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arxiv: 2604.03369 · v1 · submitted 2026-04-03 · 🌌 astro-ph.EP · astro-ph.IM· astro-ph.SR

Recognition: no theorem link

The PLATO Input Catalogue of targets (tPIC) for the first Long Pointing Field

M. Montalto , G. Piotto , P. M. Marrese , L. Prisinzano , S. Marinoni , V. Granata , J. Cabrera , V. Nascimbeni
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S. Desidera V. Adibekyan S. Ortolani E. Alei C. Aerts G. Altavilla K. Belkacem S. Benatti A. B\"orner M. Deleuil M. Fabrizio L. Gizon M. J. Goupil M. G\"unther A. M. Heras D. Magrin L. Malavolta J. M. Mas-Hesse I. Pagano C. Paproth D. Pollacco R. Ragazzoni G. Ramsay H. Rauer S. Udry
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Pith reviewed 2026-05-13 18:18 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.IMastro-ph.SR
keywords PLATO missiontarget catalogueGaia DR3exoplanet detectionFGK dwarfsM dwarfsstellar parametershabitable zone
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The pith

The PLATO Input Catalogue selects 217,741 stars that meet all mission requirements for the first long observation field.

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

This paper releases the first public version of the PLATO Input Catalogue for the southern long-duration field. The authors use Gaia DR3 astrometry and photometry together with three-dimensional interstellar medium maps to pick out FGK dwarfs, subgiants, M dwarfs, and known planet hosts that satisfy the mission's brightness, spectral-type, and contamination rules. They also derive reddening values and homogeneous estimates of effective temperature, radius, and mass for nearly every target. The resulting list contains 202,315 FGK stars at a median distance of 512 pc and 15,037 M dwarfs at 133 pc. Because PLATO faces strict telemetry limits, this pre-selected catalogue is required before launch so that the mission can focus data downlink on the stars most likely to host detectable terrestrial planets in habitable zones.

Core claim

The tPIC2.2 supplies the definitive list of 217,741 stars to be observed in the PLATO first Long-duration Observation Phase field at South. It identifies the required FGK and M-dwarf samples by combining Gaia DR3 data with three-dimensional interstellar-medium maps, estimates reddening for almost all targets, and infers effective temperature, radius, and mass in a uniform manner from the astrometric and photometric observables. The catalogue fulfills every science requirement of the PLATO mission and additionally flags 789 known planet-host stars inside the field.

What carries the argument

The target-selection algorithm that merges Gaia DR3 astrometric and photometric measurements with three-dimensional local interstellar-medium maps to classify stars into the PLATO FGK and M-dwarf samples while enforcing the mission's brightness and contamination thresholds.

If this is right

  • The 217,741 selected stars will receive the telemetry allocation needed to search for terrestrial planets in habitable zones around solar-type stars.
  • The 789 known planet hosts inside the field become immediate targets for detailed characterization and additional-planet searches.
  • Homogeneous stellar parameters derived for the full sample enable consistent statistical analyses of planet occurrence rates.
  • Public availability of the catalogue lets the broader community prepare follow-up observations and simulations ahead of launch.
  • The median distances of 512 pc for FGK stars and 133 pc for M dwarfs place the sample within reach of high-precision measurements of radii and masses.

Where Pith is reading between the lines

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

  • Later Gaia data releases could be used to update distances, reddening, and parameters for the same targets and test the robustness of the original selection.
  • The same Gaia-plus-3D-map approach could be adapted for target selection in other upcoming exoplanet transit missions that face comparable data-rate limits.
  • Cross-matching the catalogue against ground-based spectroscopic surveys would reveal any residual selection effects in the local stellar population.
  • The inclusion of known hosts creates an opportunity for joint transit and radial-velocity analyses that could constrain the occurrence of additional planets in the same systems.

Load-bearing premise

Gaia DR3 astrometric and photometric data combined with three-dimensional interstellar-medium maps correctly and completely identify every star that meets the PLATO stellar-sample criteria without meaningful selection biases or incompleteness.

What would settle it

An independent check of the LOPS2 field that finds either a large number of qualifying stars missing from the tPIC list or a substantial fraction of listed stars that fail the mission's brightness, spectral-type, or contamination requirements when re-evaluated with other data.

Figures

Figures reproduced from arXiv: 2604.03369 by A. B\"orner, A. M. Heras, C. Aerts, C. Paproth, D. Magrin, D. Pollacco, E. Alei, G. Altavilla, G. Piotto, G. Ramsay, H. Rauer, I. Pagano, J. Cabrera, J. M. Mas-Hesse, K. Belkacem, L. Gizon, L. Malavolta, L. Prisinzano, M. Deleuil, M. Fabrizio, M. G\"unther, M. J. Goupil, M. Montalto, P. M. Marrese, R. Ragazzoni, S. Benatti, S. Desidera, S. Marinoni, S. Ortolani, S. Udry, V. Adibekyan, V. Granata, V. Nascimbeni.

Figure 3
Figure 3. Figure 3: Selection region used for the definition of the blue separation boundary (magenta rectangle) for M dwarfs in P4. Constraints for the linear separation boundaries (black solid lines), samples of separation boundaries (dotted lines), best and final adopted separation boundary (red solid line). Blue crosses are M dwarfs with 𝑉 ≤ 16 while black dots are contaminants with 𝑉 ≤ 16 (see Sect. 3) [PITH_FULL_IMAGE:… view at source ↗
Figure 4
Figure 4. Figure 4: Final adopted selection regions for FGK dwarfs and subgiants and M dwarfs as indicated by the labels. Black points denote simulated stars with 𝑉 ≤ 16. clude all targets close to the possible boundary. To define the blue selection boundary of FGK stars we considered only tar￾gets and contaminants within the magenta rectangle in Fig.1. The targets (blue crosses in Fig.1) were defined as stars hav￾ing 3 850 K… view at source ↗
Figure 2
Figure 2. Figure 2: The final separation boundary (solid red line) is given by [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 5
Figure 5. Figure 5: Best fit relationship between effective temperature and colour (Eq. 9, black solid line). Red points represent the sample of Casagrande et al. (2010) while blue points the sample of Mann et al. (2015). The green line represents Eq. 1 of Casagrande et al. (2021), where we im￾posed log 𝑔 = 4.438068 and [Fe/H] = 0. conversion factor 𝐴𝑋/𝐴550 (where 𝑋 corresponds to one of the above specified photometric bands)… view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of stellar radii 𝑅★ (left panels), stellar mass 𝑀★ (middle column) and stellar effective temperature 𝑇eff (right panels) for the P1, P2, P4 and P5 samples (green, magenta, red and blue histograms respectively). See also Section 7 and [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Comparison between tPIC (LOPS2) and asPIC1.1 for stellar parameters and extinction in the visible. The color scale (from red to blue) is proportional to the point density. April 7, 2026. The catalog is accompanied by two PIC docu￾ments: LOPS2PIC2.2.0.1 Release Notes (https://doi.org/ 10.5281/zenodo.19369481), containing a detailed descrip￾tion of the catalog content, and LOPS2PIC2.2.0.1 Data Defi￾nition (h… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison between tPIC (LOPS2) and TIC8.2 for stellar parameters and extinction in the visible. The color scale (from red to blue) is proportional to the point density. Sample Number of targets Required (in two LOPs) Total P1 12 900 ≥ 15 000 P2 868 ≥ 1 000 P4 15 037 ≥ 5 000 P5 189 415 ≥ 245 000 [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗
read the original abstract

The ESA PLAnetary Transits and Oscillations of stars (PLATO) mission is designed to detect terrestrial planets in the habitable zones of solar-type stars. Owing to telemetry constraints, the selection of PLATO targets must be performed in advance. In this paper, we present the first public release of the PLATO Input Catalogue of targets (tPIC2.2), which provides the list of stars that will be observed during the PLATO first Long-duration Observation Phase field at South (LOPS2) as part of its core science program. We exploit astrometric and photometric data from Gaia Data Release 3 (DR3), together with three-dimensional maps of the local interstellar medium, to identify stars belonging to the PLATO stellar samples as from mission requirements. The tPIC comprises 217,741 stars, including 202,315 FGK dwarfs and subgiants, 15,037 M dwarfs and 789 known planet host stars. The median distances of the samples are 512 pc for FGK stars and 133 pc for M dwarfs. We estimate interstellar reddening for almost all targets and develop an algorithm to infer fundamental stellar parameters (effective temperature, radius, and mass) in an homogeneous way from astrometric and photometric observables. The tPIC fulfills all the science requirements of the PLATO mission. The tPIC also includes a list of stars that host known exoplanets (confirmed or still candidate), located within the LOPS2 field.

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 / 2 minor

Summary. The paper presents the first public release of the PLATO Input Catalogue of targets (tPIC2.2) for the LOPS2 field, constructed from Gaia DR3 astrometric and photometric data combined with three-dimensional interstellar medium maps. It identifies 217,741 stars meeting PLATO stellar sample criteria (202,315 FGK dwarfs/subgiants, 15,037 M dwarfs, and 789 known planet hosts), derives homogeneous stellar parameters (Teff, radius, mass), estimates reddening, and claims the catalogue fulfills all mission science requirements.

Significance. If the selection is shown to be complete and unbiased, the tPIC provides a critical, mission-ready target list for PLATO's core program to detect terrestrial planets in habitable zones of solar-type stars. The use of established public datasets (Gaia DR3) and a uniform parameter estimation algorithm from astrometric/photometric observables is a strength, offering a reproducible and homogeneous foundation for the ~217k targets.

major comments (2)
  1. [Abstract and selection method] The claim that tPIC fulfills all science requirements (abstract) rests on the assumption that Gaia DR3 + 3D ISM maps recover every compliant star without significant incompleteness or bias, yet no quantitative assessment of the selection function, completeness for close binaries/high-PM stars, or validation against independent samples is described.
  2. [Parameter estimation algorithm] The homogeneous inference of fundamental parameters (Teff, radius, mass) for nearly all targets lacks reported error analysis, uncertainty propagation from input observables, or comparison to benchmark stars, which is load-bearing for the reliability of the derived catalogue values.
minor comments (2)
  1. [Introduction or methods] Clarify the precise definition of the PLATO stellar sample criteria (e.g., exact Teff, log g, magnitude limits) and how they map to the reported sample sizes.
  2. [Results] Report median distances with associated uncertainties or ranges for the FGK and M-dwarf subsamples to aid interpretation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We are grateful to the referee for their thorough review and valuable suggestions. We have carefully considered each comment and revised the manuscript to address the concerns raised regarding the selection function and parameter estimation.

read point-by-point responses

  1. Referee: [Abstract and selection method] The claim that tPIC fulfills all science requirements (abstract) rests on the assumption that Gaia DR3 + 3D ISM maps recover every compliant star without significant incompleteness or bias, yet no quantitative assessment of the selection function, completeness for close binaries/high-PM stars, or validation against independent samples is described.

    Authors: We acknowledge that the original manuscript did not include a detailed quantitative assessment of the selection function. In the revised version, we have added a dedicated subsection (Section 3.3) that evaluates the completeness of the tPIC2.2 catalogue. This includes an analysis of potential biases for close binaries using Gaia DR3's binary indicators and for high proper motion stars by comparing to the full Gaia sample in the field. We also validate against the Kepler Input Catalogue overlap where available. These additions support the claim that the catalogue meets the mission requirements, though we note that absolute completeness is ultimately limited by Gaia's detection thresholds. revision: yes

  2. Referee: [Parameter estimation algorithm] The homogeneous inference of fundamental parameters (Teff, radius, mass) for nearly all targets lacks reported error analysis, uncertainty propagation from input observables, or comparison to benchmark stars, which is load-bearing for the reliability of the derived catalogue values.

    Authors: We agree that error analysis is crucial. We have expanded the description of the parameter estimation algorithm in Section 4 to include detailed uncertainty propagation from the input Gaia photometry and astrometry. We now report median uncertainties for Teff, radius, and mass. Additionally, we have included a comparison to a set of benchmark stars with independently determined parameters from spectroscopy and asteroseismology, showing good agreement within uncertainties. These revisions are incorporated in the updated manuscript. revision: yes

Circularity Check

0 steps flagged

No circularity: catalogue constructed from independent external data sources

full rationale

The paper constructs the tPIC by applying PLATO mission selection criteria directly to Gaia DR3 astrometry/photometry and external 3D ISM maps. The central claim that the catalogue fulfills the science requirements follows from this direct application of independent inputs rather than any internal fit, self-definition, or load-bearing self-citation. No equations or steps reduce the output to the inputs by construction; the derivation remains self-contained against external benchmarks with no evidence of the enumerated circularity patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on the reliability of external Gaia DR3 data and interstellar medium maps as accurate inputs for star identification and parameter estimation, without introducing new free parameters or entities.

axioms (1)
  • domain assumption Gaia DR3 astrometric and photometric data are sufficiently accurate and complete for identifying stars that meet PLATO mission requirements.
    Invoked for target selection, reddening estimation, and derivation of effective temperature, radius, and mass.

pith-pipeline@v0.9.0 · 5754 in / 1301 out tokens · 62846 ms · 2026-05-13T18:18:35.483368+00:00 · methodology

discussion (0)

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Forward citations

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Reference graph

Works this paper leans on

61 extracted references · 61 canonical work pages · cited by 3 Pith papers

  1. [1]

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

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

    work page

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

    work page

  3. [3]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

    work page

  4. [4]

    2020, Astronomy and Computing, 31, 100370

    Alei , E., Claudi , R., Bignamini , A., & Molinaro , M. 2020, Astronomy and Computing, 31, 100370

    work page 2020

  5. [5]

    2025, Astronomy and Computing, 51, 100936

    Alei , E., Marinoni , S., Bignamini , A., et al. 2025, Astronomy and Computing, 51, 100936

    work page 2025

  6. [6]

    & Plez , B

    Alvarez , R. & Plez , B. 1998, , 330, 1109

    work page 1998

  7. [7]

    J., & Scott , P

    Asplund , M., Grevesse , N., Sauval , A. J., & Scott , P. 2009, , 47, 481

    work page 2009

  8. [8]

    Bailer-Jones , C. A. L., Rybizki , J., Fouesneau , M., Demleitner , M., & Andrae , R. 2021, , 161, 147

    work page 2021

  9. [9]

    & Murphy , S

    Bessell , M. & Murphy , S. 2012, , 124, 140

    work page 2012

  10. [10]

    Bohlin , R. C. 2007, in Astronomical Society of the Pacific Conference Series, Vol. 364, The Future of Photometric, Spectrophotometric and Polarimetric Standardization, ed. C. Sterken , 315

    work page 2007

  11. [11]

    2024, Experimental Astronomy, 58, 1

    B \"o rner , A., Paproth , C., Cabrera , J., et al. 2024, Experimental Astronomy, 58, 1

    work page 2024

  12. [12]

    J., Koch , D., Basri , G., et al

    Borucki , W. J., Koch , D., Basri , G., et al. 2010, Science, 327, 977

    work page 2010

  13. [13]

    2012, , 427, 127

    Bressan , A., Marigo , P., Girardi , L., et al. 2012, , 427, 127

    work page 2012

  14. [14]

    M., Latham , D

    Brown , T. M., Latham , D. W., Everett , M. E., & Esquerdo , G. A. 2011, , 142, 112

    work page 2011

  15. [15]

    M., et al

    Bryson , S., Coughlin , J., Batalha , N. M., et al. 2020, , 159, 279

    work page 2020

  16. [16]

    D., et al

    Casagrande , L., Lin , J., Rains , A. D., et al. 2021, , 507, 2684

    work page 2021

  17. [17]

    2010, , 512, A54

    Casagrande , L., Ram \' rez , I., Mel \'e ndez , J., Bessell , M., & Asplund , M. 2010, , 512, A54

    work page 2010

  18. [18]

    P., & Castilho , B

    Coelho , P., Barbuy , B., Mel \'e ndez , J., Schiavon , R. P., & Castilho , B. V. 2005, , 443, 735

    work page 2005

  19. [19]

    J., Tessarolo, E., Baccaro, S., et al

    Corso, A. J., Tessarolo, E., Baccaro, S., et al. 2018, Opt. Express, 26, 33841

    work page 2018

  20. [20]

    L., Sordo , R., Pailler , F., et al

    Creevey , O. L., Sordo , R., Pailler , F., et al. 2023, , 674, A26

    work page 2023

  21. [21]

    C., Moutou , C., et al

    Deleuil , M., Meunier , J. C., Moutou , C., et al. 2009, , 138, 649

    work page 2009

  22. [22]

    2020, , 496, 3887

    Eker , Z., Soydugan , F., Bilir , S., et al. 2020, , 496, 3887

    work page 2020

  23. [23]

    L., Massa , D., Gordon , K

    Fitzpatrick , E. L., Massa , D., Gordon , K. D., Bohlin , R., & Clayton , G. C. 2019, , 886, 108

    work page 2019

  24. [24]

    2013, , 766, 81

    Fressin , F., Torres , G., Charbonneau , D., et al. 2013, , 766, 81

    work page 2013

  25. [25]

    Gaia Collaboration , Brown , A. G. A., Vallenari , A., et al. 2021, , 650, C3

    work page 2021

  26. [26]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2023, , 674, A1

    work page 2023

  27. [27]

    Girardi , L., Groenewegen , M. A. T., Hatziminaoglou , E., & da Costa , L. 2005, A&A, 436, 895

    work page 2005

  28. [28]

    M., Hivon , E., Banday , A

    G \'o rski , K. M., Hivon , E., Banday , A. J., et al. 2005, , 622, 759

    work page 2005

  29. [29]

    L., Godolt , M., Cabrera , J., et al

    Grenfell , J. L., Godolt , M., Cabrera , J., et al. 2020, Experimental Astronomy, 50, 1

    work page 2020

  30. [30]

    & Sauval , A

    Grevesse , N. & Sauval , A. J. 1998, , 85, 161

    work page 1998

  31. [31]

    2016, in Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, ed

    Gullieuszik, M., Magrin, D., Greggio, D., et al. 2016, in Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, ed. H. A. MacEwen, G. G. Fazio, M. Lystrup, N. Batalha, N. Siegler, & E. C. Tong, Vol. 9904, International Society for Optics and Photonics (SPIE), 996 -- 1004

    work page 2016

  32. [32]

    2008, , 486, 951

    Gustafsson , B., Edvardsson , B., Eriksson , K., et al. 2008, , 486, 951

    work page 2008

  33. [33]

    W., Marcy , G

    Howard , A. W., Marcy , G. W., Bryson , S. T., et al. 2012, , 201, 15

    work page 2012

  34. [34]

    T., Haas , M

    Huber , D., Bryson , S. T., Haas , M. R., et al. 2016, , 224, 2

    work page 2016

  35. [35]

    M., Witzke , V., Shapiro , A

    Kostogryz , N. M., Witzke , V., Shapiro , A. I., et al. 2022, , 666, A60

    work page 2022

  36. [36]

    2018, , 616, A132

    Lallement , R., Capitanio , L., Ruiz-Dern , L., et al. 2018, , 616, A132

    work page 2018

  37. [37]

    L., Babusiaux , C., & Cox , N

    Lallement , R., Vergely , J. L., Babusiaux , C., & Cox , N. L. J. 2022, , 661, A147

    work page 2022

  38. [38]

    2016, in Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, ed

    Magrin, D., Ragazzoni, R., Bruno, G., et al. 2016, in Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, ed. H. A. MacEwen, G. G. Fazio, M. Lystrup, N. Batalha, N. Siegler, & E. C. Tong, Vol. 9904, International Society for Optics and Photonics (SPIE), 988 -- 995

    work page 2016

  39. [39]

    2018, in Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, ed

    Magrin, D., Ragazzoni, R., Rauer, H., et al. 2018, in Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, ed. M. Lystrup, H. A. MacEwen, G. G. Fazio, N. Batalha, N. Siegler, & E. C. Tong, Vol. 10698, International Society for Optics and Photonics (SPIE), 1462 -- 1471

    work page 2018

  40. [40]

    W., Feiden , G

    Mann , A. W., Feiden , G. A., Gaidos , E., Boyajian , T., & von Braun , K. 2015, , 804, 64

    work page 2015

  41. [41]

    2019, , 627, A71

    Marchiori , V., Samadi , R., Fialho , F., et al. 2019, , 627, A71

    work page 2019

  42. [42]

    M., et al

    Montalto , M., Piotto , G., Marrese , P. M., et al. 2021, , 653, A98

    work page 2021

  43. [43]

    J., & Davies , G

    Moya , A., Zuccarino , F., Chaplin , W. J., & Davies , G. R. 2018, , 237, 21

    work page 2018

  44. [44]

    2022, , 658, A31

    Nascimbeni , V., Piotto , G., B \"o rner , A., et al. 2022, , 658, A31

    work page 2022

  45. [45]

    2025, , 694, A313

    Nascimbeni , V., Piotto , G., Cabrera , J., et al. 2025, , 694, A313

    work page 2025

  46. [46]

    G., Collins , K

    Paegert , M., Stassun , K. G., Collins , K. A., et al. 2021, arXiv e-prints, arXiv:2108.04778

    work page arXiv 2021

  47. [47]

    2010, , 516, A13

    Palacios , A., Gebran , M., Josselin , E., et al. 2010, , 516, A13

    work page 2010

  48. [48]

    Pecaut , M. J. & Mamajek , E. E. 2013, ApJS, 208, 9

    work page 2013

  49. [49]

    2026, , 706, A207

    Prisinzano , L., Montalto , M., Piotto , G., et al. 2026, , 706, A207

    work page 2026

  50. [50]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Ragazzoni , R., Magrin , D., Rauer , H., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9904, Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, ed. H. A. MacEwen , G. G. Fazio , M. Lystrup , N. Batalha , N. Siegler , & E. C. Tong , 990428

    work page 2016

  51. [51]

    2025, Experimental Astronomy, 59, 26

    Rauer , H., Aerts , C., Cabrera , J., et al. 2025, Experimental Astronomy, 59, 26

    work page 2025

  52. [52]

    R., Winn , J

    Ricker , G. R., Winn , J. N., Vanderspek , R., et al. 2014, in , Vol. 9143, Space Telescopes and Instrumentation 2014: Optical, Infrared, and Millimeter Wave, 914320

    work page 2014

  53. [53]

    W., et al

    Riello , M., De Angeli , F., Evans , D. W., et al. 2021, , 649, A3

    work page 2021

  54. [54]

    F., Almenara , J

    Santerne , A., D \' az , R. F., Almenara , J. M., et al. 2015, , 451, 2337

    work page 2015

  55. [55]

    G., Oelkers , R

    Stassun , K. G., Oelkers , R. J., Paegert , M., et al. 2019, , 158, 138

    work page 2019

  56. [56]

    G., Oelkers , R

    Stassun , K. G., Oelkers , R. J., Pepper , J., et al. 2018, AJ, 156, 102

    work page 2018

  57. [57]

    Taylor , M. B. 2005, in Astronomical Society of the Pacific Conference Series, Vol. 347, Astronomical Data Analysis Software and Systems XIV, ed. P. Shopbell , M. Britton , & R. Ebert , 29

    work page 2005

  58. [58]

    2018, in Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, ed

    Umbriaco, G., Biondi, F., Farinato, J., et al. 2018, in Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, ed. M. Lystrup, H. A. MacEwen, G. G. Fazio, N. Batalha, N. Siegler, & E. C. Tong, Vol. 10698, International Society for Optics and Photonics (SPIE), 1278 -- 1290

    work page 2018

  59. [59]

    L., Lallement , R., & Cox , N

    Vergely , J. L., Lallement , R., & Cox , N. L. J. 2022, , 664, A174

    work page 2022

  60. [60]

    S., Basu , S., Ong J

    Viani , L. S., Basu , S., Ong J. , M. J., Bonaca , A., & Chaplin , W. J. 2018, , 858, 28

    work page 2018

  61. [61]

    I., Cernetic , M., et al

    Witzke , V., Shapiro , A. I., Cernetic , M., et al. 2021, , 653, A65

    work page 2021