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REVIEW 7 minor 68 references

The science target sets wavelength and resolution, which fix baseline, architecture, and risk—and shared technologies maturing as flagship byproducts now decide which interferometer concepts become missions.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

T0 review · grok-4.5

2026-07-13 06:45 UTC pith:VPYRXBD7

load-bearing objection Solid invited landscape review: clear science-to-architecture map and a usable six-point roadmap, not a new result.

arxiv 2607.07746 v2 pith:VPYRXBD7 submitted 2026-07-08 astro-ph.IM astro-ph.EP

Space and Lunar Interferometry: Emerging Concepts and Pathways

classification astro-ph.IM astro-ph.EP
keywords astronomical interferometryspace interferometrylunar interferometrynulling interferometryformation flyingoptical interferometryinfrared interferometrylunar farside radio astronomy
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This review argues that space and lunar interferometry have left pure aspiration and now form a concrete landscape of free-flying, lunar-surface, structurally connected, and hybrid space-VLBI concepts. What organizes that landscape is a simple chain: the science goal sets the wavelength and the needed angular resolution; those fix the baseline; the baseline chooses the architecture and the main engineering risk. Across mid-infrared nulling for temperate exoplanets, far-side radio for the low-frequency Universe, lunar UV/optical imaging and microarcsecond astrometry, far-IR and X-ray concepts, and lunar laser strain measurement for mid-band gravitational waves, the same enabling stack appears—formation flying, absolute metrology, beam combination and nulling, cryogenics, and autonomous deployment. Those capabilities are rising largely as byproducts of other flagship programs, so technology inheritance, not only science ranking, increasingly decides which concepts fly. The coming decade’s real choices are pathfinder sequencing on both free-flying and lunar tracks, retirement of a few tall poles, and funding models that can carry integrated end-to-end demos from the lab to flight readiness.

Core claim

Off-Earth interferometry is best organized not by platform slogan but by a science-to-architecture map: science target fixes wavelength regime and angular resolution, which fix baseline scale, which in turn select free-flying, structurally connected, or surface-deployed architecture and dominate implementation risk. Across that map the concepts converge on shared enabling technologies that mature mainly as byproducts of flagship programs, and that inheritance dynamic increasingly governs which concepts become missions.

What carries the argument

The science-to-architecture map (science → wavelength and angular resolution θ ≈ λ/B → baseline → architecture and dominant risk), together with the shared enabling stack of precision formation flying, absolute metrology, beam combination/nulling, cryogenics, and autonomous deployment, which unites otherwise diverse pathways and sets the roadmap decisions.

Load-bearing premise

That small, low-cost pathfinders will actually be funded and flown often enough to retire system risk and create the first real cost and schedule anchors for larger missions, rather than staying on paper.

What would settle it

Whether at least one funded end-to-end free-flying pathfinder achieves first stellar fringes from separated spacecraft, and whether a CLPS-scale lunar single-baseline optical precursor flies and produces coherent fringes—both within the coming decade’s opportunity windows.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Free-flying mid-infrared nulling remains the strongest near-term path to thermal spectra of temperate rocky exoplanets complementary to reflected-light flagships.
  • Lunar far-side radio can open frequencies blocked on Earth if relay, power, and radio-quiet governance keep pace with surface infrastructure.
  • Lunar UV/optical arrays and fixed-baseline astrometry can supply dynamical masses and stellar-surface imaging that direct-imaging target selection needs.
  • Coordinated investment in absolute metrology and cryogenic deep nulling retires risk across many concepts more efficiently than isolated mission lines.
  • Small flown precursors create the missing cost and schedule reference class that no astronomical space interferometer has yet provided.

Where Pith is reading between the lines

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

  • Without a competed flight line at pathfinder scale, the inheritance dynamic the paper describes may favor only those interferometry pieces that piggyback on already-selected flagships, narrowing the portfolio unevenly.
  • Treating free-flying and lunar tracks as parallel fail-fast experiments implies that agency and private capital must accept partial technical dead-ends as the price of schedule anchors.
  • Spectrum and site protection on the far side may become as load-bearing as any antenna or correlator design once commercial lunar assets proliferate.
  • If first stellar fringes in free flight slip past the decade, cost models for formation-flying observatories will remain unanchored longer than the science cases can stay politically fresh.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

0 major / 7 minor

Summary. This invited review surveys the landscape of space- and lunar-based interferometry, organizing free-flying, structurally connected, hybrid VLBI, and lunar-surface concepts by a science-to-architecture map: science target sets wavelength and angular resolution, which fix baseline, architecture, and dominant risk (Abstract; Sect. 2; Table 1; Figs. 1–2). It covers mid-IR nulling (LIFE and bridge concepts), far-IR (SPIRIT/SPICE), space VLBI (BHEX, SunRISE), X-ray, lunar UV/optical (AeSI, MoonLITE, astrometry for HWO), far-side radio (FARSIDE, FarView, LuSEE-Night), and lunar GW strain (LILA). Shared enabling technologies—formation flying/metrology, beam combination/nulling, cryogenics, deployment, and data architectures—are argued to mature largely as flagship byproducts and thereby govern which concepts become missions (Sect. 5; Fig. 3). The paper closes with six strategic decisions for the coming decade and a discussion of funding models, including catalytic private/philanthropic roles (Sect. 7–7.1; Appendix A).

Significance. As a landscape and roadmap review rather than a new empirical or theoretical result, the paper’s value lies in a clear, consistently applied science-to-architecture organizing principle and an up-to-date synthesis spanning Darwin/TPF-I heritage through 2024–2026 pathfinders (PROBA-3, STARI, SEIRIOS, NICE, LuSEE-Night, etc.). Table 1 and Figs. 1–3 make the trade space legible across wavelengths and platforms; the explicit treatment of LILA as strain rather than angular resolution is carefully handled. The roadmap (Sect. 7) and funding discussion (7.1) are concrete and actionable for the community. Strengths include extensive, correctly cited primary literature (73 references), yield and baseline numbers taken from the source studies rather than re-derived, and an honest framing of pathfinder funding and cost-anchor gaps as open decisions rather than hidden premises.

minor comments (7)
  1. Abstract and opening paragraphs: the free-flying / lunar-surface / structurally-connected / hybrid taxonomy is stated slightly differently in the Abstract versus the first full paragraph of the Introduction; a single consistent phrasing would help readers.
  2. Table 1 and Fig. 1 notes: the soft boundaries and the special status of LILA (strain, not θ ≈ λ/B) are well noted, but a one-line pointer in the table caption that maturity boxes are qualitative (not formal TRL) would match the figure notes and reduce any misreading.
  3. Sect. 3.1: LIFE yield numbers (~550 / ~770 planets; rocky HZ counts) are correctly attributed to Quanz et al. and follow-on papers; a brief parenthetical that these are model-dependent (throughput, exozodi, target list) would help non-specialist readers without changing the claim.
  4. Sect. 5.1 / 5.4: absolute-metrology thresholds (~10 nm visible/UV; differential OPD for deep nulls) are stated clearly; a short cross-reference to the wavelength scaling already used in Table 1 would tighten the link between architecture risk and technology tall poles.
  5. Sect. 7 point 2 and 7.1: the ‘fail fast / startup mentality’ and philanthropic-catalytic language is appropriate for a roadmap but slightly more informal than the rest of the review; a single sentence tying it back to the absence of a flown cost-reference class (SIM cancellation) would keep the tone uniform.
  6. References: a few arXiv-only or ‘in press’ items (e.g., recent SPIE/NICE/KISS entries) will need final bibliographic updates at proof stage; no substantive citation errors were found.
  7. Appendix A figures: A1–A2 are useful schematic summaries; ensuring they remain clearly labeled as indicative (not programmatic timelines) in the final layout will avoid over-interpretation.

Circularity Check

0 steps flagged

Invited landscape review with normal self-citation of the author's AeSI/MoonLITE work; no derivation, prediction, or uniqueness claim reduces to its inputs by construction.

full rationale

This is an invited survey of mission concepts, pathfinders, and technology pathways, not a first-principles derivation or empirical prediction paper. Its central organizational claim—that science target sets wavelength and angular resolution, which fix baseline, architecture, and dominant risk, while shared enabling technologies mature as flagship byproducts—is a framing device supported by independent literature (LIFE yield studies, FARSIDE/FarView, SPIRIT/SPICE, BHEX, PROBA-3, GRACE-FO LRI, LISA Pathfinder, NOTT/NICE, etc.). The author cites her own AeSI NIAC reports and related KISS/MoonLITE studies when describing the lunar UV/optical pathway; that is ordinary and expected in an invited review of a landscape the author has helped shape. Those self-citations are not load-bearing for any uniqueness theorem, fitted parameter renamed as prediction, or self-definitional identity. There are no equations that equate a claimed output to a fitted input, no ansatz smuggled in via prior author work, and no renaming of a known empirical pattern presented as novel unification. The programmatic contingency that small pathfinders must actually fly is treated explicitly as an open decision of the coming decade (Sect. 7), not as a hidden premise required for the science-to-architecture map. Score 1 reflects only the presence of non-load-bearing self-citation; the bulk of the landscape is independent and the paper contains no circular derivation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 4 axioms · 0 invented entities

As a review the paper inherits the domain assumptions of the cited mission studies rather than introducing free parameters or new entities. The load-bearing premises are standard astrophysical scaling (θ ≈ λ/B), the empirical performance of flown formation-flying and metrology demos, and the programmatic claim that small pathfinders can create cost anchors.

axioms (4)
  • standard math Angular resolution of an interferometer scales as θ ≈ λ/B
    Used throughout Sect. 2, Figs. 1–2 and Table 1 to map science targets onto baseline requirements.
  • domain assumption Flown demonstrations (PROBA-3 mm-level formation, GRACE-FO nm ranging, LISA Pathfinder pm metrology) provide relevant heritage for free-flying optical interferometry
    Invoked in Sect. 5.1 and Sect. 7 point 1 as the foundation for claiming that subsystem risk is largely retired.
  • domain assumption Lunar far side remains radio-quiet enough for low-frequency cosmology once local Artemis-era RFI is governed
    Underpins the entire lunar radio pathway (Sect. 4.2); policy and spectrum-allocation assumptions are stated but not proven.
  • ad hoc to paper Small flown precursors establish credible cost and schedule anchors for later flagships
    Central to the multi-track strategy of Sect. 7 points 1–2; no historical counter-example of a space interferometer is available because none has flown.

pith-pipeline@v1.1.0-grok45 · 34955 in / 2562 out tokens · 25346 ms · 2026-07-13T06:45:37.763075+00:00 · methodology

0 comments
read the original abstract

Space- and lunar-based interferometry are moving from aspiration toward a concrete landscape of mission studies, pathfinders, and staged architectures. This invited review surveys that landscape across two principal platform pathways: free-flying and lunar-surface interferometers - plus structurally connected designs and hybrid space-VLBI arrays. I trace how the science target sets the wavelength regime and angular resolution, which in turn fix the baseline, architecture, and implementation risk. Mid-infrared nulling concepts such as LIFE target temperate exoplanets through thermal-emission spectroscopy; lunar far-side radio arrays (FARSIDE, FarView) open the low-frequency Universe from the only radio-quiet site in the inner Solar System; lunar UV/optical concepts (Artemis-enabled Stellar Imager, MoonLITE) revisit imaging of stellar surfaces and open a path to microarcsecond astrometry for the dynamical masses that Habitable Worlds Observatory target selection requires; far-infrared interferometers (SPIRIT/SPICE), space VLBI (BHEX), and X-ray concepts extend the reach to planet formation, high-redshift galaxies, and black-hole physics; and lunar laser interferometry (LILA) applies the lunar platform to mid-band gravitational waves, measuring strain rather than angular position. Across this range, the concepts share enabling technologies - precision formation flying, absolute metrology, beam combination and nulling, cryogenics, and autonomous deployment - maturing largely as byproducts of flagship programs, a dynamic that increasingly governs which concepts become missions. I summarize the pathways in baseline, wavelength, science return, deployment strategy, and risk, and close with the decisions of the coming decade: pathfinder sequencing, technology tall poles, and the funding models that can carry technologies from laboratory demonstration to flight readiness.

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Reference graph

Works this paper leans on

68 extracted references · 25 linked inside Pith

  1. [1]

    FREE-FLYING SPACE INTERFEROMETRY 3.1 Mid-infrared nulling for exoplanets In nulling interferometry, the apertures are combined so that on-axis starlight destructively interferes and is suppressed – the interferometric analogue of a coronagraph – revealing the faint thermal emission of off-axis planetary companions. The free-flying Large Interferometer For...

  2. [2]

    flyby without the flyby,

    LUNAR INTERFEROMETRY Having surveyed space-based concepts – free-flying formations and their structurally connected and single-spacecraft variants – we turn to the lunar surface, the second principal platform. Free-flying and surface-deployed architectures are best understood as a trade in which each removes the other's hardest problem. Free-flying archit...

  3. [3]

    long poles

    ENABLING TECHNOLOGIES The concepts surveyed above diverge widely in science and architecture, yet they converge on a set of enabling capabilities. Mapping architectures to capabilities to enabling technologies unites these concepts under a common ontology, and motivates cooperative work: the same technologies recur across mission concepts and wavelengths,...

  4. [4]

    RELATIONSHIP TO GROUND INTERFEROMETRY AND LARGE-APERTURE FACILITIES Space-based interferometers complement rather than replace ground facilities, which occupy two ends of a trade. The CHARA Array holds the longest optical baselines, up to 331 m, achieving angular resolutions of 0.20 milliarcseconds (mas) in the visible and 0.7 mas in the K-band with 1-m-c...

  5. [5]

    The decade ahead will therefore be defined less by selecting a single 'winner' than by strategic choices that require international and cross-sector collaboration

    ROADMAP AND KEY DECISIONS FOR THE COMING DECADE The concepts surveyed in this review are distinct in science and architecture, yet they rest on a shared interferometric logic, and, as Section 5 showed, on a shared technology base. The decade ahead will therefore be defined less by selecting a single 'winner' than by strategic choices that require internat...

  6. [6]

    first stellar fringes from separated free-flying spacecraft in space,

    First, fly at least one end-to-end astronomical formation-flying pathfinder. The constituent subsystems have largely been demonstrated in isolation: ESA’s PROBA-3 has retired much of the precision station-keeping and relative metrology risks, and STARI is designed to retire starlight acquisition, beam steering, and single-mode-fiber injection. However, no...

  7. [7]

    the free-flyer versus lunar-surface fork

    Second, even though many propose to resolve “the free-flyer versus lunar-surface fork”, I’d like to propose here a different approach: start small on each end, pursuing small-scale risk reduction on both frontiers: demonstrating initial feasibility and first fringes, through a rapid-iteration paradigm before scaling: fail fast, and build on what works, as...

  8. [8]

    Fourth, treat the two cross-cutting technology tall poles as the real near-term investment decision. (1) Absolute metrology at the ten-nanometer to tens-of-picometer level gates the visible/UV imaging and astrometric concepts; while (2) cryogenic deep nulling (targeting raw null depths of order 10 ⁻⁵ and effective depths approaching 10 ⁻⁸ via phase choppi...

  9. [9]

    Fifth, recognize that near-term progress is often paced less by science or technology readiness than by opportunity availability. Several of the concepts reviewed here are mature enough to be proposed, but lack a competed flight line at the appropriate scale and cadence; the lunar precursors in particular have at times had no open, suitably-scoped federal...

  10. [10]

    Sixth, treat international coordination as an explicit strategic choice. Space interferometry has transitioned into a genuinely multi-agency endeavor: JAXA is advancing dedicated formation-flying demonstrations [24, 34]; ESA maintains key mid-infrared exoplanet and X-ray initiatives alongside its precision formation-flying flight heritage; the United Stat...

  11. [11]

    Detection of the gravitational redshift in the orbit of the star S2,

    CONCLUSIONS Space and lunar interferometry offer a unique and unparalleled range of opportunities for the next generation of high-angular-resolution observatories. As surveyed in this review, the different architectural tracks populate complementary regions of discovery space: free-flying mid-infrared nulling holds the strongest near-term case for the atm...

  12. [12]

    MATISSE, the VLTI mid-infrared imaging spectro-interferometer,

    Lopez, B. et al., "MATISSE, the VLTI mid-infrared imaging spectro-interferometer," Astron. Astrophys. 659, A192 (2022)

  13. [13]

    Planet Formation Imager (PFI): project update and future directions,

    Monnier, J. D., Kraus, S., Ireland, M. J., "Planet Formation Imager (PFI): project update and future directions," arXiv:2408.03896 (2024)

  14. [14]

    L-band nulling interferometry at the VLTI with Asgard/NOTT,

    Defrère, D. et al., "L-band nulling interferometry at the VLTI with Asgard/NOTT," Proc. SPIE (2024); arXiv:2407.08397

  15. [15]

    Large Interferometer For Exoplanets (LIFE): I,

    Quanz, S. P. et al., "Large Interferometer For Exoplanets (LIFE): I," Astron. Astrophys. 664, A21 (2022). [6] Konrad, B. S. et al., "LIFE: III. Spectral resolution and sensitivity requirements," Astron. Astrophys. 664, A23 (2022)

  16. [16]

    LIFE: XIII. Combining thermal emission and reflected light,

    Alei, E. et al., "LIFE: XIII. Combining thermal emission and reflected light," Astron. Astrophys. 689, A245 (2024). [8] Hansen, J. T., Ireland, M. J., "LIFE: IV. Ideal kernel-nulling array architectures," Astron. Astrophys. 664, A52 (2022)

  17. [17]

    Artemis-enabled Stellar Imager (AeSI): a lunar long-baseline UV/optical imaging interferometer,

    Rau, G. et al., "Artemis-enabled Stellar Imager (AeSI): a lunar long-baseline UV/optical imaging interferometer," Proc. SPIE 13092 (2024); arXiv:2408.04699

  18. [18]

    AeSI NIAC Phase I Final Report,

    Carpenter, K. G. et al., "AeSI NIAC Phase I Final Report," arXiv:2503.02105 (2025). [11] van Belle, G. et al., "Astronomical optical interferometry from the lunar surface," arXiv:2510.24901 (2025). [12] Burns, J. O. et al., "FARSIDE: a low radio frequency interferometric array on the lunar farside," NASA Probe Study (2019)

  19. [19]

    The Dark Ages Explorer (DEX): a filled-aperture ultra-long wavelength radio interferometer on the lunar far side,

    Brinkerink, C. et al., "The Dark Ages Explorer (DEX): a filled-aperture ultra-long wavelength radio interferometer on the lunar far side," arXiv:2504.03418 (2025)

  20. [20]

    FarView: an in-situ manufactured lunar far side radio array concept for 21-cm Dark Ages cosmology,

    Polidan, R. S. et al., "FarView: an in-situ manufactured lunar far side radio array concept for 21-cm Dark Ages cosmology," Adv. Space Res. (2024); arXiv:2404.03840

  21. [21]

    Design, modeling, and characterization of the antenna module for the LuSEE-Night mission,

    S. D. Bale, et al., "Design, modeling, and characterization of the antenna module for the LuSEE-Night mission," in Ground-based and Airborne Telescopes X, Proc. SPIE 13092, 130927A (2024)

  22. [22]

    Sub-femto-g free fall: LISA Pathfinder results,

    Armano, M. et al., "Sub-femto-g free fall: LISA Pathfinder results," Phys. Rev. Lett. 116, 231101 (2016). [17] Abich, K. et al., "In-orbit performance of the GRACE Follow-On Laser Ranging Interferometer," Phys. Rev. Lett. 123, 031101 (2019)

  23. [23]

    Formation flying performances simulator for the shadow position sensors of the ESA PROBA-3 mission,

    Capobianco, G., Focardi, M., Landini, F., et al., "Formation flying performances simulator for the shadow position sensors of the ESA PROBA-3 mission," Proc. SPIE 11852, 118526P (2021)

  24. [24]

    The ASPIICS solar coronagraph aboard the Proba-3 formation flying mission,

    Zhukov, A. N. et al., "The ASPIICS solar coronagraph aboard the Proba-3 formation flying mission," arXiv:2509.00253 (2025)

  25. [25]

    Starlight Acquisition and Reflection toward Interferometry (STARI): A CubeSat Pathfinder,

    J. D. Monnier et al., "Starlight Acquisition and Reflection toward Interferometry (STARI): A CubeSat Pathfinder," arXiv:2408.03925 (2024)

  26. [26]

    The Space Infrared Interferometric Telescope (SPIRIT): high-resolution imaging and spectroscopy in the far-infrared,

    Leisawitz, D. et al., "The Space Infrared Interferometric Telescope (SPIRIT): high-resolution imaging and spectroscopy in the far-infrared," Adv. Space Res. (2007); arXiv:0707.0883

  27. [27]

    The Black Hole Explorer: Photon Ring Science, Detection and Shape Measurement,

    Johnson, M. D. et al., "The Black Hole Explorer: Photon Ring Science, Detection and Shape Measurement," arXiv:2406.09498 (2024)

  28. [28]

    The Black Hole Explorer: instrument system overview,

    Marrone, D. P. et al., "The Black Hole Explorer: instrument system overview," Proc. SPIE 13092 (2024) [24] Ito, T. et al., "SILVIA: Ultra-precision formation flying demonstration for space-based interferometry," Publ. Astron. Soc. Japan 77, 1080 (2025); arXiv:2504.05001

  29. [29]

    A realistic roadmap to formation-flying space interferometry,

    Monnier, J. D. et al., "A realistic roadmap to formation-flying space interferometry," arXiv:1907.09583 (2019). [26] K. C. Gendreau et al., "MAXIM Pathfinder x-ray interferometry mission," Proc. SPIE 4851, 343–352 (2003); [https://doi.org/10.1117/12.461495](https://doi.org/10.1117/12.461495)

  30. [30]

    The Lunar-based Ultraviolet Telescope (LUT) on Chang'e-3,

    Wang, J. et al., "The Lunar-based Ultraviolet Telescope (LUT) on Chang'e-3," Astrophys. Space Sci. 360, 10 (2015) [28] Sanny, A., Labadie, L. et al., "Asgard/NOTT: L-band nulling interferometry at the VLTI – III. The mid-infrared integrated-optics beam combiner," Astron. Astrophys. (2026); arXiv:2511.19790

  31. [31]

    Database of Candidate Targets for the LIFE Mission,

    Menti, F. et al., "Database of Candidate Targets for the LIFE Mission," Res. Notes AAS 8, 267 (2024); arXiv:2410.23892

  32. [32]

    (2025), NASA Exoplanet Exploration Program (ExEP) Science Gap List, JPL Document D-1792073-2, Rev

    Stapelfeldt, K., & Mamajek, E., et al. (2025), NASA Exoplanet Exploration Program (ExEP) Science Gap List, JPL Document D-1792073-2, Rev. H, released January 7, 2025; arXiv:2507.18665

  33. [33]

    Exoplanet explorer: a single spacecraft nulling interferometer,

    Lueftinger, T., et al. (2025), "Exoplanet explorer: a single spacecraft nulling interferometer," Proc. SPIE 13699, International Conference on Space Optics – ICSO 2024, 1369927. DOI: 10.1117/12.3072787

  34. [34]

    A preliminary exploration of the effects of baseline length for the LIFE space mission,

    R. L. Garcia et al., "A preliminary exploration of the effects of baseline length for the LIFE space mission," arXiv:2605.06648 (2026)

  35. [35]

    MoonLITE: a CLPS-delivered NASA Astrophysics Pioneers lunar optical interferometer for sensitive, milliarcsecond observing,

    van Belle, G. T. et al., "MoonLITE: a CLPS-delivered NASA Astrophysics Pioneers lunar optical interferometer for sensitive, milliarcsecond observing," Proc. SPIE 13092 (2024); arXiv:2408.01392

  36. [36]

    SEIRIOS: high spatial resolution spectral imaging for formation-flying small-satellite stellar interferometry,

    Matsuo, T. et al., "SEIRIOS: high spatial resolution spectral imaging for formation-flying small-satellite stellar interferometry," J. Astron. Telesc. Instrum. Syst. 8, 015001 (2022); arXiv:2201.07355

  37. [37]

    Autonomous guidance, navigation, and control of the VISORS formation-flying mission,

    Guffanti, T. et al., "Autonomous guidance, navigation, and control of the VISORS formation-flying mission," arXiv:2309.16698 (2024)

  38. [38]

    Laser Interferometer Lunar Antenna (LILA): advancing U.S. priorities in gravitational-wave and lunar science,

    Jani, K. et al., "Laser Interferometer Lunar Antenna (LILA): advancing U.S. priorities in gravitational-wave and lunar science," arXiv:2508.11631 (2025)

  39. [39]

    The Need for Ultra High Resolution X-ray Imaging,

    Gaier, J.R. (2005). The Effects of Lunar Dust on EVA Systems During the Apollo Missions. NASA/TM-2005-213610, NASA Glenn Research Center https://ntrs.nasa.gov/citations/20050160460 [38] Weaver, K. A. et al., "The Need for Ultra High Resolution X-ray Imaging," arXiv:2601.20823 (2026). [39] Ertel, S., et al. (2025), Review and Prospects of Hot Exozodiacal D...

  40. [40]

    Kilometric baseline space interferometry: comparison of free-flyer and Moon-based versions,

    Ertel et al. 2020 (the HOSTS survey results, AJ 159, 177), DOI 10.3847/1538-3881/ab7817 [41] Bély, P.-Y., Laurance, R., Volonte, S., et al. (1996), "Kilometric baseline space interferometry: comparison of free-flyer and Moon-based versions," ESA SCI(96)7, doi:10.1117/12.255123

  41. [41]

    Darwin: a mission overview,

    A. Karlsson, L. d'Arcio, R. den Hartog, and M. Fridlund, "Darwin: a mission overview," in Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Proc. SPIE 6265, 62651O (2006); doi: 10.1117/12.669791

  42. [42]

    Terrestrial Planet Finder Interferometer technology status and plans,

    P. R. Lawson et al., "Terrestrial Planet Finder Interferometer technology status and plans," Proc. SPIE 6268, 626828 (2006); doi: 10.1117/12.670318

  43. [43]

    The Fourier-Kelvin Stellar Interferometer (FKSI): a review, progress report, and update,

    W. C. Danchi, R. K. Barry, P. R. Lawson, W. A. Traub, and S. Unwin, "The Fourier-Kelvin Stellar Interferometer (FKSI): a review, progress report, and update," Proc. SPIE 7013, Optical and Infrared Interferometry, 70132Q (2008). [doi:10.1117/12.790649]

  44. [44]

    Exoplanet detection yield of a space-based Bracewell interferometer,

    C. Dandumont, D. Defrère, J. Kammerer, O. Absil, S. P. Quanz, and J. Loicq, "Exoplanet detection yield of a space-based Bracewell interferometer," J. Astron. Telesc. Instrum. Syst. 6(3), 035004 (2020). [doi:10.1117/1.JATIS.6.3.035004]

  45. [45]

    Pegase: a space-based nulling interferometer,

    J. M. Le Duigou, M. Ollivier, A. Léger, F. Cassaing, B. Sorrente, B. Fleury, and G. Rousset, "Pegase: a space-based nulling interferometer," Proc. SPIE 6265, Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, 62651N (2006). [doi:10.1117/12.671091]

  46. [46]

    The Space Interferometer for Cosmic Evolution (SPICE) Far-IR Probe,

    Leisawitz, D., Aalto, S., Bergner, J., Bonato, M., Bracken, C., Eales, S., and Farrah, D., "The Space Interferometer for Cosmic Evolution (SPICE) Far-IR Probe," Bull. Am. Astron. Soc. 55(2), 160.04 (2023)

  47. [47]

    Weather on the Moon,

    NASA, "Weather on the Moon," NASA Science Solar System Exploration (2024). [https://science.nasa.gov/moon/weather-on-the-moon/](https://science.nasa.gov/moon/weather-on-the-moon/) (Accessed 2026)

  48. [48]

    D., Felikson, D., Sabaka, T

    Loomis, B. D., Felikson, D., Sabaka, T. J., & Medley, B. (2021). High-spatial-resolution mass rates from GRACE and GRACE-FO: Global and ice sheet analyses. Journal of Geophysical Research: Solid Earth, 126(12), e2021JB023024

  49. [49]

    The SPace-based InterFerometer Feasibility (SPIFF) Project: Enabling Future High-Resolution Astronomy Across the EM Spectrum,

    https://science.nasa.gov/astrophysics/programs/physics-of-the-cosmos/studies/astra-initiative/ [51] B. V. Ricketti et al., "The SPace-based InterFerometer Feasibility (SPIFF) Project: Enabling Future High-Resolution Astronomy Across the EM Spectrum," UK Space Agency Frontiers 2035 Community White Paper , arXiv:2512.10009 (2025)

  50. [50]

    Protection of Astronomy and Science on the Moon," Conference Room Paper, UN COPUOS Scientific and Technical Subcommittee, 61st Sess., Doc. A/AC.105/C.1/2024/CRP.14, UNOOSA (2024), https://www.unoosa.org/res/oosadoc/data/documents/2024/aac_105c_12024crp/aac_105c_12024crp_14_0_html/AC105_C1_2024_CRP14E.pdf [53] Krolikowski A, Elvis M. Potential and perils: ...

  51. [51]

    Reinforcement Learning for Data-Driven Workflows in Radio Interferometry. I. Principal Demonstration in Calibration,

    Kirk, B. M., Rau, U., and Ramyaa, R., “Reinforcement Learning for Data-Driven Workflows in Radio Interferometry. I. Principal Demonstration in Calibration,” arXiv:2410.17135 (2024)

  52. [52]

    VIPCALs: A fully-automated calibration pipeline for VLBI data,

    Álvarez-Ortega, D., Casadio, C., Pötzl, F. M., Kumar, A., and Janssen, M., “VIPCALs: A fully-automated calibration pipeline for VLBI data,” arXiv:2508.13282 (2025)

  53. [53]

    A robust RFI identification for radio interferometry based on a convolutional neural network,

    Sun, H. et al., “A robust RFI identification for radio interferometry based on a convolutional neural network,” arXiv:2203.00298 (2022)

  54. [54]

    Exploring Exoplanets with Interferometry,

    Quanz, S. P., Mennesson, B., Beichman, C., et al., "Exploring Exoplanets with Interferometry," W. M. Keck Institute for Space Studies (KISS) report (2026)

  55. [55]

    Overview of the SIM PlanetQuest Light (SIM-Lite) mission concept,

    Goullioud, R., Catanzarite, J. H., Dekens, F. G., Shao, M., & Marr, J. C. IV, "Overview of the SIM PlanetQuest Light (SIM-Lite) mission concept," Proc. SPIE 7013, 70134T (2008); arXiv:0807.1668

  56. [56]

    SIM-PlanetQuest technology: A retrospective view,

    Marr, J. C. IV, et al., "SIM-PlanetQuest technology: A retrospective view," Acta Astronautica (2009). [60] Alibay, F., Kasper, J. C., Lazio, T. J. W., and Neilsen, T., "Sun radio interferometer space experiment (SunRISE): Tracking particle acceleration and transport in the inner heliosphere," in 2017 IEEE Aerospace Conference, 1-15 (2017). doi:10.1109/aer...

  57. [57]

    Optical Intensity Interferometry with Atmospheric Cerenkov Telescope Arrays,

    Le Bohec, S. and Holder, J., "Optical Intensity Interferometry with Atmospheric Cerenkov Telescope Arrays," Astrophys. J. 649(1), 399-405 (2006). [See also: Dravins, D. et al., "Optical intensity interferometry with the Cherenkov Telescope Array," Astropart. Phys. 43, 331-347 (2013)]

  58. [58]

    Optical intensity interferometry observations using the MAGIC imaging atmospheric Cherenkov telescopes,

    Acciari, V. A., Bernardos, M. I., Colombo, E., et al., "Optical intensity interferometry observations using the MAGIC imaging atmospheric Cherenkov telescopes," Mon. Not. R. Astron. Soc. 491(2), 1540-1547 (2020). doi:10.1093/mnras/stz3171

  59. [59]

    The angular diameters of 32 stars,

    Hanbury Brown, R., Davis, J., and Allen, L. R., "The angular diameters of 32 stars," Mon. Not. R. Astron. Soc. 167(1), 121-136 (1974). doi:10.1113/j.1365-2966.1974.tb01438.x

  60. [60]

    Correlation between Photons in two Coherent Beams of Light,

    Hanbury Brown, R. and Twiss, R. Q., "Correlation between Photons in two Coherent Beams of Light," Nature 177(4497), 27–29 (1956). doi:10.1038/177027a0

  61. [61]

    Imaging the surface of Altair,

    Monnier, J. D., Zhao, M., Pedretti, E., Thureau, N., Ireland, M., Muirhead, P., Berger, J.-P., Millan-Gabet, R., Van Belle, G., ten Brummelaar, T., McAlister, H., Ridgway, S., Turner, N., Sturmann, L., Sturmann, J., Berger, D., "Imaging the surface of Altair," Science 317(5836), 342–345 (2007); doi:10.1126/science.1143205

  62. [62]

    No Sun-like dynamo on the active star ζ Andromedae from starspot asymmetry,

    Roettenbacher, R. M., Monnier, J. D., Korhonen, H., et al., "No Sun-like dynamo on the active star ζ Andromedae from starspot asymmetry," Nature 533, 217–220 (2016); doi:10.1038/nature17444

  63. [63]

    First direct detection of an exoplanet by optical interferometry: Astrometry and K-band spectroscopy of HR 8799 e,

    GRAVITY Collaboration: Lacour, S., Nowak, M., Wang, J., et al., "First direct detection of an exoplanet by optical interferometry: Astrometry and K-band spectroscopy of HR 8799 e," Astron. Astrophys. 623, L11 (2019); doi:10.1051/0004-6361/201935253

  64. [64]

    Cepheid distances from infrared long-baseline interferometry. II. Calibration of the period–radius and period–luminosity relations,

    Kervella, P., Bersier, D., Mourard, D., Nardetto, N., Fouqué, P., Coudé du Foresto, V., "Cepheid distances from infrared long-baseline interferometry. II. Calibration of the period–radius and period–luminosity relations," Astron. Astrophys. 423, 327–333 (2004)

  65. [65]

    The design of a drag-free CubeSat and the housing for its gravitational reference sensor,

    Zanoni, C., Alfauwaz, A., Aljadaan, A., et al. "The design of a drag-free CubeSat and the housing for its gravitational reference sensor," Proc. 2nd IAA Conf. on University Satellite Missions and CubeSat Workshop (2016); arXiv:1605.05496

  66. [66]

    A simplified gravitational reference sensor for satellite geodesy,

    Dávila Álvarez, A., Knudtson, A., Patel, U., Gleason, J., Hollis, H., Sanjuan, J., Doughty, N., McDaniel, G., Lee, J., Leitch, J., Bennett, S., Bevilacqua, R., Mueller, G., Spero, R., Ware, B., Wass, P., Wiese, D., Ziemer, J., and Conklin, J. W., "A simplified gravitational reference sensor for satellite geodesy," J. Geod. 96, 49 (2022). doi:10.1007/s0019...

  67. [67]

    Gravitational Reference Sensor Technology Development Roadmap for the Mass Change Mission,

    Conklin, J. W., "Gravitational Reference Sensor Technology Development Roadmap for the Mass Change Mission," NASA Science Technology Report, NASA ESTO (2020) https://science.nasa.gov/wp-content/uploads/2023/05/GRS_Technology_Summary_and_Roadmap_TAGGED.pdf [72] Birbacher, T., Hansen, J. T., Dannert, F. A., Garreau, G., Glauser, A. M., Meierhofer, R., Jimén...

  68. [68]

    First light for GRAVITY Wide. Large separation fringe tracking for the Very Large Telescope Interferometer,

    GRAVITY+ Collaboration, et al., "First light for GRAVITY Wide. Large separation fringe tracking for the Very Large Telescope Interferometer," Astron. Astrophys. 665, A75 (2022)