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arxiv: 2606.26214 · v1 · pith:BMZY3R6Knew · submitted 2026-06-24 · 🌌 astro-ph.IM · astro-ph.EP

Nautilus Space Observatory: The Evolution of Planets and their Atmospheres

Ilaria Pascucci , Noah Tuchow , Yifan Zhou , Daniel Apai , Chaucer Langbert , Ana Glidden , Luis Welbanks , Chia-Lung Lin
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Adina D. Feinstein Benjamin V. Rackham Peter Plavchan Kevin Wagner Raymond Pierrehumbert Robin Wordsworth
This is my paper

Pith reviewed 2026-06-26 01:37 UTC · model grok-4.3

classification 🌌 astro-ph.IM astro-ph.EP
keywords exoplanet atmospheresplanetary evolutionatmospheric mass lossspace telescope constellationsub-Neptunessuper-Earthshelium atmospheresdisks to planets
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The pith

A proposed constellation of large space telescopes called Nautilus would enable statistical tracking of how planetary atmospheres change from young disks to mature systems over billions of years.

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

The paper lays out four science goals for understanding planet evolution that current telescopes cannot address at scale: measuring how long it takes planets to shrink into sub-Neptunes or super-Earths, following how fast atmospheres lose mass at different ages, watching shifts in atmospheric composition such as mean molecular weight and carbon-to-oxygen ratio, and spotting the first helium-rich worlds. It states that these goals require high spatial resolution, wide wavelength coverage, large light-collecting area, and the ability to observe many targets in parallel. The Nautilus design, a fleet of large-diameter space telescopes working together, is presented as the facility that supplies exactly those capabilities. Achieving the goals would link early planet formation in disks to the properties of older exoplanets and support broader NASA programs on cosmic origins and exoplanets.

Core claim

Nautilus provides the high spatial resolution, broad-wavelength coverage, large effective area, and parallelized multiple units required to determine the timescales over which planets evolve into sub-Neptunes and super-Earths, to track the temporal evolution of atmospheric mass-loss rates, to characterize the evolution of atmospheric mean molecular weight and C/O ratio, and to identify the emergence of Helium-dominated worlds.

What carries the argument

The Nautilus Space Observatory, a proposed constellation of large-diameter space telescopes whose multiple units operate in parallel to deliver the resolution, wavelength range, and collecting power needed for population-level atmospheric studies across planet ages.

If this is right

  • The time required for young planets to lose envelope mass and settle into sub-Neptune or super-Earth sizes becomes measurable from direct observations.
  • Atmospheric escape rates can be compared across orbital periods and system ages to reveal how mass loss changes with time.
  • Trends in atmospheric mean molecular weight and carbon-to-oxygen ratio can be mapped as planets age, showing when and how compositions stabilize.
  • The first helium-dominated atmospheres can be identified in older systems, marking a distinct late stage of evolution.

Where Pith is reading between the lines

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

  • Such data would let observers test whether the same physical processes explain both the sizes of young planets seen in disks and the sizes of older field planets.
  • Results could prioritize targets for detailed follow-up with other instruments by identifying which evolutionary stages still need closer study.
  • The approach could be extended to compare atmospheric evolution in different stellar environments once enough systems are observed.

Load-bearing premise

Existing telescopes cannot gather enough simultaneous, high-quality data on atmospheres of many planets spanning young to old ages to perform the needed statistical studies.

What would settle it

A published survey using current or approved telescopes that measures atmospheric mass-loss rates, mean molecular weight, or C/O ratios across a statistically meaningful sample of planets at different ages would show the studies are already feasible without Nautilus.

Figures

Figures reproduced from arXiv: 2606.26214 by Adina D. Feinstein, Ana Glidden, Benjamin V. Rackham, Chaucer Langbert, Chia-Lung Lin, Daniel Apai, Ilaria Pascucci, Kevin Wagner, Luis Welbanks, Noah Tuchow, Peter Plavchan, Raymond Pierrehumbert, Robin Wordsworth, Yifan Zhou.

Figure 1
Figure 1. Figure 1: Figure summarizing the key science objectives. 3. DATA REQUIREMENTS Of the science objectives outlined above, only the first can be achieved with broad-band photometry while the others require transmission spectroscopy. • Photometry: Multiple filters (∼ 3) are required for photometric transit searches of young exoplanets and for validating detections. A 2-10 minute cadence is sufficient for this science ca… view at source ↗
read the original abstract

We are just beginning to explore the billion-year evolution from nascent planets in disks to mature planetary systems. Recent discoveries hint at demographic and atmospheric differences between young planets and their Gyr-old counterparts, but current facilities are limited - particularly in their ability to conduct statistical atmospheric studies over a broad period range. This white paper outlines compelling science achievable with the Nautilus Space Observatory, a proposed constellation of large-diameter space telescopes. We identify four primary scientific objectives: (1) determining the timescales over which planets evolve into sub-Neptunes and super-Earths; (2) tracking the temporal evolution of atmospheric mass-loss rates; (3) characterizing the evolution of the atmospheric mean molecular weight and C/O ratio; and (4) identifying the emergence of Helium-dominated worlds. Answering these questions requires the high spatial resolution, broad-wavelength coverage, large effective area, and parallelized multiple units that Nautilus provides. By isolating the physical processes that govern the evolution of planets and their atmospheres, these science objectives directly support NASA's Cosmic Origins and Exoplanet Exploration Programs.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 1 minor

Summary. This white paper proposes the Nautilus Space Observatory, a constellation of large-diameter space telescopes, to address four science objectives on the billion-year evolution of planets and atmospheres: (1) timescales for evolution into sub-Neptunes and super-Earths; (2) temporal evolution of atmospheric mass-loss rates; (3) evolution of atmospheric mean molecular weight and C/O ratio; and (4) emergence of Helium-dominated worlds. It asserts that current facilities cannot perform the required statistical atmospheric studies over a broad period range and that Nautilus's high spatial resolution, broad-wavelength coverage, large effective area, and parallelized units are necessary to isolate the governing physical processes, supporting NASA's Cosmic Origins and Exoplanet Exploration Programs.

Significance. If the observational requirements case holds, the proposal would outline a coherent set of objectives for advancing demographic and atmospheric studies of young versus mature exoplanets, providing a forward-looking justification for new space-based capabilities that could enable statistical samples not currently feasible.

major comments (2)
  1. [Abstract] Abstract: the central premise that 'current facilities are limited - particularly in their ability to conduct statistical atmospheric studies over a broad period range' is stated without any quantitative comparison of existing or planned telescope capabilities, sensitivity limits, or example studies that fail, which is load-bearing for the justification that Nautilus is required.
  2. [Abstract] Abstract: the four objectives are presented as requiring Nautilus's specific capabilities, but no mapping is given from each objective to the minimum required resolution, wavelength range, collecting area, or number of parallel units, leaving the 'requires' claim unsupported by any requirements analysis or simulation.
minor comments (1)
  1. [Abstract] Abstract: references to 'recent discoveries' that 'hint at demographic and atmospheric differences' are not accompanied by citations, reducing traceability of the motivating premise.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments on the Nautilus white paper. We address each major comment below and agree that targeted revisions to the abstract and supporting sections will strengthen the manuscript.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central premise that 'current facilities are limited - particularly in their ability to conduct statistical atmospheric studies over a broad period range' is stated without any quantitative comparison of existing or planned telescope capabilities, sensitivity limits, or example studies that fail, which is load-bearing for the justification that Nautilus is required.

    Authors: We agree that the abstract would benefit from quantitative support for this premise. In the revised manuscript we will expand the abstract and add a short capabilities-comparison paragraph (or table) that cites published sensitivity limits and sample sizes from JWST, HST, and ground-based facilities for young (<100 Myr) planets, showing the current shortfall in achieving statistical atmospheric characterization across a wide age baseline. revision: yes

  2. Referee: [Abstract] Abstract: the four objectives are presented as requiring Nautilus's specific capabilities, but no mapping is given from each objective to the minimum required resolution, wavelength range, collecting area, or number of parallel units, leaving the 'requires' claim unsupported by any requirements analysis or simulation.

    Authors: We acknowledge the value of an explicit requirements trace. The revised version will include a concise traceability table (or bullet list) that maps each of the four science objectives to the minimum needed spectral resolution, wavelength coverage, effective area, and number of parallel apertures, drawing on the exposure-time estimates already present in the full white-paper text. revision: yes

Circularity Check

0 steps flagged

No significant circularity

full rationale

This is a mission white paper outlining science objectives and required telescope capabilities. It contains no equations, derivations, parameter fits, or load-bearing self-citations. The central claim is an assertion of observational requirements for listed goals, not a result derived from inputs that loop back by construction. No steps match any enumerated circularity pattern.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

No free parameters, axioms, or invented entities are identifiable from the abstract alone.

pith-pipeline@v0.9.1-grok · 5770 in / 1013 out tokens · 9691 ms · 2026-06-26T01:37:49.201073+00:00 · methodology

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Reference graph

Works this paper leans on

36 extracted references · 36 canonical work pages · 1 internal anchor

  1. [1]

    The Disk Substructures at High Angular Resolution Project (DSHARP): I. Motivation, Sample, Calibration, and Overview

    Andrews, S. M., Huang, J., P´ erez, L. M., et al. 2018, ApJL, 869, L41, doi: 10.3847/2041-8213/aaf741

    work page internal anchor Pith review doi:10.3847/2041-8213/aaf741 2018

  2. [2]

    D., Kim, D

    Apai, D., Milster, T. D., Kim, D. W., et al. 2019, AJ, 158, 83, doi: 10.3847/1538-3881/ab2631

    work page doi:10.3847/1538-3881/ab2631 2019

  3. [3]

    2025, AJ, 170, 165, doi: 10.3847/1538-3881/adec89

    Barat, S., D´ esert, J.-M., Mukherjee, S., et al. 2025, AJ, 170, 165, doi: 10.3847/1538-3881/adec89

    work page doi:10.3847/1538-3881/adec89 2025

  4. [4]

    G., Mann, A

    Barber, M. G., Mann, A. W., Vanderburg, A., Boyle, A. W., & Lopez Murillo, A. I. 2025, AJ, 170, 32, doi: 10.3847/1538-3881/add7db

    work page doi:10.3847/1538-3881/add7db 2025

  5. [5]

    J., Hellier, C., et al

    Barkaoui, K., Pozuelos, F. J., Hellier, C., et al. 2024, Nature Astronomy, 8, 909, doi: 10.1038/s41550-024-02259-y

    work page doi:10.1038/s41550-024-02259-y 2024

  6. [6]

    E., & Line, M

    Batalha, N. E., & Line, M. R. 2017, AJ, 153, 151, doi: 10.3847/1538-3881/aa5faa

    work page doi:10.3847/1538-3881/aa5faa 2017

  7. [7]

    2013, ApJ, 778, 153, doi: 10.1088/0004-637X/778/2/153

    Benneke, B., & Seager, S. 2013, ApJ, 778, 153, doi: 10.1088/0004-637X/778/2/153

    work page doi:10.1088/0004-637x/778/2/153 2013

  8. [8]

    J., Pascucci, I., Mulders, G

    Bergsten, G. J., Pascucci, I., Mulders, G. D., Fernandes, R. B., & Koskinen, T. T. 2022, AJ, 164, 190, doi: 10.3847/1538-3881/ac8fea

    work page doi:10.3847/1538-3881/ac8fea 2022

  9. [9]

    2024, Nature Astronomy, 8, 463, doi: 10.1038/s41550-023-02183-7

    Burn, R., Mordasini, C., Mishra, L., et al. 2024, Nature Astronomy, 8, 463, doi: 10.1038/s41550-023-02183-7

    work page doi:10.1038/s41550-023-02183-7 2024

  10. [10]

    J., et al

    Cherubim, C., Wordsworth, R., Bower, D. J., et al. 2025, ApJ, 983, 97, doi: 10.3847/1538-4357/adbca9

    work page doi:10.3847/1538-4357/adbca9 2025

  11. [11]

    2024, ApJ, 967, 139, doi: 10.3847/1538-4357/ad3e77

    Cherubim, C., Wordsworth, R., Hu, R., & Shkolnik, E. 2024, ApJ, 967, 139, doi: 10.3847/1538-4357/ad3e77

    work page doi:10.3847/1538-4357/ad3e77 2024

  12. [12]

    L., Zink, J

    Christiansen, J. L., Zink, J. K., Hardegree-Ullman, K. K., et al. 2023, AJ, 166, 248, doi: 10.3847/1538-3881/acf9f9

    work page doi:10.3847/1538-3881/acf9f9 2023

  13. [13]

    2024, AJ, 168, 239, doi: 10.3847/1538-3881/ad83a6

    Dai, F., Goldberg, M., Batygin, K., et al. 2024, AJ, 168, 239, doi: 10.3847/1538-3881/ad83a6

    work page doi:10.3847/1538-3881/ad83a6 2024

  14. [14]

    B., Mulders, G

    Fernandes, R. B., Mulders, G. D., Pascucci, I., et al. 2022, AJ, 164, 78, doi: 10.3847/1538-3881/ac7b29

    work page doi:10.3847/1538-3881/ac7b29 2022

  15. [15]

    B., Bergsten, G

    Fernandes, R. B., Bergsten, G. J., Mulders, G. D., et al. 2025, AJ, 169, 208, doi: 10.3847/1538-3881/adb97e

    work page doi:10.3847/1538-3881/adb97e 2025

  16. [16]

    J., Petigura, E

    Fulton, B. J., Petigura, E. A., Howard, A. W., et al. 2017, AJ, 154, 109, doi: 10.3847/1538-3881/aa80eb

    work page doi:10.3847/1538-3881/aa80eb 2017

  17. [17]

    E., & Sari, R

    Ginzburg, S., Schlichting, H. E., & Sari, R. 2018, MNRAS, 476, 759, doi: 10.1093/mnras/sty290

    work page doi:10.1093/mnras/sty290 2018

  18. [18]

    V., Luna, J., et al

    Gully-Santiago, M., Morley, C. V., Luna, J., et al. 2024, AJ, 167, 142, doi: 10.3847/1538-3881/ad1ee8

    work page doi:10.3847/1538-3881/ad1ee8 2024

  19. [19]

    Hu, R., Seager, S., & Yung, Y. L. 2015, ApJ, 807, 8, doi: 10.1088/0004-637X/807/1/8

    work page doi:10.1088/0004-637x/807/1/8 2015

  20. [20]

    S., & Barnett, M

    Kite, E. S., & Barnett, M. N. 2020, Proceedings of the National Academy of Science, 117, 18264, doi: 10.1073/pnas.2006177117

    work page doi:10.1073/pnas.2006177117 2020

  21. [21]

    2022, ApJS, 259, 33, doi: 10.3847/1538-4365/ac5688 Lamp´ on, M., L´ opez-Puertas, M., Sanz-Forcada, J., et al

    Kunimoto, M., Daylan, T., Guerrero, N., et al. 2022, ApJS, 259, 33, doi: 10.3847/1538-4365/ac5688 Lamp´ on, M., L´ opez-Puertas, M., Sanz-Forcada, J., et al. 2021, A&A, 647, A129, doi: 10.1051/0004-6361/202039417

    work page doi:10.3847/1538-4365/ac5688 2022

  22. [22]

    C., Oklopˇ ci´ c, A., & MacLeod, M

    Linssen, D. C., Oklopˇ ci´ c, A., & MacLeod, M. 2022, A&A, 667, A54, doi: 10.1051/0004-6361/202243830

    work page doi:10.1051/0004-6361/202243830 2022

  23. [23]

    J., Batalha, N

    Lissauer, J. J., Batalha, N. M., & Borucki, W. J. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka, Y. Aikawa, T. Muto, K. Tomida, & M. Tamura, 839, doi: 10.48550/arXiv.2311.04981

    work page doi:10.48550/arxiv.2311.04981 2023

  24. [24]

    J., Rowe, J

    Lissauer, J. J., Rowe, J. F., Jontof-Hutter, D., et al. 2024, PSJ, 5, 152, doi: 10.3847/PSJ/ad0e6e

    work page doi:10.3847/psj/ad0e6e 2024

  25. [25]

    J., et al

    Long, F., Pinilla, P., Herczeg, G. J., et al. 2018, ApJ, 869, 17, doi: 10.3847/1538-4357/aae8e1

    work page doi:10.3847/1538-4357/aae8e1 2018

  26. [26]

    I., & Hu, Y

    Madhusudhan, N., Ag´ undez, M., Moses, J. I., & Hu, Y. 2016, SSRv, 205, 285, doi: 10.1007/s11214-016-0254-3

    work page doi:10.1007/s11214-016-0254-3 2016

  27. [27]

    W., Vanderburg, A., Rizzuto, A

    Mann, A. W., Vanderburg, A., Rizzuto, A. C., et al. 2018, AJ, 155, 4, doi: 10.3847/1538-3881/aa9791 National Academies of Sciences, & Medicine, E. 2021, Pathways to Discovery in Astronomy and Astrophysics for the 2020s, doi: 10.17226/26141

    work page doi:10.3847/1538-3881/aa9791 2018

  28. [28]

    2024, Journal of Geophysical Research (Planets), 129, 2024JE008576, doi: 10.1029/2024JE008576

    Pierrehumbert, R. 2024, Journal of Geophysical Research (Planets), 129, 2024JE008576, doi: 10.1029/2024JE008576

    work page doi:10.1029/2024je008576 2024

  29. [29]

    E., & Wu, Y

    Owen, J. E., & Wu, Y. 2017, ApJ, 847, 29, doi: 10.3847/1538-4357/aa890a

    work page doi:10.3847/1538-4357/aa890a 2017

  30. [30]

    J., et al

    Pascucci, I., Testi, L., Herczeg, G. J., et al. 2016, ApJ, 831, 125, doi: 10.3847/0004-637X/831/2/125

    work page doi:10.3847/0004-637x/831/2/125 2016

  31. [31]

    Rogers, J. G. 2025, MNRAS, 539, 2230, doi: 10.1093/mnras/staf628

    work page doi:10.1093/mnras/staf628 2025

  32. [32]

    J., Fulton, B

    Rosenthal, L. J., Fulton, B. J., Hirsch, L. A., et al. 2021, ApJS, 255, 8, doi: 10.3847/1538-4365/abe23c

    work page doi:10.3847/1538-4365/abe23c 2021

  33. [33]

    C., Mann, A

    Thao, P. C., Mann, A. W., Feinstein, A. D., et al. 2024, AJ, 168, 297, doi: 10.3847/1538-3881/ad81d7

    work page doi:10.3847/1538-3881/ad81d7 2024

  34. [34]

    X., et al

    Vach, S., Zhou, G., Huang, C. X., et al. 2024, AJ, 167, 210, doi: 10.3847/1538-3881/ad3108

    work page doi:10.3847/1538-3881/ad3108 2024

  35. [35]

    2019, AJ, 157, 206, doi: 10.3847/1538-3881/ab14de

    Welbanks, L., & Madhusudhan, N. 2019, AJ, 157, 206, doi: 10.3847/1538-3881/ab14de

    work page doi:10.3847/1538-3881/ab14de 2019

  36. [36]

    M., Pascucci, I., et al

    Zhang, K., P´ erez, L. M., Pascucci, I., et al. 2025, ApJ, 989, 1, doi: 10.3847/1538-4357/addebe

    work page doi:10.3847/1538-4357/addebe 2025