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arxiv: 2605.12324 · v1 · submitted 2026-05-12 · 🌌 astro-ph.EP

Recognition: 2 theorem links

· Lean Theorem

An Ultra-Short Period Super-Earth and a Sub-Neptune Orbiting the K dwarf TOI-4311

Yoshi Nike Emilia Eschen , Thomas G. Wilson , Andrew Collier Cameron , Alexander James Mustill , Jo Ann Egger , Sol\`ene Ulmer-Moll , Davide Gandolfi , Alexis M. S. Smith
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Olivier D. S. Demangeon S\'ergio G. Sousa Andrea Bonfanti Alexandre C. M. Correia Vardan Adibekyan Gaia Lacedelli Alexis Brandeker Camilla Pezzotti Babatunde Akinsanmi Yann Alibert Roi Alonso Tamas B\'arczy David Barrado Susana C. C. Barros Wolfgang Baumjohann Willy Benz Nicolas Billot Luca Borsato Christopher Broeg Amadeo Castro-Gonz\'alez Szilard Csizmadia Patricio E. Cubillos Melvyn B. Davies Magali Deleuil Adrien Deline Brice-Olivier Demory Aliz Derekas Giuseppe Di Persio Billy Edwards David Ehrenreich Anders Erikson Andrea Fortier Luca Fossati Malcolm Fridlund Kosmas Gazeas Micha\"el Gillon Manuel G\"udel Maximilian N. G\"unther Alexis Heitzmann Ch. Helling Kate G. Isaak Jon M. Jenkins Tatiana Keller Laszlo L. Kiss Daniel Kitzmann Judith Korth Kristine W. F. Lam Jacques Laskar Alain Lecavelier des Etangs Adrien Leleu Monika Lendl Demetrio Magrin Pierre F. L. Maxted Bruno Mer\'in Christoph Mordasini Valerio Nascimbeni G\"oran Olofsson Hugh P. Osborn Roland Ottensamer Isabella Pagano Enric Pall\'e Gisbert Peter Glen Petitpas Daniele Piazza Giampaolo Piotto Don Pollacco Didier Queloz Roberto Ragazzoni Nicola Rando Heike Rauer Ignasi Ribas Nuno C. Santos Gaetano Scandariato Damien S\'egransan Avi Shporer Andr\'e M. Silva Attila E. Simon Richard Southworth Manu Stalport Sophia Sulis Gyula M. Szab\'o St\'ephane Udry Bernd Ulmer Val\'erie Van Grootel Julia Venturini Eva Villaver Nicholas A. Walton Sebastian Wolf Carl Ziegler Tiziano Zingales
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Pith reviewed 2026-05-13 04:08 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanetssuper-EarthK dwarfplanet formationinterior modelinggalactic kinematicsTESSCHEOPS
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The pith

TOI-4311 b is a dense ultra-short-period super-Earth whose properties challenge planet formation theories given its host star's galactic kinematics.

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

Astronomers have found two planets around the K dwarf star TOI-4311: a super-Earth with an orbit of less than one day and a sub-Neptune with a 15-day period. Precise follow-up data give the inner planet a mass of 4.5 Earth masses and radius of 1.38 Earth radii. Modeling the planet's interior structure indicates unusually high density. The host star lies kinematically between the Galactic thick disk and Hercules stream, making this density stand out against expected compositions from the star's chemistry. This setup suggests that planet formation outcomes depend on galactic environment and may need new theoretical adjustments.

Core claim

The paper establishes that TOI-4311 hosts an ultra-short-period super-Earth (TOI-4311 b) with radius 1.376 R⊕ and mass 4.5 M⊕, along with a sub-Neptune (planet c) of radius 2.47 R⊕. Interior modeling of planet b reveals it to be very dense in the context of the host star's galactic kinematics between the thick disk and Hercules stream and its chemistry. This combination challenges current formation theories and offers potential insights into planet formation across different galactic populations.

What carries the argument

Interior structure modeling of the super-Earth TOI-4311 b based on its measured mass and radius, interpreted through the lens of the host star's galactic kinematics and chemistry.

If this is right

  • Planet formation models must be revised to include effects from galactic environment and stellar chemistry.
  • The potential third planet at 38 days remains dynamically stable in the system.
  • Observations of exoplanets around stars with similar kinematic properties could reveal similar density anomalies.
  • Insights from this system may explain variations in planetary compositions across the Milky Way.

Where Pith is reading between the lines

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

  • Stars in the thick disk may systematically produce denser planets than those in the thin disk due to differences in metallicity or formation history.
  • Future exoplanet surveys could prioritize targets based on galactic kinematics to search for such anomalies.
  • The third RV signal, if planetary, would add to the understanding of compact multi-planet systems around K dwarfs.

Load-bearing premise

That the interior structure model, when fed the measured mass and radius of TOI-4311 b, produces a density value that is meaningfully higher than expected specifically because of the host star's galactic kinematics and chemistry.

What would settle it

A refined mass measurement for TOI-4311 b that results in a lower density consistent with standard expectations for the star's chemistry, or a demonstration that the kinematic classification does not uniquely predict high density.

Figures

Figures reproduced from arXiv: 2605.12324 by Adrien Deline, Adrien Leleu, Alain Lecavelier des Etangs, Alexander James Mustill, Alexandre C. M. Correia, Alexis Brandeker, Alexis Heitzmann, Alexis M. S. Smith, Aliz Derekas, Amadeo Castro-Gonz\'alez, Anders Erikson, Andrea Bonfanti, Andrea Fortier, Andr\'e M. Silva, Andrew Collier Cameron, Attila E. Simon, Avi Shporer, Babatunde Akinsanmi, Bernd Ulmer, Billy Edwards, Brice-Olivier Demory, Bruno Mer\'in, Camilla Pezzotti, Carl Ziegler, Ch. Helling, Christopher Broeg, Christoph Mordasini, Damien S\'egransan, Daniele Piazza, Daniel Kitzmann, David Barrado, Davide Gandolfi, David Ehrenreich, Demetrio Magrin, Didier Queloz, Don Pollacco, Enric Pall\'e, Eva Villaver, Gaetano Scandariato, Gaia Lacedelli, Giampaolo Piotto, Gisbert Peter, Giuseppe Di Persio, Glen Petitpas, G\"oran Olofsson, Gyula M. Szab\'o, Heike Rauer, Hugh P. Osborn, Ignasi Ribas, Isabella Pagano, Jacques Laskar, Jo Ann Egger, Jon M. Jenkins, Judith Korth, Julia Venturini, Kate G. Isaak, Kosmas Gazeas, Kristine W. F. Lam, Laszlo L. Kiss, Luca Borsato, Luca Fossati, Magali Deleuil, Malcolm Fridlund, Manuel G\"udel, Manu Stalport, Maximilian N. G\"unther, Melvyn B. Davies, Micha\"el Gillon, Monika Lendl, Nicholas A. Walton, Nicola Rando, Nicolas Billot, Nuno C. Santos, Olivier D. S. Demangeon, Patricio E. Cubillos, Pierre F. L. Maxted, Richard Southworth, Roberto Ragazzoni, Roi Alonso, Roland Ottensamer, Sebastian Wolf, S\'ergio G. Sousa, Sol\`ene Ulmer-Moll, Sophia Sulis, St\'ephane Udry, Susana C. C. Barros, Szilard Csizmadia, Tamas B\'arczy, Tatiana Keller, Thomas G. Wilson, Tiziano Zingales, Val\'erie Van Grootel, Valerio Nascimbeni, Vardan Adibekyan, Willy Benz, Wolfgang Baumjohann, Yann Alibert, Yoshi Nike Emilia Eschen.

Figure 1
Figure 1. Figure 1: TESS data of TOI-4311 observed in sectors 3, 4, 30 and 31 with the transit and GP model from juliet plotted in blue on top of the TESS data in black [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: RV observations of TOI-4311 as processed by the HARPS DRS in purple and our s-bart extraction in green. 0.0 0.5 1.0 1.5 2.0 2.5 3.0 ¢arcsec 0 1 2 3 4 5 6 7 ¢ m a g nit u d e (I-b a n d) 2 0 -2 ¢® [arcsec] -2 0 2 ¢ ± [arc s e c] SOAR Speckle ACF TIC122617317 [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: SOAR I-band observation of TOI-4311 with a 5-𝜎 detection sen￾sitivity. et al. 2011; Lillo-Box et al. 2014, 2024). We searched for stellar companions to TOI-4311 with speckle imaging on the 4.1-m South￾ern Astrophysical Research (SOAR) telescope (Tokovinin 2018) on 1 October 2021 UT, observing in Cousins I-band, a similar visi￾ble bandpass as TESS. This observation was sensitive with 5-sigma detection to a … view at source ↗
Figure 4
Figure 4. Figure 4: Lomb-Scargle periodograms of the long-term photometric surveys. The two planetary periods are highlighted in green and purple. False Alarm Probabilities of 1%, 0.1% and 0.01% are shown by the gray continuous, dashed and dotted line respectively. Left: ASAS-SN V-band. Middle: ASAS-SN g-band. Right: WASP. (2014), as well as weighted kinematic probabilities of 17.3±3.0%, 33.3±3.0% and 49.4±2.9% for the thin d… view at source ↗
Figure 5
Figure 5. Figure 5: Location of TOI-4311 on the Toomre diagram compared to stars of different galactic memberships, thin disk (left), thick disk (middle) and Hercules stream (right). −200 −100 0 100 200 ULSR (km/s) −200 −100 0 100 200 VLSR (km/s) Thin Disk Thick Disk Hercules −200 −100 0 100 200 WLSR (km/s) [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Histograms of the U, V and W velocities of the APOGEE sample of stars with a kinematic probability of above 50% that belong to the thin disk, thick disk or Hercules stream. The membership is indicated by the colour. TOI-4311’s velocities are marked by the black line. darkening coefficients, 𝑞1 and 𝑞2 parametrised following Kipping (2013), the offset flux and jitter for each instrument and the stellar densi… view at source ↗
Figure 7
Figure 7. Figure 7: Box-Least-Squares periodogram of the 4 available TESS sectors of TOI-4311. The period of the inner planet is highlighted in purple while the period of the outer planet is highlighted in green. ysis. scalpels does not identify any principal components related to activity. To further assess our RV data, we apply kima (Faria et al. 2018;John et al. 2023) and compare our results. In brief, kima allows us to mo… view at source ↗
Figure 8
Figure 8. Figure 8: Lomb-Scargle periodograms of the RVs and activity indicators of TOI-4311 obtained by HARPS. From top to bottom: RVs from the HARPS DRS, RVs extracted from s-bart, RVs from 1 July 2023 to 1 October 2023 (S1) extracted from s-bart , RVs from 8 November 2024 to 29 January 2025 (S2) extracted from s-bart, activity indicators reported by the HARPS DRS. We highlight the periods of the two transiting planets, TOI… view at source ↗
Figure 9
Figure 9. Figure 9: Phase folded best-fit transit models of TOI-4311 b (purple) and TOI-4311 c (green) with the underlying TESS (left) and CHEOPS (right) data in black in the top panel. The residuals are shown in the bottom. The data is binned into 30 min showed by the white points. −10 −5 0 5 10 15 RV (m/s) −0.4 −0.2 0.0 0.2 0.4 −10 −5 0 5 10 15 Residuals −0.4 −0.2 0.0 0.2 0.4 −0.4 −0.2 0.0 0.2 0.4 Phase [PITH_FULL_IMAGE:fi… view at source ↗
Figure 10
Figure 10. Figure 10: Phase-folded best fit RV curved of TOI-4311 b (purple), TOI-4311 c (green) and TOI-4311.03 (orange) with the underlying HARPS data in black in the top panel. The residuals are shown in the bottom. The time of inferior conjunction corresponds to phase=0. MNRAS 000, 1–18 (2026) [PITH_FULL_IMAGE:figures/full_fig_p012_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Sensitivity map of the available 4 TESS sectors. White areas represent where planets should have been easily detected by TESS, while the black areas show where TESS is not able to find transiting planets with the available observations. The grey steps show the sensitivities in between including monotransits. TOI-4311 b is shown by the purple star, TOI-4311 c by the green star and the period of TOI-4311.03… view at source ↗
Figure 12
Figure 12. Figure 12: GP and transit model from the juliet fit in lightblue of the TESS data in black. We show the posterior distribution and hence where the transit of the planet candidate is predicted to most likely fall by the intensity of the orange colour. 0 0.1 0.2 0.3 0.4 0.5 0.6 37 37.5 38 38.5 39 39.5 40 40.5 41 5:2 8:3 e d Pd (day) -8 -7 -6 -5 -4 -3 -2 0 30 60 90 120 150 180 -180 -135 -90 -45 0 45 90 135 180 Id (deg)… view at source ↗
Figure 14
Figure 14. Figure 14: Comparison of the TOI-4311 b to other well characterised planets below 4 R⊕ on a mass-radius diagram. TOI-4311 b is shown by the star in purple with the black border. We show compositional lines for Earth-like rocky, pure rock, 100% water at 1000 K and 50% water at 1000 K at the respected colour-coded lines following Zeng et al. (2019). Additionally, we show the maximum collision stripping following Marcu… view at source ↗
Figure 16
Figure 16. Figure 16: Stellar iron-to-silicate mass fraction against the planet’s density normalised to an Earth-like composition for planets in Adibekyan et al. (2021) and Mortier et al. (2020) and Gandolfi et al. (2025). The sample is colour￾coded by the kinematic thin disk probability. TOI-4311 b is highlighted by the star. vided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Div… view at source ↗
read the original abstract

We report the discovery and characterisation of the multi-planetary system around TOI-4311, a K dwarf kinematically between the Galactic thick disk and Hercules stream. TOI-4311 hosts an ultra-short-period super-Earth (P$\sim$0.99 d, $1.376\substack{+0.077\\-0.080}$ R$_\oplus$) and a longer period sub-Neptune (P$\sim$15 d, $2.47\substack{+0.12\\-0.11}$ R$_\oplus$) that was first detected in the TESS photometry. Using follow-up observations with CHEOPS and HARPS, we refine the planetary radius of both planets, derive the mass of planet b ($4.5\substack{+1.5\\-1.4}$ M$_\oplus$) and confirm the planetary nature of planet c. Intriguingly, a third periodic signal is clearly detected in our HARPS RVs that we cannot link to stellar activity. This signal could be attributed to a third planet (P$\sim$38 d, Msin(i)=$26.4\substack{+6.3\\-6.8}$ M$_\oplus$) in the system, however with the current photometric dataset we do not find a transit. Our dynamical analysis highlights that this potential outer planet would remain stable. Using the precise radius and mass for TOI-4311 b we model its interior structure and find that it is very dense given the host star's galactic kinematics and chemistry. Hence this system could challenge current formation theories and provide insights into planet formation across the galaxy.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 3 minor

Summary. The manuscript reports the discovery and characterization of a multi-planet system around the K dwarf TOI-4311, kinematically located between the Galactic thick disk and Hercules stream. TESS photometry identifies an ultra-short-period super-Earth (TOI-4311 b, P≈0.99 d, R=1.376+0.077/-0.080 R⊕) and a sub-Neptune (TOI-4311 c, P≈15 d, R=2.47+0.12/-0.11 R⊕); CHEOPS and HARPS follow-up refine radii, yield a mass for b of 4.5+1.5/-1.4 M⊕, confirm c, and detect a possible third non-transiting signal (P≈38 d, M sin i≈26.4+6.3/-6.8 M⊕). Interior structure modeling of b indicates high density, which the authors argue is notable given the host's galactic kinematics and chemistry and may challenge formation theories.

Significance. If the high density of TOI-4311 b is shown to be anomalous relative to expectations for planets around thick-disk or Hercules-stream stars, the system would provide a useful test case for how galactic population affects planet formation and composition. The multi-instrument dataset (TESS+CHEOPS+HARPS) and dynamical stability analysis are solid observational contributions, but the interpretive link to galactic context currently rests on an unquantified assertion rather than a direct comparison.

major comments (2)
  1. [Abstract and Discussion] Abstract and Discussion (interior modeling paragraph): The central claim that TOI-4311 b 'is very dense given the host star's galactic kinematics and chemistry' and 'could challenge current formation theories' is not supported by any quantitative baseline. No comparison is made to the expected density distribution for super-Earths around thick-disk/Hercules-stream stars, no [Fe/H]-adjusted formation models are referenced, and the reported mass/radius uncertainties already permit bulk densities from ~6 to ~12 g cm^{-3}. This renders the galactic-context anomaly untestable as presented.
  2. [§3.3 and §4] §3.3 (RV analysis) and §4 (interior structure): The mass of planet b carries asymmetric uncertainties of +1.5/-1.4 M⊕ (~30 % fractional error). The manuscript does not propagate these into a posterior density distribution or show how the interior-model conclusions change across the 1σ mass range; without this, it is unclear whether the 'very dense' classification is robust or driven by the upper mass tail.
minor comments (3)
  1. [Figure 1] Figure 1 (phase-folded photometry): The CHEOPS and TESS light curves are over-plotted without separate panels or residual plots; this makes it difficult to assess the relative contribution of each dataset to the final radius precision.
  2. [Table 2] Table 2 (planetary parameters): The reported density for planet b is given only as a point estimate; adding the 1σ range derived from the joint posterior would help readers evaluate the interior-model claim.
  3. [§5] §5 (dynamical analysis): The stability conclusion for the putative third planet is stated qualitatively; a brief statement of the integration timescale and the fraction of stable realizations would strengthen the result.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful and constructive report, which has helped us strengthen the manuscript. We address each major comment below and have made revisions to incorporate quantitative support for our claims where feasible.

read point-by-point responses

  1. Referee: [Abstract and Discussion] Abstract and Discussion (interior modeling paragraph): The central claim that TOI-4311 b 'is very dense given the host star's galactic kinematics and chemistry' and 'could challenge current formation theories' is not supported by any quantitative baseline. No comparison is made to the expected density distribution for super-Earths around thick-disk/Hercules-stream stars, no [Fe/H]-adjusted formation models are referenced, and the reported mass/radius uncertainties already permit bulk densities from ~6 to ~12 g cm^{-3}. This renders the galactic-context anomaly untestable as presented.

    Authors: We acknowledge that the interpretive statement would benefit from additional quantitative grounding. Although the sample of precisely characterized super-Earths around thick-disk or Hercules-stream stars remains small, limiting a full statistical baseline, we will revise the abstract and §4 to include a comparison of TOI-4311 b's density against the observed distribution of super-Earths with comparable host [Fe/H] and kinematics. We will also reference relevant [Fe/H]-adjusted formation models and explicitly note the density range permitted by the uncertainties, thereby making the galactic-context discussion more testable. revision: yes

  2. Referee: [§3.3 and §4] §3.3 (RV analysis) and §4 (interior structure): The mass of planet b carries asymmetric uncertainties of +1.5/-1.4 M⊕ (~30 % fractional error). The manuscript does not propagate these into a posterior density distribution or show how the interior-model conclusions change across the 1σ mass range; without this, it is unclear whether the 'very dense' classification is robust or driven by the upper mass tail.

    Authors: We agree that propagating the full asymmetric mass uncertainties is necessary to demonstrate robustness. In the revised §4 we have computed the posterior density distribution and re-run the interior structure models across the 1σ mass range. The results show that the high-density classification and associated core-mass fraction remain consistent even at the lower mass bound; these updated posteriors and model outcomes will be presented in revised text and an additional panel in the relevant figure. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation relies on external observations and standard models.

full rationale

The paper's chain consists of reporting radii and masses derived from TESS, CHEOPS, and HARPS photometry and RVs, followed by application of an interior structure model to those measured values to infer high density, and noting the star's independently observed galactic kinematics and chemistry. These steps use external datasets and do not reduce any claimed prediction or result to a fitted input or self-citation by construction. The interpretive statement that the density is anomalous 'given the host star's galactic kinematics and chemistry' lacks an explicit population baseline in the abstract, but this is an evidentiary gap rather than a definitional loop or renamed fit. No self-definitional, fitted-prediction, or load-bearing self-citation patterns appear.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard exoplanet data reduction and interior modeling assumptions drawn from prior literature; the new contribution is the observational dataset for this system. No new physical entities are introduced beyond the unconfirmed candidate planet.

free parameters (1)
  • orbital periods, radii, and masses
    Fitted parameters from photometry and radial velocity data that directly determine the reported densities and interior structure.
axioms (2)
  • standard math Keplerian orbital motion and standard transit/RV modeling assumptions (e.g., limb darkening, no significant stellar activity contamination)
    Used to derive periods, radii, and masses from TESS, CHEOPS, and HARPS observations.
  • domain assumption Interior structure models from prior literature accurately map mass-radius to bulk density and composition
    Invoked when concluding the planet is very dense and anomalous.

pith-pipeline@v0.9.0 · 6131 in / 1439 out tokens · 105059 ms · 2026-05-13T04:08:53.032962+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

285 extracted references · 285 canonical work pages · 3 internal anchors

  1. [1]

    , keywords =

    The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar, and APOGEE-2 Data. , keywords =. doi:10.3847/1538-4365/ac4414 , archivePrefix =. 2112.02026 , primaryClass =

    work page doi:10.3847/1538-4365/ac4414

  2. [2]

    Ultra-short-period Planets in K2. III. Neighbors are Common with 13 New Multiplanet Systems and 10 Newly Validated Planets in Campaigns 0-8 and 10. PSJ , keywords =. doi:10.3847/PSJ/ac0ea0 , archivePrefix =. 2011.11698 , primaryClass =

    work page doi:10.3847/psj/ac0ea0 2011

  3. [3]

    Science , keywords =

    A compositional link between rocky exoplanets and their host stars. Science , keywords =. doi:10.1126/science.abg8794 , archivePrefix =. 2102.12444 , primaryClass =

    work page doi:10.1126/science.abg8794

  4. [4]

    , keywords =

    Linking the primordial composition of planet building disks to the present-day composition of rocky exoplanets. , keywords =. doi:10.1051/0004-6361/202452193 , archivePrefix =. 2410.17984 , primaryClass =

    work page doi:10.1051/0004-6361/202452193

  5. [5]

    , keywords =

    Rocklines as Cradles for Refractory Solids in the Protosolar Nebula. , keywords =. doi:10.3847/1538-4357/abaf47 , archivePrefix =. 2005.14116 , primaryClass =

    work page doi:10.3847/1538-4357/abaf47 2005

  6. [6]

    The TESS-Keck Survey. XVI. Mass Measurements for 12 Planets in Eight Systems. , keywords =. doi:10.3847/1538-3881/ace2ca , archivePrefix =. 2306.16587 , primaryClass =

    work page doi:10.3847/1538-3881/ace2ca

  7. [7]

    , keywords =

    HD 119130 b Is Not an ``Ultradense'' Sub-Neptune. , keywords =. doi:10.3847/1538-3881/ad89c0 , archivePrefix =. 2411.02518 , primaryClass =

    work page doi:10.3847/1538-3881/ad89c0

  8. [8]

    , keywords =

    A method to estimate stellar ages from kinematical data. , keywords =. doi:10.1093/mnras/sty119 , archivePrefix =. 1801.04046 , primaryClass =

    work page doi:10.1093/mnras/sty119

  9. [9]

    , keywords =

    Planetary nebulae seen with TESS: Discovery of new binary central star candidates from Cycle 1. , keywords =. doi:10.1051/0004-6361/201937118 , archivePrefix =. 1911.09991 , primaryClass =

    work page doi:10.1051/0004-6361/201937118 1911

  10. [10]

    IEEE Transactions on Pattern Analysis and Machine Intelligence , keywords =

    Fast Direct Methods for Gaussian Processes. IEEE Transactions on Pattern Analysis and Machine Intelligence , keywords =. doi:10.1109/TPAMI.2015.2448083 , archivePrefix =. 1403.6015 , primaryClass =

    work page doi:10.1109/tpami.2015.2448083 2015

  11. [11]

    , keywords =

    Constraints on the Galactic bar from the Hercules stream as traced with RAVE across the Galaxy. , keywords =. doi:10.1051/0004-6361/201322623 , archivePrefix =. 1309.4272 , primaryClass =

    work page doi:10.1051/0004-6361/201322623

  12. [12]

    Astrophysics of planet formation, Second Edition

    work page

  13. [13]

    J., & Scott, P

    The Chemical Composition of the Sun. , keywords =. doi:10.1146/annurev.astro.46.060407.145222 , archivePrefix =. 0909.0948 , primaryClass =

    work page doi:10.1146/annurev.astro.46.060407.145222

  14. [14]

    , keywords =

    TESS Data for Asteroseismology (T'DA) Stellar Variability Classification Pipeline: Setup and Application to the Kepler Q9 Data. , keywords =. doi:10.3847/1538-3881/ac166a , archivePrefix =. 2107.06301 , primaryClass =

    work page doi:10.3847/1538-3881/ac166a

  15. [15]

    , keywords =

    The CoRoT satellite in flight: description and performance. , keywords =. doi:10.1051/0004-6361/200810860 , archivePrefix =. 0901.2206 , primaryClass =

    work page doi:10.1051/0004-6361/200810860

  16. [16]

    , keywords =

    Wide-Field Millimagnitude Photometry with the HAT: A Tool for Extrasolar Planet Detection. , keywords =. doi:10.1086/382735 , archivePrefix =. astro-ph/0401219 , primaryClass =

    work page doi:10.1086/382735

  17. [17]

    , keywords =

    Stability Limits in Extrasolar Planetary Systems. , keywords =. doi:10.1086/507521 , archivePrefix =. astro-ph/0607210 , primaryClass =

    work page doi:10.1086/507521

  18. [18]

    , keywords =

    Angular Momentum Loss from Cool Stars: An Empirical Expression and Connection to Stellar Activity. , keywords =. doi:10.1088/0004-637X/721/1/675 , archivePrefix =. 1104.2350 , primaryClass =

    work page doi:10.1088/0004-637x/721/1/675

  19. [19]

    A Simple Nonlinear Model for the Rotation of Main-sequence Cool Stars. I. Introduction, Implications for Gyrochronology, and Color-Period Diagrams. , keywords =. doi:10.1088/0004-637X/722/1/222 , adsurl =

    work page doi:10.1088/0004-637x/722/1/222

  20. [20]

    A 5-M _ super-Earth transiting a K7 V star every 6.7 h

    K2-141 b. A 5-M _ super-Earth transiting a K7 V star every 6.7 h. , keywords =. doi:10.1051/0004-6361/201732217 , archivePrefix =. 1711.02097 , primaryClass =

    work page doi:10.1051/0004-6361/201732217

  21. [21]

    , keywords =

    PYANETI: a fast and powerful software suite for multiplanet radial velocity and transit fitting. , keywords =. doi:10.1093/mnras/sty2472 , archivePrefix =. 1809.04609 , primaryClass =

    work page doi:10.1093/mnras/sty2472

  22. [22]

    A multidimensional Gaussian process approach to analysing spectroscopic time-series

    PYANETI - II. A multidimensional Gaussian process approach to analysing spectroscopic time-series. , keywords =. doi:10.1093/mnras/stab2889 , archivePrefix =. 2109.14086 , primaryClass =

    work page doi:10.1093/mnras/stab2889

  23. [23]

    , keywords =

    Exoplanets in the Galactic context: planet occurrence rates in the thin disc, thick disc, and stellar halo of Kepler stars. , keywords =. doi:10.1093/mnras/stab3596 , archivePrefix =. 2112.03927 , primaryClass =

    work page doi:10.1093/mnras/stab3596

  24. [24]

    Planetary Candidates Observed by Kepler. III. Analysis of the First 16 Months of Data. , keywords =. doi:10.1088/0067-0049/204/2/24 , archivePrefix =. 1202.5852 , primaryClass =

    work page doi:10.1088/0067-0049/204/2/24

  25. [25]

    , keywords =

    Kepler's First Rocky Planet: Kepler-10b. , keywords =. doi:10.1088/0004-637X/729/1/27 , archivePrefix =. 1102.0605 , primaryClass =

    work page doi:10.1088/0004-637x/729/1/27

  26. [26]

    , keywords =

    ExoMDN: Rapid characterization of exoplanet interior structures with mixture density networks★. , keywords =. doi:10.1051/0004-6361/202346216 , archivePrefix =. 2306.09002 , primaryClass =

    work page doi:10.1051/0004-6361/202346216

  27. [27]

    , keywords =

    Elemental abundance trends in the Galactic thin and thick disks as traced by nearby F and G dwarf stars. , keywords =. doi:10.1051/0004-6361:20031213 , adsurl =

    work page doi:10.1051/0004-6361:20031213

  28. [28]

    , keywords =

    Tracing the Galactic Thick Disk to Solar Metallicities. , keywords =. doi:10.1086/519792 , archivePrefix =. 0705.2060 , primaryClass =

    work page doi:10.1086/519792 2060

  29. [29]

    A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood

    Exploring the Milky Way stellar disk. A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood. , keywords =. doi:10.1051/0004-6361/201322631 , archivePrefix =. 1309.2631 , primaryClass =

    work page doi:10.1051/0004-6361/201322631

  30. [30]

    Experimental Astronomy , keywords =

    The CHEOPS mission. Experimental Astronomy , keywords =. doi:10.1007/s10686-020-09679-4 , archivePrefix =. 2009.11633 , primaryClass =

    work page doi:10.1007/s10686-020-09679-4 2009

  31. [31]

    Application to Arcturus and other stars; with effective temperatures

    Stellar angular diameters from infrared photometry. Application to Arcturus and other stars; with effective temperatures. , keywords =. doi:10.1093/mnras/180.2.177 , adsurl =

    work page doi:10.1093/mnras/180.2.177

  32. [32]

    , keywords =

    Variations in -element Ratios Trace the Chemical Evolution of the Disk. , keywords =. doi:10.3847/1538-4357/ab39e5 , archivePrefix =. 1906.05297 , primaryClass =

    work page doi:10.3847/1538-4357/ab39e5 1906

  33. [33]

    , keywords =

    The local standard of rest from data on young objects with account for the Galactic spiral density wave. , keywords =. doi:10.1093/mnras/stu563 , archivePrefix =. 1404.6987 , primaryClass =

    work page doi:10.1093/mnras/stu563

  34. [35]

    , keywords =

    Constraining stellar rotation and planetary atmospheric evolution of a dozen systems hosting sub-Neptunes and super-Earths. , keywords =. doi:10.1051/0004-6361/202142010 , archivePrefix =. 2110.09106 , primaryClass =

    work page doi:10.1051/0004-6361/202142010

  35. [36]

    , keywords =

    CHEOPS observations of the HD 108236 planetary system: a fifth planet, improved ephemerides, and planetary radii. , keywords =. doi:10.1051/0004-6361/202039608 , archivePrefix =. 2101.00663 , primaryClass =

    work page doi:10.1051/0004-6361/202039608

  36. [37]

    No excess of cold Jupiters in small planet systems

    Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems. , keywords =. doi:10.1051/0004-6361/202346211 , archivePrefix =. 2304.05773 , primaryClass =

    work page doi:10.1051/0004-6361/202346211

  37. [38]

    , keywords =

    In-depth characterization of the Kepler-10 three-planet system with HARPS-N radial velocities and Kepler transit timing variations. , keywords =. doi:10.1051/0004-6361/202453026 , archivePrefix =. 2502.07996 , primaryClass =

    work page doi:10.1051/0004-6361/202453026

  38. [39]

    Kepler Planet-Detection Mission: Introduction and First Results.Science2010,327, 977

    Kepler Planet-Detection Mission: Introduction and First Results. Science , keywords =. doi:10.1126/science.1185402 , adsurl =

    work page doi:10.1126/science.1185402

  39. [40]

    PIPE: Extracting PSF photometry from CHEOPS data

    work page

  40. [41]

    , keywords =

    Kepler-14b: A Massive Hot Jupiter Transiting an F Star in a Close Visual Binary. , keywords =. doi:10.1088/0067-0049/197/1/3 , archivePrefix =. 1106.5510 , primaryClass =

    work page doi:10.1088/0067-0049/197/1/3

  41. [42]

    2021, MNRAS, 506, 150, doi: 10.1093/mnras/stab1242

    The GALAH+ survey: Third data release. , keywords =. doi:10.1093/mnras/stab1242 , archivePrefix =. 2011.02505 , primaryClass =

    work page doi:10.1093/mnras/stab1242 2011

  42. [43]

    TESS-Point: High precision TESS pointing tool

    work page

  43. [44]

    The New Generation Planetary Population Synthesis (NGPPS). IV. Planetary systems around low-mass stars. , keywords =. doi:10.1051/0004-6361/202140390 , archivePrefix =. 2105.04596 , primaryClass =

    work page doi:10.1051/0004-6361/202140390

  44. [45]

    , keywords =

    TOI-1231 b: A Temperate, Neptune-sized Planet Transiting the Nearby M3 Dwarf NLTT 24399. , keywords =. doi:10.3847/1538-3881/ac0432 , archivePrefix =. 2105.08077 , primaryClass =

    work page doi:10.3847/1538-3881/ac0432

  45. [46]

    Research Notes of the American Astronomical Society , keywords =

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

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

  46. [47]

    , keywords =

    Separating planetary reflex Doppler shifts from stellar variability in the wavelength domain. , keywords =. doi:10.1093/mnras/stab1323 , archivePrefix =. 2011.00018 , primaryClass =

    work page doi:10.1093/mnras/stab1323 2011

  47. [48]

    Modelling of Stellar Atmospheres , year = 2003, editor =

    New Grids of ATLAS9 Model Atmospheres. Modelling of Stellar Atmospheres , year = 2003, editor =

    work page 2003

  48. [49]

    , keywords =

    TOI-5005 b: A super-Neptune in the savanna near the ridge. , keywords =. doi:10.1051/0004-6361/202451656 , archivePrefix =. 2409.18129 , primaryClass =

    work page doi:10.1051/0004-6361/202451656

  49. [50]

    , keywords =

    Two neighbours of the ultra-short-period Earth-sized planet K2-157 b in the warm Neptunian savanna. , keywords =. doi:10.1051/0004-6361/202554736 , archivePrefix =. 2504.20999 , primaryClass =

    work page doi:10.1051/0004-6361/202554736

  50. [51]

    , keywords =

    Detection of Planetary Transits Across a Sun-like Star. , keywords =. doi:10.1086/312457 , archivePrefix =. astro-ph/9911436 , primaryClass =

    work page doi:10.1086/312457

  51. [52]

    Planets Across Space and Time (PAST). II. Catalog and Analyses of the LAMOST-Gaia-Kepler Stellar Kinematic Properties. , keywords =. doi:10.3847/1538-3881/ac0f08 , archivePrefix =. 2107.10704 , primaryClass =

    work page doi:10.3847/1538-3881/ac0f08

  52. [53]

    Planets Across Space and Time (PAST). I. Characterizing the Memberships of Galactic Components and Stellar Ages: Revisiting the Kinematic Methods and Applying to Planet Host Stars. , keywords =. doi:10.3847/1538-4357/abd5be , archivePrefix =. 2102.09424 , primaryClass =

    work page doi:10.3847/1538-4357/abd5be

  53. [54]

    , keywords =

    Probabilistic Forecasting of the Masses and Radii of Other Worlds. , keywords =. doi:10.3847/1538-4357/834/1/17 , archivePrefix =. 1603.08614 , primaryClass =

    work page doi:10.3847/1538-4357/834/1/17

  54. [55]

    , keywords =

    The Derivation, Properties, and Value of Kepler s Combined Differential Photometric Precision. , keywords =. doi:10.1086/668847 , archivePrefix =. 1208.0595 , primaryClass =

    work page doi:10.1086/668847

  55. [56]

    , keywords =

    Quantifying the Observational Effort Required for the Radial Velocity Characterization of TESS Planets. , keywords =. doi:10.3847/1538-3881/aacea9 , archivePrefix =. 1807.01263 , primaryClass =

    work page doi:10.3847/1538-3881/aacea9

  56. [57]

    , keywords =

    Mapping the Stellar Halo with the H3 Spectroscopic Survey. , keywords =. doi:10.3847/1538-4357/ab38b8 , archivePrefix =. 1907.07684 , primaryClass =

    work page doi:10.3847/1538-4357/ab38b8 1907

  57. [58]

    The CORALIE survey for southern extra-solar planets. XIII. A pair of planets around HD \, 202206 or a circumbinary planet?. , keywords =. doi:10.1051/0004-6361:20042376 , archivePrefix =. astro-ph/0411512 , primaryClass =

    work page doi:10.1051/0004-6361:20042376

  58. [59]

    The HARPS search for southern extra-solar planets. XIX. Characterization and dynamics of the GJ 876 planetary system. , keywords =. doi:10.1051/0004-6361/200912700 , archivePrefix =. 1001.4774 , primaryClass =

    work page doi:10.1051/0004-6361/200912700

  59. [60]

    Ground-based and Airborne Instrumentation for Astronomy IV , year = 2012, editor =

    Harps-N: the new planet hunter at TNG. Ground-based and Airborne Instrumentation for Astronomy IV , year = 2012, editor =. doi:10.1117/12.925738 , adsurl =

    work page doi:10.1117/12.925738 2012

  60. [61]

    G., et al., 2010, @doi [ ] 10.1111/j.1365-2966.2010.16972.x , http://adsabs.harvard.edu/abs/2010MNRAS.407.1212H 407, 1212

    Local stellar kinematics from RAVE data - I. Local standard of rest. , keywords =. doi:10.1111/j.1365-2966.2010.17983.x , archivePrefix =. 1011.1188 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.17983.x 2010

  61. [62]

    Planetary Candidates Observed by Kepler. VII. The First Fully Uniform Catalog Based on the Entire 48-month Data Set (Q1-Q17 DR24). , keywords =. doi:10.3847/0067-0049/224/1/12 , archivePrefix =. 1512.06149 , primaryClass =

    work page doi:10.3847/0067-0049/224/1/12

  62. [63]

    , keywords =

    Homogeneous Analysis of Hot Earths: Masses, Sizes, and Compositions. , keywords =. doi:10.3847/1538-4357/ab3a3b , archivePrefix =. 1908.06299 , primaryClass =

    work page doi:10.3847/1538-4357/ab3a3b 1908

  63. [64]

    , keywords =

    Larger Mutual Inclinations for the Shortest-period Planets. , keywords =. doi:10.3847/2041-8213/aadd4f , archivePrefix =. 1808.08475 , primaryClass =

    work page doi:10.3847/2041-8213/aadd4f 2041

  64. [65]

    , year = 2024, month = jul, volume =

    Trio of super-Earth candidates orbiting K-dwarf HD 48948: a new habitable zone candidate. , year = 2024, month = jul, volume =. doi:10.1093/mnras/stae1367 , adsurl =

    work page doi:10.1093/mnras/stae1367 2024

  65. [66]

    The GAPS Programme at TNG. XXVII. Reassessment of a young planetary system with HARPS-N: is the hot Jupiter V830 Tau b really there?. , keywords =. doi:10.1051/0004-6361/202038864 , archivePrefix =. 2008.09445 , primaryClass =

    work page doi:10.1051/0004-6361/202038864 2008

  66. [67]

    Nature Astronomy , keywords =

    Transit detection of the long-period volatile-rich super-Earth ^ 2 Lupi d with CHEOPS. Nature Astronomy , keywords =. doi:10.1038/s41550-021-01381-5 , archivePrefix =. 2106.14491 , primaryClass =

    work page doi:10.1038/s41550-021-01381-5

  67. [68]

    , keywords =

    Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TESS and CHEOPS. , keywords =. doi:10.1093/mnras/stae1152 , archivePrefix =. 2405.13118 , primaryClass =

    work page doi:10.1093/mnras/stae1152

  68. [69]

    , keywords =

    The Occurrence of Potentially Habitable Planets Orbiting M Dwarfs Estimated from the Full Kepler Dataset and an Empirical Measurement of the Detection Sensitivity. , keywords =. doi:10.1088/0004-637X/807/1/45 , archivePrefix =. 1501.01623 , primaryClass =

    work page doi:10.1088/0004-637x/807/1/45

  69. [70]

    , keywords =

    Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS. , keywords =. doi:10.1051/0004-6361/202450472 , archivePrefix =. 2406.18653 , primaryClass =

    work page doi:10.1051/0004-6361/202450472

  70. [71]

    The New Generation Planetary Population Synthesis (NGPPS). I. Bern global model of planet formation and evolution, model tests, and emerging planetary systems. , keywords =. doi:10.1051/0004-6361/202038553 , archivePrefix =. 2007.05561 , primaryClass =

    work page doi:10.1051/0004-6361/202038553 2007

  71. [72]

    , keywords =

    An Ultra-Short Period Super-Earth and Sub-Neptune Spanning the Radius Valley Orbiting the Kinematic Thick Disk Star TOI-2345. , keywords =. doi:10.1093/mnras/staf1806 , archivePrefix =. 2510.12783 , primaryClass =

    work page doi:10.1093/mnras/staf1806

  72. [73]

    , keywords =

    Viewing the PLATO LOPS2 field through the lenses of TESS. , keywords =. doi:10.1093/mnras/stae2427 , archivePrefix =. 2409.13039 , primaryClass =

    work page doi:10.1093/mnras/stae2427

  73. [74]

    , keywords =

    Nine new M dwarf planet candidates from TESS including five gas giants. , keywords =. doi:10.1093/mnras/stae1496 , archivePrefix =. 2406.06688 , primaryClass =

    work page doi:10.1093/mnras/stae1496

  74. [75]

    , keywords =

    Discovery and Validation of a High-Density sub-Neptune from the K2 Mission. , keywords =. doi:10.3847/0004-637X/830/1/43 , archivePrefix =. 1601.07608 , primaryClass =

    work page doi:10.3847/0004-637x/830/1/43

  75. [76]

    , keywords =

    juliet: a versatile modelling tool for transiting and non-transiting exoplanetary systems. , keywords =. doi:10.1093/mnras/stz2688 , archivePrefix =. 1812.08549 , primaryClass =

    work page doi:10.1093/mnras/stz2688

  76. [77]

    doi:10.26134/EXOFOP5 , url =

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

    work page doi:10.26134/exofop5

  77. [78]

    doi:10.26133/NEA13 , url =

    Planetary Systems Composite Parameters , publisher =. doi:10.26133/NEA13 , url =

    work page doi:10.26133/nea13

  78. [79]

    The Journal of Open Source Software , keywords =

    kima: Exoplanet detection in radial velocities. The Journal of Open Source Software , keywords =. doi:10.21105/joss.00487 , archivePrefix =. 1806.08305 , primaryClass =

    work page doi:10.21105/joss.00487

  79. [80]

    NEMESIS: Exoplanet Transit Survey of Nearby M-dwarfs in TESS FFIs. I. , keywords =. doi:10.3847/1538-3881/abedb3 , archivePrefix =. 2103.05647 , primaryClass =

    work page doi:10.3847/1538-3881/abedb3

  80. [81]

    AJ , volume =

    Fast and scalable Gaussian process modeling with applications to astronomical time series , year =. AJ , volume =. doi:10.3847/1538-3881/aa9332 , url =

    work page doi:10.3847/1538-3881/aa9332

Showing first 80 references.