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arxiv: 1907.04443 · v1 · pith:H2UNHMHPnew · submitted 2019-07-09 · 🌌 astro-ph.IM

SETI in the Spatio-Temporal Survey Domain

James. R. A. Davenport This is my paper

Pith reviewed 2026-05-24 23:45 UTC · model grok-4.3

classification 🌌 astro-ph.IM
keywords SETItechnosignaturestime domain surveysoptical surveyscosmic haystacksynoptic surveysexoplanet transits
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The pith

Current optical time domain surveys can probe 10-100 times more cosmic haystack volume for technosignatures than many radio SETI efforts.

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

The paper claims that traditional SETI relies on dedicated pointings at single targets, while synoptic optical surveys already collect repeated measurements across wide sky areas. These data enable a spatio-temporal search that covers far more combinations of position, time, and signal properties without new telescope time. A reader would care because the approach uses data already being taken for other science, at much lower added cost, and the author shows the volume gain is substantial for surveys such as ZTF and Evryscope. The work also notes that new algorithms will be required to exploit signals that appear across both space and time.

Core claim

The central claim is that current optical time domain surveys such as ZTF and the Evryscope can probe 10-100 times more of the Cosmic Haystack parameter space volume than many radio SETI investigations, because they supply spatially resolved, time-series photometry on many stars simultaneously; small-aperture high-cadence surveys can reach comparable completeness to deeper surveys such as LSST, and all such work can be done at a fraction of the cost of dedicated SETI observations since the data are already gathered.

What carries the argument

The Cosmic Haystack parameter space volume, which measures the searchable combinations of sky position, time, frequency, and sensitivity; the spatio-temporal SETI method uses existing survey light curves to search this volume without new observations.

If this is right

  • SETI searches can be performed with data already collected by ongoing surveys at negligible extra cost.
  • Small-aperture surveys such as Evryscope can match the haystack completeness of deeper surveys like LSST.
  • New algorithms are required that search for signals appearing across both spatial and temporal domains.
  • Transiting exoplanets can serve as a natural distributed beacon geometry for such searches.

Where Pith is reading between the lines

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

  • SETI funding priorities could shift toward analysis of archival survey data rather than new dedicated instruments.
  • Cross-survey combinations could multiply the searchable volume further if data archives are aligned.
  • The same spatio-temporal logic may apply to infrared or other time-domain datasets once they reach comparable cadence and sky coverage.

Load-bearing premise

Technosignatures are likely to appear as detectable signals within the combined spatial and temporal coverage of existing optical survey data.

What would settle it

A side-by-side calculation of the haystack volume actually covered by ZTF or Evryscope versus a representative radio SETI survey that yields a factor less than 10 improvement.

Figures

Figures reproduced from arXiv: 1907.04443 by James. R. A. Davenport.

Figure 1
Figure 1. Figure 1: Comparison of the 8-D “Cosmic Haystack” SETI search volume fraction, defined by Wright et al. (2018), com￾puted using five optical surveys with varying designs. The Haystack fraction covered by these optical surveys is 1-2 dex larger than typical SETI programs conducted in the radio. Evryscope Law et al. (2015) is the best survey considered here for SETI work, narrowly beating LSST due to its wide field of… view at source ↗
Figure 2
Figure 2. Figure 2: two point correlation function of transiting exo￾planets versus all stars in the kepler field. No obvious signs of engineering of the exoplanet population as a whole. ex￾oplanets are actually slightly less correlated on small size scales than stars in general, which may be an artifact of de￾tected planets being around brighter stars in the sample (i.e. having lower total density). While overly simple, this… view at source ↗
Figure 3
Figure 3. Figure 3: Fractional range of orbital periods versus the mean angular separation for KNN clusters in (RA, Dec) space of transiting exoplanet systems in Kepler. This sample only includes systems with only a single known transiting ex￾oplanet. These KNN clusters have typical spatial separations of ∼0.1 deg. For K=3, three unique clusters have a spread in their orbital periods below 6% (red points). However this is not… view at source ↗
read the original abstract

Traditional searches for extraterrestrial intelligence (SETI) or "technosignatures" focus on dedicated observations of single stars or regions in the sky to detect excess or transient emission from intelligent sources. The newest generation of synoptic time domain surveys enable an entirely new approach: spatio-temporal SETI, where technosignatures may be discovered from spatially resolved sources or multiple stars over time. Current optical time domain surveys such as ZTF and the Evryscope can probe 10-100 times more of the "Cosmic Haystack" parameter space volume than many radio SETI investigations. Small-aperture, high cadence surveys like Evryscope can be comparable in their Haystack volume completeness to deeper surveys including LSST. Investigations with these surveys can also be conducted at a fraction of the cost of dedicated SETI surveys, since they make use of data already being gathered. However, SETI methodology has not widely utilized such surveys, and the field is in need of new search algorithms that can account for signals in both the spatial and temporal domains. Here I describe the broad potential for modern wide-field time domain optical surveys to revolutionize our search for technosignatures, and illustrate some example SETI approaches using transiting exoplanets to form a distributed beacon.

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 manuscript proposes a spatio-temporal approach to SETI that leverages existing wide-field optical time-domain survey data (e.g., ZTF, Evryscope) rather than dedicated single-target observations. It asserts that these surveys can access 10-100 times more Cosmic Haystack volume than many radio SETI programs, notes that small-aperture high-cadence surveys can match deeper ones like LSST in completeness, and illustrates example search strategies that treat transiting exoplanets as potential distributed beacons while calling for new algorithms that jointly exploit spatial and temporal domains.

Significance. If the volume-comparison claim can be placed on a reproducible quantitative footing, the work would usefully highlight the low marginal cost of mining archival synoptic data for technosignatures and could motivate the development of spatio-temporal search pipelines; the suggestion to repurpose transit surveys as beacon searches is a concrete, falsifiable direction.

major comments (2)
  1. [Abstract] Abstract: the claim that ZTF and Evryscope “can probe 10-100 times more of the Cosmic Haystack parameter space volume than many radio SETI investigations” is presented without an explicit metric, integration limits, sensitivity thresholds, or comparison table that augments the classic 9-D Haystack with spatial-resolution and temporal-sampling dimensions. Because this factor is the central quantitative assertion, its absence prevents verification or stress-testing.
  2. [§1] §1 (or wherever the Haystack comparison is developed): no derivation, error propagation, or parameter-space integration is supplied to support the 10-100× multiplier; the text remains a forward-looking proposal rather than a calculation whose result can be reproduced from stated assumptions.
minor comments (2)
  1. [Throughout] The manuscript would benefit from a short table or appendix that lists the adopted Haystack dimensions, their ranges, and the weighting used for the volume ratio once the metric is defined.
  2. [Abstract / §2] Notation for “spatio-temporal” versus classic Haystack axes should be introduced consistently when the quantitative comparison is added.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful review and for identifying the need for greater quantitative rigor around our central claim. We address each major comment below and will incorporate the requested details in a revised manuscript.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the claim that ZTF and Evryscope “can probe 10-100 times more of the Cosmic Haystack parameter space volume than many radio SETI investigations” is presented without an explicit metric, integration limits, sensitivity thresholds, or comparison table that augments the classic 9-D Haystack with spatial-resolution and temporal-sampling dimensions. Because this factor is the central quantitative assertion, its absence prevents verification or stress-testing.

    Authors: We agree that the abstract claim requires an explicit supporting metric to be verifiable. The 10–100× factor is an order-of-magnitude estimate arising from the simultaneous monitoring of ~10^5–10^6 stars (versus typical targeted radio SETI samples of tens to hundreds) together with the added dimensions of spatial resolution and high-cadence temporal sampling. In the revision we will add a short paragraph and comparison table to the abstract (or a footnote) that states the integration limits, sensitivity thresholds, and the two new Haystack dimensions used to obtain the multiplier. revision: yes

  2. Referee: [§1] §1 (or wherever the Haystack comparison is developed): no derivation, error propagation, or parameter-space integration is supplied to support the 10-100× multiplier; the text remains a forward-looking proposal rather than a calculation whose result can be reproduced from stated assumptions.

    Authors: We acknowledge that the manuscript currently presents the multiplier without a reproducible derivation. Although the work is framed as a conceptual proposal, the quantitative assertion does need grounding. We will expand the relevant section (likely a new subsection in §1 or a short “Methods” paragraph) to include the explicit parameter-space volume integral, the assumed limits on each dimension, and a brief discussion of uncertainties. This will allow readers to reproduce or stress-test the factor from the stated assumptions. revision: yes

Circularity Check

0 steps flagged

Proposal paper with no derivations or load-bearing equations

full rationale

The manuscript is a forward-looking proposal paper that states comparative claims about Cosmic Haystack volume coverage (e.g., the 10-100x factor for ZTF/Evryscope) without presenting any equations, parameter fits, derivations, or self-citations that reduce to the target result by construction. No self-definitional steps, fitted inputs renamed as predictions, or ansatz smuggling occur. The text is self-contained as a conceptual discussion and does not rely on internal reductions for its central assertions.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review contains no explicit free parameters, axioms, or invented entities; the central claim rests on the unstated premise that survey data volumes translate directly to technosignature search volume.

pith-pipeline@v0.9.0 · 5749 in / 984 out tokens · 15956 ms · 2026-05-24T23:45:03.239616+00:00 · methodology

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. A Framework for Applying the Loeb-Turner $\alpha$-Slope Test to Archival Photometry of Trans-Neptunian Objects

    astro-ph.EP 2026-05 unverdicted novelty 5.0

    A formalized eligibility pipeline applied to 8,557 TNO photometry bins finds 109 anomalous slopes likely caused by per-instrument calibration offsets, with all 24 self-luminous-like cases coming from Pan-STARRS.

Reference graph

Works this paper leans on

41 extracted references · 41 canonical work pages · cited by 1 Pith paper · 6 internal anchors

  1. [1]

    2005, in SF2A-2005: Semaine de l’Astrophysique Francaise, ed

    Arnold, L. 2005, in SF2A-2005: Semaine de l’Astrophysique Francaise, ed. F. Casoli, T. Contini, J. M. Hameury, & L. Pagani, 207 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33

    work page 2005

  2. [2]

    2014, in The Third Hot-wiring the Transient Universe Workshop, ed

    Bellm, E. 2014, in The Third Hot-wiring the Transient Universe Workshop, ed. P. R. Wozniak, M. J. Graham, A. A. Mahabal, & R. Seaman, 27–33

    work page 2014

  3. [3]

    The Promise of Data Science for the Technosignatures Field

    Berea, A., Croft, S., & Angerhausen, D. 2019, arXiv e-prints, arXiv:1903.08381

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  4. [4]

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

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

    work page 2010

  5. [5]

    Planet Hunters X. KIC 8462852 - Where's the Flux?

    Boyajian, T. S., LaCourse, D. M., Rappaport, S. A., et al. 2015, ArXiv e-prints, arXiv:1509.03622

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  6. [6]

    Council, N. R. 2010, New Worlds, New Horizons in Astronomy and Astrophysics (Washington, DC: The National Academies Press), doi:10.17226/12951

    work page doi:10.17226/12951 2010

  7. [7]

    2000, in Astronomical Society of the Pacific Conference Series, Vol

    Djorgovski, S. 2000, in Astronomical Society of the Pacific Conference Series, Vol. 213, Bioastronomy 99, ed. G. Lemarchand & K. Meech, 519

    work page 2000

  8. [8]

    2013, Sky Surveys, ed

    Donalek, C. 2013, Sky Surveys, ed. T. D. Oswalt & H. E. Bond, 223

    work page 2013

  9. [9]

    J., Djorgovski, S

    Drake, A. J., Djorgovski, S. G., Mahabal, A., et al. 2009, ApJ, 696, 870

    work page 2009

  10. [10]

    2019, Research Notes of the AAS, 3, 32

    Forgan, D. 2019, Research Notes of the AAS, 3, 32

    work page 2019

  11. [11]

    Forgan, D. H. 2017, ArXiv e-prints, arXiv:1707.03730

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  12. [12]

    Heller, R., & Pudritz, R. E. 2016, Astrobiology, 16, 259

    work page 2016

  13. [13]

    W., Horowitz, P., Wilkinson, D

    Howard, A. W., Horowitz, P., Wilkinson, D. T., et al. 2004, ApJ, 613, 1270

    work page 2004

  14. [14]

    Hunter, J. D. 2007, Computing In Science & Engineering, 9, 90

    work page 2007

  15. [15]

    Isaacson, H., Siemion, A. P. V., Marcy, G. W., et al. 2019, PASP, 131, 014201 —. 2017, PASP, 129, 054501 Ivezi´ c,ˇZ., Connolly, A., Vanderplas, J., & Gray, A. 2014,

    work page 2019

  16. [16]

    LSST: from Science Drivers to Reference Design and Anticipated Data Products

    Statistics, Data Mining and Machine Learning in Astronomy (Princeton University Press) Ivezi´ c,ˇZ., Tyson, J. A., Acosta, E., et al. 2008, ArXiv e-prints, # 0805.2366, arXiv:0805.2366

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  17. [17]

    2001–, SciPy: Open source scientific tools for Python, , , [Online; accessed ¡today¿]

    Jones, E., Oliphant, T., Peterson, P., et al. 2001–, SciPy: Open source scientific tools for Python, , , [Online; accessed ¡today¿]

    work page 2001

  18. [18]

    2012, LSD: Large Survey Database framework, , , ascl:1209.003

    Juric, M. 2012, LSD: Large Survey Database framework, , , ascl:1209.003

    work page 2012

  19. [19]

    M., & Teachey, A

    Kipping, D. M., & Teachey, A. 2016, MNRAS, 459, 1233

    work page 2016

  20. [20]

    Lacki, B. C. 2019, arXiv e-prints, arXiv:1903.05839

    work page arXiv 2019

  21. [21]

    D., & Szalay, A

    Landy, S. D., & Szalay, A. S. 1993, ApJ, 412, 64

    work page 1993

  22. [22]

    M., Fors, O., Ratzloff, J., et al

    Law, N. M., Fors, O., Ratzloff, J., et al. 2015, PASP, 127, 234

    work page 2015

  23. [23]

    Lemarchand, G. A. 1994, Ap&SS, 214, 209

    work page 1994

  24. [24]

    Makovetskii, P. V. 1977, Soviet Ast., 21, 251

    work page 1977

  25. [25]

    2017, Research Notes of the American Astronomical Society, 1, 21

    Mamajek, E. 2017, Research Notes of the American Astronomical Society, 1, 21

    work page 2017

  26. [26]

    2010, in Proceedings of the 9th Python in Science Conference, ed

    McKinney, W. 2010, in Proceedings of the 9th Python in Science Conference, ed. S. van der Walt & J. Millman, 51 – 56

    work page 2010

  27. [27]

    Oliphant, T. E. 2007, Computing in Science Engineering, 9, 10

    work page 2007

  28. [28]

    T., Bellm, E

    Patterson, M. T., Bellm, E. C., Rusholme, B., et al. 2019, PASP, 131, 018001 P´ erez, F., & Granger, B. E. 2007, Computing in Science and Engineering, 9, 21

    work page 2019

  29. [29]

    The Breakthrough Listen Search for Intelligent Life: Wide-bandwidth Digital Instrumentation for the CSIRO Parkes 64-m Telescope

    Price, D. C., MacMahon, D. H. E., Lebofsky, M., et al. 2018, ArXiv e-prints, arXiv:1804.04571

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  30. [30]

    R., Winn, J

    Ricker, G. R., Winn, J. N., Vanderspek, R., et al. 2015, Journal of Astronomical Telescopes, Instruments, and Systems, 1, 014003

    work page 2015

  31. [31]

    E., Hsieh, H., Bannister, M

    Schwamb, M. E., Hsieh, H., Bannister, M. T., et al. 2019, Research Notes of the AAS, 3, 51

    work page 2019

  32. [32]

    2004, in IAU Symposium, Vol

    Shostak, S. 2004, in IAU Symposium, Vol. 213, Bioastronomy 2002: Life Among the Stars, ed. R. Norris & F. Stootman, 409

    work page 2004

  33. [33]

    2001, ARA&A, 39, 511

    Tarter, J. 2001, ARA&A, 39, 511

    work page 2001

  34. [34]

    J., Tremblay, C

    Tingay, S. J., Tremblay, C. D., & Croft, S. 2018, ApJ, 856, 31 8 Davenport

    work page 2018

  35. [35]

    2016, AJ, 152, 76

    Villarroel, B., Imaz, I., & Bergstedt, J. 2016, AJ, 152, 76

    work page 2016

  36. [36]

    J., & Dolence, J

    Wang, Y., Brunner, R. J., & Dolence, J. C. 2013, MNRAS, 432, 1961

    work page 2013

  37. [37]

    P., Drew, J., Siemion, A., et al

    Worden, S. P., Drew, J., Siemion, A., et al. 2017, Acta Astronautica, 139, 98

    work page 2017

  38. [38]

    Wright, J. T. 2017, Exoplanets and SETI, 186

    work page 2017

  39. [39]

    T., Cartier, K

    Wright, J. T., Cartier, K. M. S., Zhao, M., Jontof-Hutter, D., & Ford, E. B. 2016, ApJ, 816, 17

    work page 2016

  40. [40]

    T., Kanodia, S., & Lubar, E

    Wright, J. T., Kanodia, S., & Lubar, E. 2018, AJ, 156, 260

    work page 2018

  41. [41]

    AXS: A framework for fast astronomical data processing based on Apache Spark

    Wright, J. T., & Oman-Reagan, M. P. 2018, International Journal of Astrobiology, 17, 177 Zeˇ cevi´ c, P., Slater, C. T., Juri´ c, M., et al. 2019, arXiv e-prints, arXiv:1905.09034

    work page internal anchor Pith review Pith/arXiv arXiv 2018