40]

    222(1):8

    Dotter A (2016) MESA Isochrones and Stellar Tracks (MIST) 0: Methods for the Construction of Stellar Isochrones . 222(1):8. doi:10.3847/0067-0049/222/1/8 [astro-ph.SR]

    2016 doi

  33. [41]

    Monthly Notices of the Royal Astronomical Society 474(4):5036--5048

    Forgan DH, Hall C, Meru F, et al (2017) Towards a population synthesis model of self-gravitating disc fragmentation and tidal downsizing II: the effect of fragment–fragment interactions . Monthly Notices of the Royal Astronomical Society 474(4):5036--5048

    2017

  34. [42]

    160(6):288

    Fortney JJ, Visscher C, Marley MS, et al (2020) Beyond Equilibrium Temperature: How the Atmosphere/Interior Connection Affects the Onset of Methane, Ammonia, and Clouds in Warm Transiting Giant Planets . 160(6):288. doi:10.3847/1538-3881/abc5bd [astro-ph.EP]

    2020 doi

  35. [43]

    The ESO Reflex environment

    Freudling W, Romaniello M, Bramich DM, et al (2013) Automated data reduction workflows for astronomy. The ESO Reflex environment . 559:A96. doi:10.1051/0004-6361/201322494 [astro-ph.IM]

    2013 doi

  36. [44]

    Summary of the contents and survey properties

    Gaia Collaboration , Brown AGA, Vallenari A, et al (2021) Gaia Early Data Release 3. Summary of the contents and survey properties . 649:A1. doi:10.1051/0004-6361/202039657 [astro-ph.GA]

    2021 doi

  37. [45]

    514(3):4120--4139

    Gan T, Soubkiou A, Wang SX, et al (2022) TESS discovery of a sub-Neptune orbiting a mid-M dwarf TOI-2136 . 514(3):4120--4139. doi:10.1093/mnras/stac1448 [astro-ph.EP]

    2022 doi

  38. [46]

    166(4):165

    Gan T, Cadieux C, Jahandar F, et al (2023 a ) A Massive Hot Jupiter Orbiting a Metal-rich Early M Star Discovered in the TESS Full-frame Images . 166(4):165. doi:10.3847/1538-3881/acf56d [astro-ph.EP]

    2023 doi

  39. [47]

    165(1):17

    Gan T, Wang SX, Wang S, et al (2023 b ) Occurrence Rate of Hot Jupiters Around Early-type M Dwarfs Based on Transiting Exoplanet Survey Satellite Data . 165(1):17. doi:10.3847/1538-3881/ac9b12 [astro-ph.EP]

    2023 doi

  40. [48]

    509(4):4817--4828

    Garcia LJ, Timmermans M, Pozuelos FJ, et al (2022) PROSE: a PYTHON framework for modular astronomical images processing . 509(4):4817--4828. doi:10.1093/mnras/stab3113 [astro-ph.IM]

    2022 doi

  41. [49]

    EPJ Web of Conferences 11:06002

    Gillon M, Jehin E, Magain P, et al (2011) TRAPPIST : a robotic telescope dedicated to the study of planetary systems. EPJ Web of Conferences 11:06002. doi:10.1051/epjconf/20101106002

    2011

  42. [50]

    The Journal of Open Source Software 3(31):667

    Gomes da Silva J, Figueira P, Santos N, et al (2018) ACTIN: A tool to calculate stellar activity indices . The Journal of Open Source Software 3(31):667. doi:10.21105/joss.00667 [astro-ph.IM]

    2018 doi

  43. [51]

    Gomes da Silva J, Santos NC, Adibekyan V, et al (2021) Stellar chromospheric activity of 1674 FGK stars from the AMBRE-HARPS sample. I. A catalogue of homogeneous chromospheric activity . 646:A77. doi:10.1051/0004-6361/202039765 [astro-ph.SR]

    2021 doi

  44. [52]

    157(2):55

    Hartman JD, Bakos G \'A , Bayliss D, et al (2019) HATS-60b-HATS-69b: 10 Transiting Planets from HATSouth . 157(2):55. doi:10.3847/1538-3881/aaf8b6 [astro-ph.EP]

    2019 doi

  45. [53]

    166(4):163

    Hartman JD, Bakos G \'A , Csubry Z, et al (2023) TOI 4201 b and TOI 5344 b: Discovery of Two Transiting Giant Planets around M-dwarf Stars and Revised Parameters for Three Others . 166(4):163. doi:10.3847/1538-3881/acf56e [astro-ph.EP]

    2023 doi

  46. [54]

    doi:10.1051/0004-6361/202346850 [astro-ph.EP]

    Helled R (2023) The mass of gas giant planets: Is Saturn a failed gas giant? 675:L8. doi:10.1051/0004-6361/202346850 [astro-ph.EP]

    2023 doi

  47. [55]

    185(1):64--71

    Helled R, Podolak M, Kovetz A (2006) Planetesimal capture in the disk instability model . 185(1):64--71. doi:10.1016/j.icarus.2006.06.011 [astro-ph]

    2006 doi

  48. [56]

    142(1):19

    Howell SB, Everett ME, Sherry W, et al (2011) Speckle Camera Observations for the NASA Kepler Mission Follow-up Program . 142(1):19. doi:10.1088/0004-6256/142/1/19

    2011 doi

  49. [57]

    Ida S, Lin DNC (2005) Toward a Deterministic Model of Planetary Formation. III. Mass Distribution of Short-Period Planets around Stars of Various Masses . 626(2):1045--1060. doi:10.1086/429953 [astro-ph]

    2005 doi

  50. [58]

    The Messenger 145:2--6

    Jehin E, Gillon M, Queloz D, et al (2011) TRAPPIST: TRAnsiting Planets and PlanetesImals Small Telescope . The Messenger 145:2--6

    2011

  51. [59]

    The Messenger 174:2--7

    Jehin E, Gillon M, Queloz D, et al (2018) The SPECULOOS Southern Observatory Begins its Hunt for Rocky Planets . The Messenger 174:2--7. doi:10.18727/0722-6691/5105

    2018 doi

  52. [60]

    575:493--505

    Jenkins JM (2002) The Impact of Solar-like Variability on the Detectability of Transiting Terrestrial Planets . 575:493--505. doi:10.1086/341136

    2002 doi

  53. [61]

    In: Radziwill NM, Bridger A (eds) Software and Cyberinfrastructure for Astronomy, p 77400D, doi:10.1117/12.856764

    Jenkins JM, Chandrasekaran H, McCauliff SD, et al (2010) Transiting planet search in the Kepler pipeline . In: Radziwill NM, Bridger A (eds) Software and Cyberinfrastructure for Astronomy, p 77400D, doi:10.1117/12.856764

    2010 doi

  54. [62]

    In: Chiozzi G, Guzman JC (eds) Software and Cyberinfrastructure for Astronomy IV, p 99133E, doi:10.1117/12.2233418

    Jenkins JM, Twicken JD, McCauliff S, et al (2016) The TESS science processing operations center . In: Chiozzi G, Guzman JC (eds) Software and Cyberinfrastructure for Astronomy IV, p 99133E, doi:10.1117/12.2233418

    2016 doi

  55. [63]

    Kepler Science Document KSCI-19081-003

    Jenkins JM, Tenenbaum P, Seader S, et al (2020) Kepler Data Processing Handbook: Transiting Planet Search . Kepler Science Document KSCI-19081-003

    2020

  56. [64]

    165(3):120

    Kanodia S, Mahadevan S, Libby-Roberts J, et al (2023) TOI-5205b: A Short-period Jovian Planet Transiting a Mid-M Dwarf . 165(3):120. doi:10.3847/1538-3881/acabce [astro-ph.EP]

    2023 doi

  57. [65]

    130(993):114401

    Kempton EMR, Bean JL, Louie DR, et al (2018) A Framework for Prioritizing the TESS Planetary Candidates Most Amenable to Atmospheric Characterization . 130(993):114401. doi:10.1088/1538-3873/aadf6f [astro-ph.EP]

    2018 doi

  58. [66]

    670:A136

    Kiefer F, H \'e brard G, Martioli E, et al (2023) A sub-Neptune planet around TOI-1695 discovered and characterized with SPIRou and TESS . 670:A136. doi:10.1051/0004-6361/202245129 [astro-ph.EP]

    2023 doi

  59. [67]

    391:369--377

    Kov \'a cs G, Zucker S, Mazeh T (2002) A box-fitting algorithm in the search for periodic transits . 391:369--377. doi:10.1051/0004-6361:20020802 [astro-ph]

    2002 doi

  60. [68]

    612(1):L73--L76

    Laughlin G, Bodenheimer P, Adams FC (2004) The Core Accretion Model Predicts Few Jovian-Mass Planets Orbiting Red Dwarfs . 612(1):L73--L76. doi:10.1086/424384 [astro-ph]

    2004 doi

  61. [69]

    642:A121

    Lillo-Box J, Figueira P, Leleu A, et al (2020) Planetary system LHS 1140 revisited with ESPRESSO and TESS . 642:A121. doi:10.1051/0004-6361/202038922 [astro-ph.EP]

    2020 doi

  62. [70]

    480(4):4338--4354

    Lin JW, Lee EJ, Chiang E (2018) A balanced budget view on forming giant planets by pebble accretion . 480(4):4338--4354. doi:10.1093/mnras/sty2159 [astro-ph.EP]

    2018 doi

  63. [71]

    Liu B, Lambrechts M, Johansen A, et al (2019) Super-Earth masses sculpted by pebble isolation around stars of different masses . 632:A7. doi:10.1051/0004-6361/201936309 [astro-ph.EP]

    2019 doi

  64. [72]

    668:A175

    Liu Y, Linz H, Fang M, et al (2022) Underestimation of the dust mass in protoplanetary disks: Effects of disk structure and dust properties . 668:A175. doi:10.1051/0004-6361/202244505 [astro-ph.EP]

    2022 doi

  65. [73]

    160(6):273

    Lopez-Santiago J, Martino L, M \' guez J, et al (2020) A Likely Magnetic Activity Cycle for the Exoplanet Host M Dwarf GJ 3512 . 160(6):273. doi:10.3847/1538-3881/abc171 [astro-ph.EP]

    2020 doi

  66. [74]

    158(1):27

    Lustig-Yaeger J, Meadows VS, Lincowski AP (2019) The detectability and characterization of the trappist-1 exoplanet atmospheres with jwst. 158(1):27

    2019

  67. [75]

    In: Inutsuka S, Aikawa Y, Muto T, et al (eds) Protostars and Planets VII, p 539, doi:10.48550/arXiv.2203.09930

    Manara CF, Ansdell M, Rosotti GP, et al (2023) Demographics of Young Stars and their Protoplanetary Disks: Lessons Learned on Disk Evolution and its Connection to Planet Formation . In: Inutsuka S, Aikawa Y, Muto T, et al (eds) Protostars and Planets VII, p 539, doi:10.48550/a...

    2023 doi arXiv

  68. [76]

    580(2):L171--L175

    Mandel K, Agol E (2002) Analytic Light Curves for Planetary Transit Searches . 580(2):L171--L175. doi:10.1086/345520 [astro-ph]

    2002 doi

  69. [77]

    147(6):160

    Mann AW, Deacon NR, Gaidos E, et al (2014) Prospecting in Ultracool Dwarfs: Measuring the Metallicities of Mid- and Late-M Dwarfs . 147(6):160. doi:10.1088/0004-6256/147/6/160 [astro-ph.SR]

    2014 doi

  70. [78]

    804(1):64

    Mann AW, Feiden GA, Gaidos E, et al (2015) How to constrain your m dwarf: Measuring effective temperature, bolometric luminosity, mass, and radius. 804(1):64. doi:10.1088/0004-637X/804/1/64

    2015 doi

  71. [79]

    Mann AW, Dupuy T, Kraus AL, et al (2019) How to Constrain Your M Dwarf. II. The Mass-Luminosity-Metallicity Relation from 0.075 to 0.70 Solar Masses . 871(1):63. doi:10.3847/1538-4357/aaf3bc [astro-ph.SR]

    2019 doi

  72. [80]

    Martioli E, H \'e brard G, Fouqu \'e P, et al (2022) TOI-1759 b: A transiting sub-Neptune around a low mass star characterized with SPIRou and TESS . 660:A86. doi:10.1051/0004-6361/202142540 [astro-ph.EP]

    2022 doi

  73. [81]

    In: Software and Cyberinfrastructure for Astronomy V, p 107070K, doi:10.1117/12.2314340

    McCully C, Volgenau NH, Harbeck DR, et al (2018) Real-time processing of the imaging data from the network of Las Cumbres Observatory Telescopes using BANZAI . In: Software and Cyberinfrastructure for Astronomy V, p 107070K, doi:10.1117/12.2314340

    2018 doi

  74. [82]

    Fragmentation conditions and protoplanet properties

    Mercer A, Stamatellos D (2020) Planet formation around M dwarfs via disc instability. Fragmentation conditions and protoplanet properties . 633:A116. doi:10.1051/0004-6361/201936954 [astro-ph.SR]

    2020 doi

  75. [83]

    491(2):1998--2009

    Miguel Y, Cridland A, Ormel CW, et al (2020) Diverse outcomes of planet formation and composition around low-mass stars and brown dwarfs . 491(2):1998--2009. doi:10.1093/mnras/stz3007 [astro-ph.EP]

    2020 doi

  76. [84]

    In: Pizzo R, Deul ER, Mol JD, et al (eds) Astronomical Data Analysis Software and Systems XXIX, p 667

    Modigliani A, Freudling W, Anderson RI, et al (2020) The EsoReflex Workflow to Reduce ESPRESSO Data . In: Pizzo R, Deul ER, Mol JD, et al (eds) Astronomical Data Analysis Software and Systems XXIX, p 667

    2020

  77. [85]

    Science 365(6460):1441--1445

    Morales JC, Mustill AJ, Ribas I, et al (2019) A giant exoplanet orbiting a very-low-mass star challenges planet formation models . Science 365(6460):1441--1445. doi:10.1126/science.aax3198 [astro-ph.EP]

    2019 doi

  78. [86]

    850(2):121

    Morley CV, Kreidberg L, Rustamkulov Z, et al (2017) Observing the atmospheres of known temperate earth-sized planets with jwst. 850(2):121

    2017

  79. [87]

    doi:10.3847/2041-8213/ac2947 [astro-ph.EP]

    Mulders GD, Dr a \.z kowska J, van der Marel N, et al (2021) Why Do M Dwarfs Have More Transiting Planets? 920(1):L1. doi:10.3847/2041-8213/ac2947 [astro-ph.EP]

    2021 doi

  80. [88]

    Journal of Astronomical Telescopes, Instruments, and Systems 5:015001

    Narita N, Fukui A, Kusakabe N, et al (2019) MuSCAT2: four-color simultaneous camera for the 1.52-m Telescopio Carlos S \'a nchez . Journal of Astronomical Telescopes, Instruments, and Systems 5:015001. doi:10.1117/1.JATIS.5.1.015001 [astro-ph.IM]

    2019 doi

  81. [89]

    Research Notes of the American Astronomical Society 6(10):207

    Nguyen KT, Caldwell DA, Twicken JD, et al (2022) Release of TESS Objects of Interest from TESS-SPOC Sectors 48 to 50 Full Frame Images . Research Notes of the American Astronomical Society 6(10):207. doi:10.3847/2515-5172/ac983a

    2022 doi

  82. [90]

    477(3):3273--3278

    Nixon CJ, King AR, Pringle JE (2018) The Maximum Mass Solar Nebula and the early formation of planets . 477(3):3273--3278. doi:10.1093/mnras/sty593 [astro-ph.EP]

    2018 doi

  83. [91]

    Noll S, Kausch W, Kimeswenger S, et al (2014) Skycorr: A general tool for spectroscopic sky subtraction. 567:A25. doi:10.1051/0004-6361/201423908 [astro-ph.IM]

    2014 doi

  84. [92]

    Parviainen H, Palle E, Zapatero-Osorio MR, et al (2020) MuSCAT2 multicolour validation of TESS candidates: an ultra-short-period substellar object around an M dwarf . 633:A28. doi:10.1051/0004-6361/201935958 [astro-ph.EP]

    2020 doi

  85. [93]

    831(2):125

    Pascucci I, Testi L, Herczeg GJ, et al (2016) A Steeper than Linear Disk Mass-Stellar Mass Scaling Relation . 831(2):125. doi:10.3847/0004-637X/831/2/125 [astro-ph.EP]

    2016 doi

  86. [94]

    166(1):11

    Pass EK, Winters JG, Charbonneau D, et al (2023) Mid-to-late M Dwarfs Lack Jupiter Analogs . 166(1):11. doi:10.3847/1538-3881/acd349 [astro-ph.EP]

    2023 doi

  87. [95]

    192(1):3

    Paxton B, Bildsten L, Dotter A, et al (2011) Modules for Experiments in Stellar Astrophysics (MESA) . 192(1):3. doi:10.1088/0067-0049/192/1/3 [astro-ph.SR]

    2011 doi

  88. [96]

    208(1):4

    Paxton B, Cantiello M, Arras P, et al (2013) Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars . 208(1):4. doi:10.1088/0067-0049/208/1/4 [astro-ph.SR]

    2013 doi

  89. [97]

    220(1):15

    Paxton B, Marchant P, Schwab J, et al (2015) Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions . 220(1):15. doi:10.1088/0067-0049/220/1/15 [astro-ph.SR]

    2015 doi

  90. [98]

    On-sky performance and first results

    Pepe F, Cristiani S, Rebolo R, et al (2021) ESPRESSO at VLT. On-sky performance and first results . 645:A96. doi:10.1051/0004-6361/202038306 [astro-ph.IM]

    2021 doi

  91. [99]

    124(1):62--85

    Pollack JB, Hubickyj O, Bodenheimer P, et al (1996) Formation of the Giant Planets by Concurrent Accretion of Solids and Gas . 124(1):62--85. doi:10.1006/icar.1996.0190

    1996

  92. [100]

    Pozuelos FJ, Su \'a rez JC, de El \' a GC, et al (2020) GJ 273: on the formation, dynamical evolution, and habitability of a planetary system hosted by an M dwarf at 3.75 parsec . 641:A23. doi:10.1051/0004-6361/202038047 [astro-ph.EP]

    2020 doi

  93. [101]

    Pozuelos FJ, Timmermans M, Rackham BV, et al (2023) A super-Earth and a mini-Neptune near the 2:1 MMR straddling the radius valley around the nearby mid-M dwarf TOI-2096 . 672:A70. doi:10.1051/0004-6361/202245440 [astro-ph.EP]

    2023 doi

  94. [102]

    Two Saturn-mass planets orbiting active stars

    Quirrenbach A, Passegger VM, Trifonov T, et al (2022) The CARMENES search for exoplanets around M dwarfs. Two Saturn-mass planets orbiting active stars . 663:A48. doi:10.1051/0004-6361/202142915 [astro-ph.EP]

    2022 doi

  95. [103]

    185(2):289--432

    Rayner JT, Cushing MC, Vacca WD (2009) The Infrared Telescope Facility (IRTF) Spectral Library: Cool Stars . 185(2):289--432. doi:10.1088/0067-0049/185/2/289 [astro-ph.SR]

    2009 doi

  96. [104]

    Journal of Astronomical Telescopes, Instruments, and Systems 1:014003

    Ricker GR, Winn JN, Vanderspek R, et al (2015) Transiting Exoplanet Survey Satellite (TESS) . Journal of Astronomical Telescopes, Instruments, and Systems 1:014003. doi:10.1117/1.JATIS.1.1.014003

    2015 doi

  97. [105]

    748(2):93

    Rojas-Ayala B, Covey KR, Muirhead PS, et al (2012) Metallicity and Temperature Indicators in M Dwarf K-band Spectra: Testing New and Updated Calibrations with Observations of 133 Solar Neighborhood M Dwarfs . 748(2):93. doi:10.1088/0004-637X/748/2/93 [astro-ph.SR]

    2012 doi

  98. [106]

    614(7949):659--663

    Rustamkulov Z, Sing DK, Mukherjee S, et al (2023) Early Release Science of the exoplanet WASP-39b with JWST NIRSpec PRISM . 614(7949):659--663. doi:10.1038/s41586-022-05677-y [astro-ph.EP]

    2023 doi

  99. [107]

    Planet occurrence rates from a subsample of 71 stars

    Sabotta S, Schlecker M, Chaturvedi P, et al (2021) The CARMENES search for exoplanets around M dwarfs. Planet occurrence rates from a subsample of 71 stars . 653:A114. doi:10.1051/0004-6361/202140968 [astro-ph.EP]

    2021 doi

  100. [108]

    Frontiers in Astronomy and Space Sciences 8:138

    Scott NJ, Howell SB, Gnilka CL, et al (2021) Twin High-resolution, High-speed Imagers for the Gemini Telescopes: Instrument description and science verification results . Frontiers in Astronomy and Space Sciences 8:138. doi:10.3389/fspas.2021.716560

    2021

  101. [109]

    Target list and strategy

    Sebastian D, Gillon M, Ducrot E, et al (2021) SPECULOOS: Ultracool dwarf transit survey. Target list and strategy . 645:A100. doi:10.1051/0004-6361/202038827 [astro-ph.EP]

    2021 doi

  102. [110]

    549(7671):238--241

    Sedaghati E, Boffin HMJ, MacDonald RJ, et al (2017) Detection of titanium oxide in the atmosphere of a hot Jupiter . 549(7671):238--241. doi:10.1038/nature23651 [astro-ph.EP]

    2017 doi

  103. [111]

    125(925):270

    Simcoe RA, Burgasser AJ, Schechter PL, et al (2013) FIRE: A Facility Class Near-Infrared Echelle Spectrometer for the Magellan Telescopes . 125(925):270. doi:10.1086/670241

    2013 doi

  104. [112]

    131:1163--1183

    Skrutskie MF, Cutri RM, Stiening R, et al (2006) The Two Micron All Sky Survey (2MASS) . 131:1163--1183. doi:10.1086/498708

    2006 doi

  105. [113]

    124(919):1000

    Smith JC, Stumpe MC, Van Cleve JE, et al (2012) Kepler Presearch Data Conditioning II - A Bayesian Approach to Systematic Error Correction . 124(919):1000. doi:10.1086/667697 [astro-ph.IM]

    2012 doi

  106. [114]

    In: Taylor AR, Rosolowsky E (eds) Astronomical Data Analysis Software an Systems XXIV (ADASS XXIV), p 285, doi:10.48550/arXiv.1509.05584

    Sosnowska D, Lovis C, Figueira P, et al (2015) A Flexible and Modular Data Reduction Library for Fiber-fed Echelle Spectrographs . In: Taylor AR, Rosolowsky E (eds) Astronomical Data Analysis Software an Systems XXIV (ADASS XXIV), p 285, doi:10.48550/arXiv.1509.05584

    2015 doi arXiv

  107. [115]

    379(1):L11--L15

    Southworth J, Wheatley PJ, Sams G (2007) A method for the direct determination of the surface gravities of transiting extrasolar planets . 379(1):L11--L15. doi:10.1111/j.1745-3933.2007.00324.x [astro-ph]

    2007

  108. [116]

    158(4):138

    Stassun KG, Oelkers RJ, Paegert M, et al (2019) The Revised TESS Input Catalog and Candidate Target List . 158(4):138. doi:10.3847/1538-3881/ab3467 [astro-ph.SR]

    2019 doi

  109. [117]

    Science 382(6674):1031--1035

    Stef \'a nsson G, Mahadevan S, Miguel Y, et al (2023) A Neptune-mass exoplanet in close orbit around a very low-mass star challenges formation models . Science 382(6674):1031--1035. doi:10.1126/science.abo0233 [astro-ph.EP]

    2023 doi

  110. [118]

    124(919):985

    Stumpe MC, Smith JC, Van Cleve JE, et al (2012) Kepler Presearch Data Conditioning I Architecture and Algorithms for Error Correction in Kepler Light Curves . 124(919):985. doi:10.1086/667698 [astro-ph.IM]

    2012 doi

  111. [119]

    126(935):100

    Stumpe MC, Smith JC, Catanzarite JH, et al (2014) Multiscale Systematic Error Correction via Wavelet-Based Bandsplitting in Kepler Data . 126(935):100. doi:10.1086/674989

    2014 doi

  112. [120]

    874(2):L31

    Thorngren D, Fortney JJ (2019) Connecting Giant Planet Atmosphere and Interior Modeling: Constraints on Atmospheric Metal Enrichment . 874(2):L31. doi:10.3847/2041-8213/ab1137 [astro-ph.EP]

    2019 doi

  113. [121]

    831(1):64

    Thorngren DP, Fortney JJ, Murray-Clay RA, et al (2016) The Mass-Metallicity Relation for Giant Planets . 831(1):64. doi:10.3847/0004-637X/831/1/64 [astro-ph.EP]

    2016 doi

  114. [122]

    Research Notes of the American Astronomical Society 3(9):128

    Thorngren DP, Marley MS, Fortney JJ (2019) An Empirical Mass-Radius Relation for Cool Giant Planets . Research Notes of the American Astronomical Society 3(9):128. doi:10.3847/2515-5172/ab4353

    2019 doi

  115. [123]

    450(3):2279--2290

    Triaud AHMJ, Gillon M, Ehrenreich D, et al (2015) WASP-80b has a dayside within the T-dwarf range . 450(3):2279--2290. doi:10.1093/mnras/stv706 [astro-ph.EP]

    2015 doi

  116. [124]

    130(6):064502

    Twicken JD, Catanzarite JH, Clarke BD, et al (2018) Kepler Data Validation I Architecture, Diagnostic Tests, and Data Products for Vetting Transiting Planet Candidates . 130(6):064502. doi:10.1088/1538-3873/aab694 [astro-ph.EP]

    2018 doi

  117. [125]

    Tychoniec , Manara CF, Rosotti GP, et al (2020) Dust masses of young disks: constraining the initial solid reservoir for planet formation . 640:A19. doi:10.1051/0004-6361/202037851 [astro-ph.EP]

    2020 doi

  118. [126]

    160(4):155

    Wong I, Shporer A, Daylan T, et al (2020) Systematic Phase Curve Study of Known Transiting Systems from Year One of the TESS Mission . 160(4):155. doi:10.3847/1538-3881/ababad [astro-ph.EP]

    2020 doi

  119. [127]

    140:1868-1881

    Wright EL, Eisenhardt PRM, Mainzer AK, et al (2010) The Wide-field Infrared Survey Explorer (WISE): Mission Description and Initial On-orbit Performance . 140:1868-1881. doi:10.1088/0004-6256/140/6/1868 [astro-ph.IM]

    2010 doi

  120. [128]

    797(1):41

    Zahnle KJ, Marley MS (2014) Methane, Carbon Monoxide, and Ammonia in Brown Dwarfs and Self-Luminous Giant Planets . 797(1):41. doi:10.1088/0004-637X/797/1/41 [astro-ph.EP]

    2014 doi

  121. [129]

    High-precision radial velocities and two alternative spectral indicators

    Zechmeister M, Reiners A, Amado PJ, et al (2018) Spectrum radial velocity analyser (SERVAL). High-precision radial velocities and two alternative spectral indicators . 609:A12. doi:10.1051/0004-6361/201731483 [astro-ph.IM]

    2018 doi

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.