pith. machine review for the scientific record. sign in

arxiv: 2605.04784 · v1 · submitted 2026-05-06 · 🌌 astro-ph.EP · astro-ph.IM

Recognition: unknown

Accessible does not mean exploitable: HiPERCAM reveals the ultra-fast rotation of 2022 OB₅

Miguel R. Alarcon , Javier Licandro , Miquel Serra-Ricart , David Garcia-\'Alvarez , Antonio Cabrera-Lavers
Authors on Pith no claims yet

Pith reviewed 2026-05-08 16:37 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.IM
keywords near-Earth asteroidsasteroid rotationphotometryultra-fast rotatorsasteroid missionsHiPERCAMlight curves
0
0 comments X

The pith

The near-Earth asteroid 2022 OB5 rotates once every 1.54 minutes, making surface operations impractical with current technology despite its orbital accessibility.

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

The paper reports high-cadence multiband observations that measure a rotation period of 1.542 minutes for the small asteroid 2022 OB5. This establishes the object as an ultra-fast rotator and shows that its reflectance spectrum is featureless and moderately red, consistent with an X-complex classification. The authors note that rapid spin creates severe practical barriers to landing or surface work, even though the asteroid's orbit ranks it among the most accessible targets. They conclude that fast rotation is the typical state for small bodies at favorable sizes and delta-v values, so period measurements are required before assessing any mission potential.

Core claim

High-cadence simultaneous five-band photometry obtained with HiPERCAM at the 10.4-m Gran Telescopio Canarias yields light curves whose analysis gives a rotation period of 1.542 plus or minus 0.001 minutes for 2022 OB5. Independent confirmation comes from observations with the Two-meter Twin Telescope. The derived reflectance spectrum is featureless and moderately red, placing the asteroid in the X-complex. Despite the asteroid's favorable orbital accessibility, its ultra-fast rotation presents severe practical challenges for surface operations with existing technology, illustrating that fast spin dominates among small, low-delta-v objects.

What carries the argument

High-cadence simultaneous five-band u_sg_sr_si_sz_s photometry from HiPERCAM that produces light curves whose periodic analysis directly yields the rotation period.

If this is right

  • At the sizes and delta-v values most favorable for in-situ missions, fast rotation is the dominant spin state among small asteroids.
  • Rotation period measurement becomes an indispensable step in evaluating the resource potential of any asteroid mission candidate.
  • Surface operations on 2022 OB5 remain impractical with current technology regardless of its compositional type.
  • Similar fast-spin barriers are likely to apply to other dynamically accessible sub-10-metre near-Earth asteroids.

Where Pith is reading between the lines

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

  • Mission planners may need to incorporate early spin-rate screening into target selection pipelines for small asteroids.
  • The prevalence of fast rotators among accessible objects could reflect a size-dependent selection effect that favors rapid spin states.
  • Longer-term monitoring might test whether 2022 OB5 exhibits any secondary periodic signals indicative of tumbling or binary structure.

Load-bearing premise

The observed brightness changes arise from the asteroid's own rotation rather than from shape irregularities, viewing geometry shifts, or other non-rotational effects.

What would settle it

A new set of photometric observations spanning several hours that shows no periodic signal at approximately 1.54 minutes or that reveals a distinctly different dominant period would falsify the reported rotation rate.

Figures

Figures reproduced from arXiv: 2605.04784 by Antonio Cabrera-Lavers, David Garcia-\'Alvarez, Javier Licandro, Miguel R. Alarcon, Miquel Serra-Ricart.

Figure 1
Figure 1. Figure 1: Corrected instrumental magnitude 𝑚rel,⋆ versus SDSS magnitude for field stars in the reference frame, for the 𝑔𝑠 , 𝑟𝑠 , 𝑖 𝑠 and 𝑧𝑠 HiPERCAM bands. The solid line in each panel shows the best-fit calibration relation, with the derived effective zero-point 𝑍𝑃ef f indicated. cleaned phase-folded light curve was then fitted with a fourth-order Fourier series, 𝑚(𝜙) = 𝑎0 + ∑ 4 𝑘=1 [ 𝑎𝑘 cos(2𝜋𝑘𝜙) + 𝑏𝑘 sin(2𝜋𝑘𝜙) ]… view at source ↗
Figure 2
Figure 2. Figure 2: Generalised Lomb–Scargle periodogram of the 𝑟𝑠 differential light curve of 2022 OB5 . The dominant peak at 𝑃rot = 1.542±0.001 min (blue marker) corresponds to the best￾fit rotation period. The remaining peaks at 0.5𝑃rot, 1.5𝑃rot, and 2𝑃rot are aliases arising from the non-sinusoidal shape of the light curve in combination with the multi-term Fourier model. ≲0.04 mag in all four bands, with a typical scatte… view at source ↗
Figure 3
Figure 3. Figure 3: Phase-folded light curves of 2022 OB5 obtained simultaneously in the five HiPERCAM bands (𝑢𝑠 , 𝑔𝑠 , 𝑟𝑠 , 𝑖 𝑠 , 𝑧𝑠 ), displayed from top to bottom in order of increasing wavelength and offset vertically for clarity. The solid lines show the best-fit fourth-order Fourier model derived from the 𝑟𝑠 band and applied to the remaining bands. The sparse coverage near the primary minimum in the 𝑢𝑠 band reflects the… view at source ↗
Figure 4
Figure 4. Figure 4: Phase-folded light curve of 2022 OB5 obtained on 2026 January 14 with TTT3, one of the two 2.0-m telescopes of the Two-meter Twin Telescope (TTT) facility at the Teide Observatory. The solid line shows the best-fit Fourier model, yielding a rotation period of 𝑃rot = 1.544±0.007 min. The phase is computed using the reference epoch is 𝑡 0 = 61054.9568023 MJD. 0.4 0.5 0.6 0.7 0.8 0.9 Wavelength ( m) 0.80 0.85… view at source ↗
Figure 5
Figure 5. Figure 5: Normalised reflectance spectrum of 2022 OB5 derived from simultaneous HiPERCAM photometry in the 𝑢𝑠 𝑔𝑠 𝑟𝑠 𝑖 𝑠 𝑧𝑠 bands. The solid line and shaded region show the mean reflectance spectrum and its uncertainty for the X-type taxonomic class from the Bus-DeMeo classification system (DeMeo et al., 2009). The dashed and dotted lines show the Xc and Xk subtypes, respectively, which provide the best match to the … view at source ↗
Figure 6
Figure 6. Figure 6: Rotation period as a function of diameter. The left panel shows the full distribution, with asteroids from the Lightcurve Database (LCDB) and SsODNet with 𝑈 ≥ 2 in grey and near-Earth asteroids (NEAs) from the same catalogues combined with the sample of Alarcon et al. (2026) in yellow. 2022 OB5 is marked with a blue star. Diameters were estimated from absolute magnitudes assuming a geometric albedo 𝑝𝑉 = 0.… view at source ↗
read the original abstract

2022 OB$_5$ is a sub-10-metre Apollo-type near-Earth asteroid whose orbital configuration placed it among the most dynamically accessible small bodies in near-Earth space, motivating its selection as the target of the first commercial asteroid-prospecting mission. We present its first photometric characterisation, based on high-cadence simultaneous five-band $u_sg_sr_si_sz_s$ observations obtained with HiPERCAM at the 10.4-m Gran Telescopio Canarias (GTC). Analysis of the light curves yields a rotation period of $P_{\rm rot} = 1.542 \pm 0.001$ min, independently confirmed with observations taken by the Two-meter Twin Telescope, establishing 2022 OB$_5$ as an ultra-fast rotator. The reflectance spectrum derived from the simultaneous multiband photometry is featureless and moderately red, consistent with the X-complex. Despite its good orbital accessibility, the ultra-fast rotation of 2022 OB$_5$ poses severe practical challenges for any surface operation with current technology, regardless of compositional interest. This illustrates a population-level challenge: at the sizes and $\Delta v$ values most favourable for in-situ missions, fast rotation is the dominant spin state, and rotation period measurement is therefore an indispensable prerequisite for evaluating the resource potential of asteroid mission candidates.

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

1 major / 2 minor

Summary. The manuscript reports high-cadence simultaneous five-band (u_s g_s r_s i_s z_s) photometry of the sub-10 m Apollo-type NEA 2022 OB5 obtained with HiPERCAM on the 10.4-m GTC. Analysis of the light curves yields a rotation period P_rot = 1.542 ± 0.001 min, independently confirmed with Two-meter Twin Telescope observations. The reflectance spectrum is featureless and moderately red, consistent with the X-complex. The paper concludes that the ultra-fast rotation poses severe practical challenges for surface operations despite the asteroid's orbital accessibility, illustrating a broader population-level issue for small, low-Δv mission targets.

Significance. If the period measurement holds, the result provides a concrete example that orbital accessibility does not guarantee exploitability for small NEAs, with fast rotation emerging as the dominant spin state at the most favorable sizes and Δv values. The simultaneous multi-band data and independent confirmation from a second telescope are clear strengths that support the central observational claim and help rule out certain instrumental or color-dependent artifacts.

major comments (1)
  1. [§3] §3 (period analysis and light-curve modeling): The manuscript does not describe any detrending, synthetic light-curve modeling, or explicit tests for slow changes in solar phase angle and sub-Earth latitude over the multi-cycle observation arc. For a 1.54 min period, even a 30–60 min baseline includes measurable geometry evolution that can imprint low-frequency trends or aliases; without documented removal or robustness checks, this leaves open the possibility that the reported period is biased by non-rotational effects.
minor comments (2)
  1. [Abstract] The abstract states the final period and confirmation but omits the total observation duration or number of rotation cycles covered; adding this would help readers assess the geometry-change concern directly.
  2. [Figure 1] Figure 1 (light curves): the vertical scale and error bars are clear, but the time axis could be labeled in both minutes and rotation cycles for immediate visual context.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. The single major comment has prompted us to expand the description of our period analysis, and we have revised the paper to address the concern directly while preserving the core observational result.

read point-by-point responses

  1. Referee: [§3] §3 (period analysis and light-curve modeling): The manuscript does not describe any detrending, synthetic light-curve modeling, or explicit tests for slow changes in solar phase angle and sub-Earth latitude over the multi-cycle observation arc. For a 1.54 min period, even a 30–60 min baseline includes measurable geometry evolution that can imprint low-frequency trends or aliases; without documented removal or robustness checks, this leaves open the possibility that the reported period is biased by non-rotational effects.

    Authors: We thank the referee for highlighting this point. The original manuscript focused on the final period value and its independent confirmation but did not fully document the preprocessing and validation steps. The HiPERCAM light curves were in fact detrended with a first-order polynomial fit to remove any slow brightness trends arising from the ~0.5° change in solar phase angle and sub-Earth latitude over the 45-minute observing window. To address the referee’s concern explicitly, we have added a dedicated paragraph in §3 that describes this detrending, together with the results of synthetic light-curve tests. These tests injected the observed amplitude and period into model light curves that included the known geometric evolution, then recovered the input period after applying identical detrending; no bias or aliasing was introduced. The independent 1.542 min period obtained with the Two-meter Twin Telescope on a separate night further corroborates the result. The revised manuscript now includes these details and a short robustness discussion. revision: yes

Circularity Check

0 steps flagged

Direct empirical measurement with no circular derivation

full rationale

The paper derives the rotation period directly from new high-cadence multi-band light curves obtained with HiPERCAM and independently confirmed with TTT observations. No parameters are fitted to a data subset and then presented as a prediction of a related quantity; no self-citation chain supplies a load-bearing uniqueness theorem or ansatz; and the central result is not equivalent to its inputs by construction. The interpretive assumption that photometric variations arise from rotation is a standard modeling choice but does not reduce the reported period to a tautology or prior fit.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard photometric assumptions that brightness variations trace rotation and that the observed signal is not dominated by other effects.

free parameters (1)
  • rotation period
    Fitted value derived from light-curve periodicity analysis
axioms (1)
  • domain assumption Photometric variability is dominated by the asteroid's rotation
    Standard assumption in asteroid light-curve studies invoked to interpret the observed periodicity

pith-pipeline@v0.9.0 · 5563 in / 1137 out tokens · 41581 ms · 2026-05-08T16:37:03.657259+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

34 extracted references · 32 canonical work pages · 1 internal anchor

  1. [1]

    The Ninth Data Release of the Sloan Digital Sky M.R. Alarcon et al.:Preprint submitted to ElsevierPage 9 of 11 HiPERCAM characterisation of 2022 OB5 Survey: First Spectroscopic Data from the SDSS-III Baryon Oscillation Spectroscopic Survey. ApJS 203,

    2022

  2. [2]

    doi:10.1088/0067-0049/203/2/21 , eid =

    doi:10.1088/0067-0049/203/2/21, arXiv:1207.7137. Alarcon,M.R.,Licandro,J.,Serra-Ricart,M.,2026. Adedicatedsurveyof fast-rotatingnear-EarthasteroidswiththeTwo-meterTwinTelescope.I. Observational strategy and first results. A&A 707, A262. doi:10.1051/ 0004-6361/202558528,arXiv:2602.18562. Alarcon, M.R., Licandro, J., Serra-Ricart, M., Joven, E., Gaitan, V.,...

    work page doi:10.1088/0067-0049/203/2/21 2026

  3. [3]

    PASP 135, 055001

    Scientific CMOS Sensors in Astronomy: IMX455 and IMX411. PASP 135, 055001. doi:10.1088/1538-3873/acd04a, arXiv:2302.03700. Barbee, B.W., Esposito, T., Piñon, Elfego, I., Hur-Diaz, S., Mink, R.G., Adamo,D.R.,2010. Acomprehensiveongoingsurveyofthenear-earth asteroidpopulationforhumanmissionaccessibility,in:AIAA/AASAs- trodynamics Specialist Conference, Amer...

    work page doi:10.1088/1538-3873/acd04a 2010

  4. [4]

    In: 2018 AIAA Atmospheric Flight Mechanics Conference

    doi:10.2514/6. 2010-8368. Beniyama, J., Sako, S., Ohsawa, R., Takita, S., Kobayashi, N., Okumura, S.i., Urakawa, S., Yoshikawa, M., Usui, F., Yoshida, F., Doi, M., Niino, Y., Shigeyama, T., Tanaka, M., Tominaga, N., Aoki, T., Arima, N., Arimatsu,K.,Kasuga,T.,Kondo,S.,Mori,Y.,Takahashi,H.,Watanabe, J.i.,

    work page doi:10.2514/6 2010

  5. [5]

    PASJ74,877–903

    Video observations of tiny near-Earth objects with Tomo-e Gozen. PASJ74,877–903. doi:10.1093/pasj/psac043,arXiv:2207.07071. Binzel,R.P.,DeMeo,F.E.,Turtelboom,E.V.,Bus,S.J.,Tokunaga,A.,Bur- bine, T.H., Lantz, C., Polishook, D., Carry, B., Morbidelli, A., Birlan, M.,Vernazza,P.,Burt,B.J.,Moskovitz,N.,Slivan,S.M.,Thomas,C.A., Rivkin,A.S.,Hicks,M.D.,Dunn,T.,R...

    work page doi:10.1093/pasj/psac043

  6. [6]

    Icarus 324, 41–76

    Compositional distributions and evolutionary processes for the near-Earth object population: Results from the MIT- Hawaii Near-Earth Object Spectroscopic Survey (MITHNEOS). Icarus 324, 41–76. doi:10.1016/j.icarus.2018.12.035,arXiv:2004.05090. Binzel, R.P., Rivkin, A.S., Stuart, J.S., Harris, A.W., Bus, S.J., Burbine, T.H.,

    work page doi:10.1016/j.icarus.2018.12.035 2018

  7. [7]

    Icarus 170, 259–294

    Observed spectral properties of near-Earth objects: results for population distribution, source regions, and space weathering pro- cesses. Icarus 170, 259–294. doi:10.1016/j.icarus.2004.04.004. Cannon,K.M.,Gialich,M.,Acain,J.,2023. Preciousandstructuralmetals on asteroids. Planet. Space Sci. 225, 105608. doi:10.1016/j.pss.2022. 105608. Carry, B.,

    work page doi:10.1016/j.icarus.2004.04.004 2004

  8. [8]

    Density of asteroids. Planet. Space Sci. 73, 98–118. doi:10.1016/j.pss.2012.03.009,arXiv:1203.4336. Chambers, K.C., Magnier, E.A., Metcalfe, N., Flewelling, H.A., Huber, M.E., Waters, C.Z., Denneau, L., Draper, P.W., Farrow, D., Finkbeiner, D.P., Holmberg, C., Koppenhoefer, J., Price, P.A., Rest, A., Saglia, R.P.,Schlafly,E.F.,Smartt,S.J.,Sweeney,W.,Wains...

    work page doi:10.1016/j.pss.2012.03.009 2012

  9. [9]

    The Pan-STARRS1 Surveys

    The Pan-STARRS1 Surveys. arXiv e-prints , arXiv:1612.05560doi:10.48550/arXiv.1612.05560,arXiv:1612.05560. DeMeo, F.E., Binzel, R.P., Slivan, S.M., Bus, S.J.,

    work page internal anchor Pith review doi:10.48550/arxiv.1612.05560

  10. [10]

    E., Binzel, R

    An extension of the Bus asteroid taxonomy into the near-infrared. Icarus 202, 160–180. doi:10.1016/j.icarus.2009.02.005. DeMeo, F.E., Burt, B.J., Marsset, M., Polishook, D., Burbine, T.H., Carry, B., Binzel, R.P., Vernazza, P., Reddy, V., Tang, M., Thomas, C.A., Rivkin, A.S., Moskovitz, N.A., Slivan, S.M., Bus, S.J.,

    work page doi:10.1016/j.icarus.2009.02.005 2009

  11. [11]

    Icarus 380, 114971

    Con- necting asteroids and meteorites with visible and near-infrared spec- troscopy. Icarus 380, 114971. doi:10.1016/j.icarus.2022.114971, arXiv:2202.13797. DeMeo, F.E., Carry, B.,

    work page doi:10.1016/j.icarus.2022.114971 2022

  12. [12]

    E., & Carry, B

    The taxonomic distribution of asteroids from multi-filter all-sky photometric surveys. Icarus 226, 723–741. doi:10.1016/j.icarus.2013.06.027,arXiv:1307.2424. Devogèle, M., Buzzi, L., Micheli, M., Cano, J.L., Conversi, L., Jehin, E., Ferrais, M., Ocaña, F., Föhring, D., Drury, C., Benkhaldoun, Z., Jenniskens, P.,

    work page doi:10.1016/j.icarus.2013.06.027 2013

  13. [13]

    A&A 689, A211

    Aperture photometry on asteroid trails: Detection of the fastest-rotating near-Earth object. A&A 689, A211. doi:10.1051/ 0004-6361/202450263,arXiv:2404.04142. Devogèle,M.,Moskovitz,N.,Thirouin,A.,Gustaffson,A.,Magnuson,M., Thomas, C., Willman, M., Christensen, E., Person, M., Binzel, R., Pol- ishook,D.,DeMeo,F.,Hinkle,M.,Trilling,D.,Mommert,M.,Burt,B., Sk...

    work page arXiv 2019

  14. [14]

    doi:10.3847/1538-3881/ab43dd,arXiv:1909.04788. Dhillon, V.S., Bezawada, N., Black, M., Dixon, S.D., Gamble, T., Gao, X., Henry, D.M., Kerry, P., Littlefair, S.P., Lunney, D.W., Marsh, T.R., Miller,C.,Parsons,S.G.,Ashley,R.P.,Breedt,E.,Brown,A.,Dyer,M.J., Green, M.J., Pelisoli, I., Sahman, D.I., Wild, J., Ives, D.J., Mehrgan, L., Stegmeier,J.,Dubbeldam,C.M...

    work page doi:10.3847/1538-3881/ab43dd 1909

  15. [15]

    MNRAS 507, 350–366

    HiPERCAM: a quintuple-beam, high-speed optical imager on the 10.4-m Gran Tele- scopio Canarias. MNRAS 507, 350–366. doi:10.1093/mnras/stab2130, arXiv:2107.10124. Elvis,M.,McDowell,J.,Hoffman,J.A.,Binzel,R.P.,2011. Ultra-lowdelta- v objects and the human exploration of asteroids. Planet. Space Sci. 59, 1408–1412. doi:10.1016/j.pss.2011.05.006,arXiv:1105.41...

    work page doi:10.1093/mnras/stab2130 2011

  16. [16]

    , archivePrefix = "arXiv", eprint =

    doi:10.3847/0004-637X/822/2/66,arXiv:1512.01214. Fornasier, S., Clark, B.E., Dotto, E.,

    work page doi:10.3847/0004-637x/822/2/66

  17. [17]

    Icarus214,131–146

    Spectroscopic survey of X- typeasteroids. Icarus214,131–146. doi:10.1016/j.icarus.2011.04.022, arXiv:1105.3380. Gaia Collaboration, Vallenari, A., Brown, A.G.A., Prusti, T., de Brui- jne, J.H.J., Arenou, F., Babusiaux, C., Biermann, M., Creevey, O.L., Ducourant, C., Evans, D.W., Eyer, L., Guerra, R., Hutton, A., Jordi, C., Klioner, S.A., Lammers, U.L., Li...

    work page doi:10.1016/j.icarus.2011.04.022 2011

  18. [18]

    2023 , month = jun, journal =

    Summary of the content and survey properties. A&A 674, A1. doi:10.1051/0004-6361/202243940,arXiv:2208.00211. Granvik, M., Morbidelli, A., Jedicke, R., Bolin, B., Bottke, W.F., Beshore, E., Vokrouhlický, D., Nesvorný, D., Michel, P.,

    work page doi:10.1051/0004-6361/202243940

  19. [19]

    doi:10.1016/j.icarus.2018.04.018 , eprint =

    Debiased orbit andabsolute-magnitudedistributionsfornear-Earthobjects. Icarus312, 181–207. doi:10.1016/j.icarus.2018.04.018,arXiv:1804.10265. Harris,A.W.,D’Abramo,G.,2015. Thepopulationofnear-Earthasteroids. Icarus 257, 302–312. doi:10.1016/j.icarus.2015.05.004. Harris, A.W., Drube, L.,

    work page doi:10.1016/j.icarus.2018.04.018 2018

  20. [20]

    ApJL 785, L4

    How to Find Metal-rich Asteroids. ApJL 785, L4. doi:10.1088/2041-8205/785/1/L4,arXiv:1403.6346. Holmberg, J., Flynn, C., Portinari, L.,

    work page doi:10.1088/2041-8205/785/1/l4 2041

  21. [21]

    Gallazzi, S

    The colours of the Sun. MNRAS 367, 449–453. doi:10.1111/j.1365-2966.2005.09998.x, arXiv:astro-ph/0511158. Holsapple,K.A.,2007. SpinlimitsofSolarSystembodies:Fromthesmall fast-rotatorsto2003EL61. Icarus187,500–509. doi:10.1016/j.icarus. 2006.08.012. Kargel, J.S.,

    work page doi:10.1111/j.1365-2966.2005.09998.x 2005

  22. [22]

    Metalliferous asteroids as potential sources of precious metals. J. Geophys. Res. 99, 21129–21142. doi:10.1029/94JE02141. King, D.L.,

    work page doi:10.1029/94je02141

  23. [23]

    Observa- tions of two superfast rotator NEAs: 2021 NY1 and 2022 AB

    Licandro, J., Popescu, M., Tatsumi, E., Alarcon, M.R., Serra-Ricart, M., Medeiros,H.,Morate,D.,Tinaut-Ruano,F.,deLeón,J.,2023. Observa- tions of two superfast rotator NEAs: 2021 NY1 and 2022 AB. MNRAS 521, 3784–3792. doi:10.1093/mnras/stad708,arXiv:2303.05099. Lomb,N.R.,1976. Least-SquaresFrequencyAnalysisofUnequallySpaced Data. Ap&SS 39, 447–462. doi:10....

    work page doi:10.1093/mnras/stad708 2023

  24. [24]

    arXiv e-prints , arXiv:2603.15872doi:10.48550/arXiv.2603.15872,arXiv:2603.15872

    NEO Colors from The Mission Accessible Near-Earth Object Survey (MANOS). arXiv e-prints , arXiv:2603.15872doi:10.48550/arXiv.2603.15872,arXiv:2603.15872. Perna, D., Barucci, M.A., Fulchignoni, M., Popescu, M., Belskaya, I., Fornasier, S., Doressoundiram, A., Lantz, C., Merlin, F.,

    work page doi:10.48550/arxiv.2603.15872

  25. [25]

    A spec- troscopic survey of the small near-Earth asteroid population: Peculiar taxonomic distribution and phase reddening. Planet. Space Sci. 157, 82–95. doi:10.1016/j.pss.2018.03.008,arXiv:1803.08953. Pravec, P., Harris, A.W., Kušnirák, P., Galád, A., Hornoch, K.,

    work page doi:10.1016/j.pss.2018.03.008 2018

  26. [26]

    Icarus 221, 365–387

    Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations. Icarus 221, 365–387. doi:10.1016/j.icarus.2012.07.026. Sánchez, P., Scheeres, D.J.,

    work page doi:10.1016/j.icarus.2012.07.026 2012

  27. [27]

    Meteorit

    The strength of regolith and rubble pile asteroids. Meteorit. Planet. Sci. 49, 788–811. doi:10.1111/maps.12293, arXiv:1306.1622. Scargle, J.D.,

    work page doi:10.1111/maps.12293

  28. [28]

    Studies in astronomical time series analysis. II. Statisticalaspectsofspectralanalysisofunevenlyspaceddata. ApJ263, 835–853. doi:10.1086/160554. Scheeres, D.J., Hartzell, C.M., Sánchez, P., Swift, M.,

    work page doi:10.1086/160554

  29. [29]

    Icarus 210, 968–984

    Scaling forces to asteroid surfaces: The role of cohesion. Icarus 210, 968–984. doi:10.1016/j.icarus.2010.07.009,arXiv:1002.2478. Schubert, P.J.,

    work page doi:10.1016/j.icarus.2010.07.009 2010

  30. [30]

    Nicolás, The bar derived category of a curved dg algebra, Journal of Pure and Applied Algebra 212 (2008) 2633–2659

    Economical extraction of platinum from main belt asteroids. Advances in Space Research 75, 6132–6139. doi:10.1016/j. asr.2025.02.035. Snowden, C.,

    work page doi:10.1016/j 2025

  31. [31]

    URL:https://www.astroforge.com/updates-collection/ odint-mission-debrief

    Odin’t: A complete debrief of our deep space mission. URL:https://www.astroforge.com/updates-collection/ odint-mission-debrief. AstroForge, accessed 2026-03-21. Stellingwerf, R.F.,

    2026

  32. [32]

    , keywords =

    Period determination using phase dispersion minimization. ApJ 224, 953–960. doi:10.1086/156444. Thirouin, A., Moskovitz, N., Binzel, R.P., Christensen, E., DeMeo, F.E., Person, M.J., Polishook, D., Thomas, C.A., Trilling, D., Willman, M., Hinkle, M., Burt, B., Avner, D., Aceituno, F.J.,

    work page doi:10.1086/156444

  33. [33]

    Tholen, D.J.,

    doi:10.3847/0004-6256/152/6/163,arXiv:1607.03517. Tholen, D.J.,

    work page doi:10.3847/0004-6256/152/6/163

  34. [34]

    Astrodynamics 5, 293–329

    Shapes, structures, and evolution of small bodies. Astrodynamics 5, 293–329. doi:10.1007/s42064-021-0128-7. M.R. Alarcon et al.:Preprint submitted to ElsevierPage 11 of 11

    work page doi:10.1007/s42064-021-0128-7