Pith. sign in

REVIEW 3 major objections 6 minor 2 cited by

JWST Reveals Varied Origins Between Jupiter's Irregular Satellites

T0 review · 3 major / 6 minor · reviewed 2026-08-10 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read JWST spectra show Jupiter's irregular moons carry at least three surface compositions, with Himalia and Elara matching Ceres-like ammoniated phyllosilicates.

desk verdict First JWST spectra of Jupiter's irregular satellites show real compositional diversity; the ammoniated phyllosilicate identification on Himalia/Elara is an interpretation, not a detection, and the paper's own alternative fit is just as good. read the letter →

arxiv 2501.16484 v2 pith:PETHW4RC submitted 2025-01-27 astro-ph.EP

Benjamin N. L. Sharkey , Andrew S. Rivkin , Richard J. Cartwright , Bryan J. Holler , Joshua P. Emery , Cristina Thomas This is my paper · ORCID
classification astro-ph.EP
keywords JupiterirregularsatellitesJWSTNIRSpecspectroscopyammoniatedphyllosilicatesHimaliafamily3micronabsorptionbandaqueousalterationJovianTrojanssatelliteorigins
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Jupiter's irregular satellites - captured moons on wide, tilted orbits - are usually assumed to share a single origin reservoir. This paper uses JWST near-infrared spectra of eight of them to show they do not: the surfaces fall into at least three distinct compositional classes. The two largest, Himalia and Elara, display a 2.7 and 3.05 micron absorption complex that best matches laboratory ammoniated phyllosilicates, clays with ammonium in their structure, similar to the dwarf planet Ceres and unlike any meteorite. The retrograde satellite Ananke shows a 3 micron band consistent with phyllosilicates in water-altered carbonaceous chondrites, the first such signature in the retrograde swarm. The paper argues that the Himalia parent body was heterogeneous and Ceres-like, and that Jupiter captured bodies with different initial compositions or different heating histories, which would make the irregular satellites a record of multiple formation environments rather than one captured population.

What carries the argument

The load-bearing object is the 3 micron absorption complex measured by JWST NIRSpec, specifically the combination of the sharp 2.7 micron metal-OH stretch and the rounded 3.05 micron NH4-related minimum that together fingerprint ammoniated phyllosilicates. Comparison of band centers, depths, and shapes across the sample separates the eight satellites into four spectral groups, while Elara's intermediate spectrum - reproduced as a mean of Himalia and Lysithea - supplies the key evidence that the Himalia family members share a single heterogeneous parent body. The band pair also carries the link to Ceres, whose 2.72 and 3.05 micron features provide the closest known analog.

What would settle it

Measure the 3.05 micron band on a freshly exposed crater on Himalia: ammoniated phyllosilicates decompose above about 600 K, so a band that persists on unheated, fresh surface material would support the Ceres-like interpretation, while a band appearing only after space weathering would point to a radiolytic product.

Watch

Extended reading notes

Core claim

On its own terms, the paper establishes that Jupiter's irregular satellites carry at least three surface types rather than the single Trojan-like composition previously inferred from color. Himalia and Elara show a sharp 2.72 micron band and a rounded 3.05 micron band that match ammoniated phyllosilicates; Ananke's deep, rounded 3 micron band resembles phyllosilicates found in water-altered carbonaceous chondrites (petrologic type 2); and Carme, Sinope, and Themisto reproduce the 3.0 and 3.4 micron absorptions of red Jovian Trojans, with Lysithea and Pasiphae falling between the Trojan and hydrated-chondrite band centers. The paper further finds that Elara's 3 micron complex is approximately a 50/50 average of Himalia's and Lysithea's bands, and proposes that the Himalia family came from a single heterogeneous parent analogous to Ceres with regard to water, organics, and ammonium. The conclusion is that Jupiter captured bodies that either formed from different initial compositions or experienced different levels of aqueous alteration.

Load-bearing premise

The interpretation that Himalia's 2.7 plus 3.05 micron band complex comes from ammoniated phyllosilicates rests on a non-unique spectral match, since the paper notes that a two-component mixture of the C2 chondrite Essebi and 67P-like ammonium salts fits equally well and no meteorite shows the 3.05 micron feature.

Editorial extensions

If this is right

  • Himalia and Elara become the first Jovian irregular satellites with a Ceres-like ammonium-bearing surface, implying that ammonium-bearing material existed in the captured planetesimal population.
  • Ammonia-bearing dust from the Himalia family could deliver nitrogen to the Galilean moons, contributing to Callisto's CN-related 4.57 micron feature and to Europa's ocean through subsurface conduits.
  • Red-Trojan-like 3.0 and 3.4 micron absorptions on Carme, Sinope, and Themisto show that these surface components either survived collisional fragmentation after capture or form in the circumjovian environment.
  • Ananke's water-altered phyllosilicate band places aqueous alteration inside the retrograde satellite swarm for the first time, so water-altered material was available to retrograde capture.
  • Elara's spectrum as a mean of Himalia and Lysithea predicts that smaller Himalia family members sample an alteration gradient, a trend that future targeted observations can check.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the Himalia parent body is Ceres-like, then the family's collisional dust is a nitrogen source for Europa's ocean; the paper lays out the delivery route but does not quantify the flux, leaving a gap a dynamical model could fill.
  • The intermediate 3 micron band centers of Lysithea and Pasiphae may define a spectral class bridging Trojans and hydrated chondrites; a survey of 3 micron bands across other small-body collisional families would tell whether this class is a separate reservoir or a weakly altered Trojan material.
  • Since no known meteorite displays the 3.05 micron feature, confirming ammoniated phyllosilicates on Himalia would imply that some ammonia-bearing parent bodies are absent from the meteorite collection, or that their samples were destroyed by terrestrial alteration.
  • Treating Elara as a mixture of Himalia and Lysithea end-members suggests a simple linear mixing rule that future modeling could invert to map material fractions across the Himalia family, though the paper does not carry out such an inversion.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. The paper presents JWST NIRSpec 0.7–5.2 μm reflectance spectra of eight Jovian irregular satellites (Himalia, Elara, Lysithea, Pasiphae, Sinope, Carme, Ananke, Themisto), grouped into four spectral classes. It reports that the three large Himalia family members have different 3 μm band complexes, with Himalia and Elara showing a 2.7 + 3.05 μm complex that the authors attribute to ammoniated phyllosilicates; that the red objects Carme, Sinope, and Themisto resemble red Jovian Trojans; that Ananke shows a rounded 3 μm band similar to aqueously altered C2 chondrites; and that Pasiphae and Lysithea share an intermediate 3 μm absorber. The paper argues for a heterogeneous, Ceres-like Himalia parent body, discusses nitrogen delivery to the Galilean moons, and proposes that irregular satellites and Trojans may have complex, partially separate origins.

Significance. If the compositional identifications hold, this is a major observational advance: it is the first high-SNR 3 μm survey of Jupiter's irregular satellites, provides a consistent reduction of JWST Trojan comparison spectra, and offers concrete new constraints on the formation and alteration histories of these captured bodies. The detections of complexed CO2 on Himalia/Elara and aqueous alteration products on Ananke are important and robust. The paper also makes a valuable methodological contribution by showing that Trojans and irregular satellites can be compared on a uniform reduction pipeline. However, the central claim that Himalia and Elara contain ammoniated phyllosilicates is not uniquely constrained by the data, and the quantitative band parameters lack propagated systematic uncertainties; these issues affect the parent-body and nitrogen-delivery interpretations.

major comments (3)
  1. [§4, Abstract, §9] The identification of ammoniated phyllosilicates on Himalia and Elara is presented as the central result ('contain ammoniated phyllosilicates' in the Abstract and Conclusions), but the paper itself shows that the 2.7 + 3.05 μm complex is also well matched by a two-component mixture of the C2 chondrite Essebi and 67P-like ammonium salts (Fig. 7, right), and explicitly states that no meteorite shows the 3.05 μm feature. The preference for ammoniated phyllosilicates rests on 'simplicity as a single-absorber fit,' which is not a spectral discriminator among NH-bearing phases. Because the Ceres-like parent-body interpretation and the nitrogen-delivery argument in Section 6 depend on the specific NH4-in-phyllosilicate assignment, the paper should either (a) present ammoniated phyllosilicates as one of several viable carriers, with the Ceres-like and nitrogen-delivery conclusions correspondingly downgraded, or (b) add quantitative spectral modeling (e.g., band-strength ratios for NH4 vs. NH3-bearing salts, or radiative-transfer mixing) that can break the degeneracy. As written, the claim exceeds the evidence.
  2. [§2, §3.1, Table 2] The reported band centers and depths (Table 2) incorporate only random uncertainties from the Monte Carlo resampling; they do not include systematic errors from the NEATM thermal subtraction or from the choice of continuum polynomial order and breakpoints. The thermal model is fit with free albedo and beaming parameter and iterated 'until a smooth output spectrum was produced' (Section 2), and the global continuum order varies between 2 and 4 per object (Section 3.1). These choices can shift 3 μm band centers by tens of nanometers, which is comparable to the 0.03–0.05 μm separations used to define the spectral groups (e.g., Ananke at 2.93 μm vs. Pasiphae/Lysithea at 2.94–2.97 μm). The authors should quantify the sensitivity of Table 2 parameters to alternative thermal models and continuum definitions, or explicitly state that the quantitative group separations are not robust to these systematics.
  3. [§5, Figure 8] The claim that Elara's 3 μm band is a simple average of Himalia and Lysithea is based on a visual comparison with a multiplicative rescaling factor of 1.07; no goodness-of-fit metric or uncertainty is provided. This comparison is used to argue that Himalia, Elara, and Lysithea share a single heterogeneous parent body. The paper should quantify the agreement (e.g., reduced chi-square between Elara and the scaled Himalia/Lysithea mean) or present the comparison as a qualitative suggestion rather than a supporting observation for the common-parent-body hypothesis.
minor comments (6)
  1. [Title and §1 intro] The manuscript title contains 'V aried' (spacing error); the abstract also contains the typo 'the the' in the sentence describing the Himalia family sample.
  2. [§3.2] The text reporting the ground-based comparison says 'discrepencies'; it should read 'discrepancies'.
  3. [§5] The phrase 'heterogeneous aqeuous alteration' contains a typo; it should be 'aqueous alteration'.
  4. [Table 2] For Ananke and Elara, the 2.63–2.67 μm feature is listed with band depths of 1.4±1.4% and 1.2±1.5% (both consistent with zero) and an attribution of '?'. Given the text also inconsistently describes which objects show this feature (Section 3.2 says Lysithea has it, while Section 5 says Himalia and Lysithea display it), the table and text should be reconciled and these non-detections should be flagged as tentative or removed.
  5. [Figure 6 caption] The caption states that all compared bodies 'show the 3.05 micron feature,' but the 67P feature is attributed to ammonium salts and is broader than the narrow band on Himalia; this could be phrased more carefully to avoid implying the absorbers are identical.
  6. [§6] The nitrogen-delivery discussion is written conditionally in places but would benefit from an explicit caveat that the NH4-bearing species identification is non-unique; in particular, the statement that 'NH4-bearing species on Himalia and Elara represent an important source of nitrogen' should be explicitly contingent on the band assignment.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the paper's compositional conclusions are comparisons to external laboratory and independent JWST datasets, not consequences of fitted constants or self-citation chains.

full rationale

The manuscript is an observational spectroscopy paper. Its reduction pipeline (template PSF fitting from Wong et al. 2024) is a methodological choice, not a scientific ansatz, and the Eurybates spectrum is reprocessed with the same pipeline only for consistency (Section 3.2). The central detections—the 2.7/3.05 micron complex on Himalia and Elara, the 3 micron bands on the other satellites, and the 4.27 micron CO2 features—are identified by direct comparison to external laboratory data (De Angelis et al. 2021), meteorite spectra (Takir et al. 2019; Yu et al. 2024), and independently published Trojan observations (Wong et al. 2024). Band centers and depths are measured from the data via Monte Carlo resampling (Section 3.1) and are not derived from any fitted parameter that already encodes the conclusion. The NEATM thermal subtraction uses albedo and beaming parameter as free parameters, but it is a data-calibration step, not a prediction engine. The paper explicitly concedes that the Himalia band complex is also matched by an Essebi/67P mixture (Section 4), which weakens the uniqueness of the ammoniated-phyllosilicate identification, but that is a non-uniqueness or interpretive limitation, not circularity. No self-citation chain is load-bearing: Wong et al. (2024) is an external dataset with a co-author overlap, but the cited spectra and laboratory results stand independently of this paper's fitted values. Therefore no circular step can be exhibited.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The central compositional claims rest on the spectral interpretation of 3 micron bands and on the thermal and continuum reduction. Free parameters in the NEATM model and continuum choices affect band parameters; the mineralogical attribution to ammoniated phyllosilicates relies on domain assumptions about spectral matching to lab and meteorite samples. No new physical entities are introduced.

free parameters (4)
  • NEATM geometric albedo (fit per target, 8 targets) = not reported; initial 2%
    Free parameter in the thermal model used to subtract thermal emission; affects the 3-5 micron continuum and all band depths and centers.
  • NEATM beaming parameter eta (fit per target, 8 targets) = not reported; initial 1.0
    Free parameter in the NEATM fit; controls the shape of the thermal tail; systematic uncertainty not propagated.
  • Global continuum polynomial order (per object, order 2-4) = not reported per object
    Chosen by hand to define continua on either side of the 3 micron complex; affects band measurements.
  • Reflected component baseline (linear extension of slope at thermal cut-on) = not reported
    Iterated until a smooth output spectrum is produced; a subjective choice that can influence band shapes and depths.
assumptions (5)
  • domain assumption The NIRSpec calibration pipeline (v1.14.0, context jwst 1225.pmap) and the template PSF extraction routine produce accurate, background-subtracted 1D spectra.
    Invoked in Section 2; the entire analysis rests on the correctness of this reduction.
  • domain assumption SNAP-2 is an appropriate solar analog star for dividing out the reflected solar component.
    Section 2; if the standard star spectrum mismatches the Sun, reflectance spectra and band depths would be biased.
  • domain assumption The NEATM model with free albedo and beaming parameter adequately represents the thermal emission of these small, irregularly shaped satellites in the 4-5 micron region.
    Section 2; thermal subtraction shapes the continuum and the 3-5 micron bands. The paper does not explore degeneracies.
  • domain assumption The orbital family groupings (Himalia, Ananke, Carme, Pasiphae) reflect collisional families from single parent bodies.
    Section 1 and Figure 1; the inference that Himalia, Elara, and Lysithea share a parent body relies on this grouping.
  • domain assumption Spectral matches to laboratory samples of ammoniated phyllosilicates and meteorite spectra are diagnostic of surface mineralogy.
    Section 4; the Ceres-like ammonium interpretation depends on the uniqueness of these matches, which the paper acknowledges is not unique.

how reviews work

0 comments
Cite this review

Pith. "Pith review of JWST Reveals Varied Origins Between Jupiter's Irregular Satellites." pith.science (2026). https://pith.science/paper/PETHW4RC

@misc{pith2026250116484,
  author       = {Pith},
  title        = {Pith review of: JWST Reveals Varied Origins Between Jupiter's Irregular Satellites},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/PETHW4RC}},
  note         = {Machine review of arXiv:2501.16484}
}
abstract

We report observations of eight Jovian irregular satellites with JWST's NIRSpec instrument: Himalia, Elara, Pasiphae, Sinope, Lysithea, Carme, Ananke, and Themisto. Irregular satellite families, which are presumed to have formed via collisions, contain various Trojan-like and C-type-asteroid-like surfaces. We sample the three largest members of the Himalia satellite family, detecting the presence of complexed CO$_2$ and a unique absorption band from $\sim2.7-3.6\ \mu m$ whose character correlates with satellite size. The two largest irregular satellites, Himalia family members Himalia and Elara, contain ammoniated phyllosilicates that are not seen in the meteorite inventory. We propose that the Himalia parent body was heterogeneous and formed with materials similar to Ceres-like ammonium-bearing asteroids. Several small ($D\sim 10km$) irregular satellites closely track the colors and absorption bands of ``red'' Jovian Trojans, demonstrating that these compositions are retained amongst the products of collisions that occurred after Jovian capture. We report the first detection of aqueous alteration products in the retrograde satellite swarm, finding Ananke's 3 micron band to closely match phyllosilicates seen in C2 chondrites. Notably, objects with OH absorption features similar to the Trojan asteroid Eurybates are found in both the retrograde Pasiphae family and the prograde Himalia family, confounding a simple link between such materials and a single surface type. The irregular satellites appear consistent with some materials that experienced alteration from liquid water and others that did not. Consequently, Jupiter may have captured bodies that formed from different initial compositions, or bodies that experienced different levels of heating, driving differential alteration processes.

Figures

Figures reproduced from arXiv: 2501.16484 by the authors.

Figure 1
Figure 1. Irregular satellite orbital inclinations and semimajor axes (normalized to Jupiter’s Hill radius). Family groupings are given as indicated. The prograde population is dominated in mass and number by the Himalia family. The retrograde population is categorized into three orbital families, with the more widely dispersed Pasiphae and Ananke families and the more tightly grouped Carme family. This work studies the Himal… view at source ↗
Figure 2
Figure 2. Top: Estimated thermal flux (data points) and resulting NEATM best-fit thermal model (blue curve) for irregular satellite Lysithea. Fits were performed by varying target albedo and beaming parameter to reproduce the cut-on wavelength where measurable thermal emission begins (typically near 4.0 microns, related to the observed surface’s temperature), as well as the shape and magnitude of the thermal fluxes at longer … view at source ↗
Figure 3
Figure 3. Left: Processed relative reflectances for all observed targets in JWST GO 4028, labeled according to groupings identified in the text. Right: Continuum-divided reflectances using a polynomial of order 2-4 fit on either side of major absorption bands. Objects are normalized to have reflectance equal to 1 at 2.5 microns, and displayed with offsets for ease of comparison. Targets are arranged according to spectral char… view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: Comparison of the 3 µm band complex on Lysithea (prograde, Himalia group) and Pasiphae (retrograde, Pasiphae group). The centers and depths of these features are highly similar. Lysithea includes an additional narrow absorption near 2.63 µm, and Pasiphae includes a nar…
Figure 5
Figure 5. Figure 5: Continuum-divided reflectance of the 4.15 to 4.40 µm region of Himalia and Elara. They are compared with previous observations of Jovian Trojan Eurybates, which was reprocessed using the same reduction pipeline. The two irregular satellites show features near 4.27µm th…
Figure 6
Figure 6. Figure 6: Himalia compared with other small solar system bodies that show the 3.05 micron feature. While Himalia shows major spectral features similar to Ceres (Kurokawa et al. 2020) at 2.7 and 3.05 microns, the differing relative strength of these bands suggest novel materials …
Figure 7
Figure 7. Figure 7: Left: Comparison of Himalia’s continuum-divided 3.0 micron band complex to laboratory samples of ammoniated Illite from De Angelis et al. (2021). Note that absorption band depths are rescaled to approximate Himalia’s 2.7 micron feature, as pure laboratory samples have …
Figure 8
Figure 8. Figure 8: The 3 µm regions of Himalia family objects (with shifts for Lysithea and Himalia of ±0.05 for readability) . Note that Lysithea displays a sharper band, overprinted by numerous subtle absorptions, while Elara and Himalia have more rounded features near 3 µm. Bottom: We…
Figure 9
Figure 9. Figure 9: Comparisons of 3µm band complexes between irregular satellites Themisto, Sinope, and Carme to the Jovian Trojans Leucus and Patroclus. Band depths for all objects were normalized at 3.0µm to aid comparisons of the relative strengths and shapes of the 3.0 and 3.4 µm ban…
Figure 10
Figure 10. Figure 10: The 3.0 µm band shapes for: irregular satellites Lysithea and Ananke; meteorites Murchison and DOM 10085; Jupiter Trojans Eurybates and Polymele. Objects are sorted according to the central wavelength (λc) of their features, which is marked by a square on each curve. …
Figure 11
Figure 11. Figure 11: The 3 µm band centers vs. band depths of Jovian Trojan and irregular satellites with available band analysis parameters, from this work and (Wong et al. 2024). Himalia and Elara are excluded from this analysis due to their overlapping features at 2.7 and 3.0 microns, …

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 2 Pith papers

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

  1. Spectroscopic Mapping of Callisto with HST/STIS and Implications for its Surface Composition

    astro-ph.EP 2025-05 conditional novelty 7.0 of 10

    Global UV-visible maps of Callisto trace regional surface compositions and indicate that the 280 nm band previously attributed to SO2 is better explained by dividing a leading-hemisphere 320 nm band by a trailing-hemi...

  2. Tracing the source of carbon oxides on the large moons of Uranus

    astro-ph.EP 2026-07 conditional novelty 6.5 of 10

    Exposed carbon oxides on Uranus's large moons are potentially native, with trailing-hemisphere concentrations and crystalline spectral signatures shaped by irradiation and seasonal sublimation-condensation cycles.

Reference graph

Works this paper leans on

105 extracted references · 25 canonical work pages · cited by 2 Pith papers

  1. [1]

    2018, Astronomy & Astrophysics, 620, A123

    Accolla, M., Pellegrino, G., Baratta, G., et al. 2018, Astronomy & Astrophysics, 620, A123

    2018

  2. [2]

    C., Ciarniello, M., et al

    Ammannito, E., DeSanctis, M. C., Ciarniello, M., et al. 2016, Science, 353, aaf4279, doi: 10.1126/science.aaf4279

    doi:10.1126/science.aaf4279 2016

  3. [3]

    A., Burbanks, A

    Astakhov, S. A., Burbanks, A. D., Wiggins, S., & Farrelly, D. 2003, Nature, 423, 264, doi: 10.1038/nature01622

    work page doi:10.1038/nature01622 2003

  4. [4]

    2010, GeoCoA, 74, 4881, doi: 10.1016/j.gca.2010.05.020

    Beck, P., Quirico, E., Montes-Hernandez, G., et al. 2010, GeoCoA, 74, 4881, doi: 10.1016/j.gca.2010.05.020

    doi:10.1016/j.gca.2010.05.020 2010

  5. [5]

    Belyakov, M., & Brown, M. E. 2025, PSJ, 6, 97, doi: 10.3847/PSJ/adc55d

    doi:10.3847/psj/adc55d 2025

  6. [6]

    2017, A&A, 608, A67, doi: 10.1051/0004-6361/201630361

    Bhatt, M., Reddy, V., Schindler, K., et al. 2017, A&A, 608, A67, doi: 10.1051/0004-6361/201630361

    doi:10.1051/0004-6361/201630361 2017

  7. [7]

    L., King, S

    Bishop, J. L., King, S. J., Lane, M. D., et al. 2021, Earth and Space Science, 8, e01844, doi: 10.1029/2021EA001844

    doi:10.1029/2021ea001844 2021

  8. [8]

    2019, ACS Earth and Space Chemistry, 3, 1550, doi: 10.1021/acsearthspacechem.9b00130

    Biver, N., & Bockel´ ee-Morvan, D. 2019, ACS Earth and Space Chemistry, 3, 1550, doi: 10.1021/acsearthspacechem.9b00130

    work page doi:10.1021/acsearthspacechem.9b00130 2019

Show all 105 references
  1. [9]

    2010, AJ, 139, 994, doi: 10.1088/0004-6256/139/3/994

    Morbidelli, A. 2010, AJ, 139, 994, doi: 10.1088/0004-6256/139/3/994

    2010 doi

  2. [10]

    F., Vokrouhlick´ y, D., Nesvorn´ y, D., & Moore, J

    Bottke, W. F., Vokrouhlick´ y, D., Nesvorn´ y, D., & Moore, J. M. 2013, Icarus, 223, 775, doi: 10.1016/j.icarus.2013.01.008

    2013 doi

  3. [11]

    F., Vokrouhlick´ y, D., Marschall, R., et al

    Bottke, W. F., Vokrouhlick´ y, D., Marschall, R., et al. 2023, PSJ, 4, 168, doi: 10.3847/PSJ/ace7cd

    2023 doi

  4. [12]

    F., Vokrouhlick` y, D., Nesvorn` y, D., et al

    Bottke, W. F., Vokrouhlick` y, D., Nesvorn` y, D., et al. 2024, The Planetary Science Journal, 5, 88

    2024

  5. [13]

    Brown, M. E. 2016, AJ, 152, 159, doi: 10.3847/0004-6256/152/6/159

    2016 doi

  6. [14]

    E., & Rhoden, A

    Brown, M. E., & Rhoden, A. R. 2014, ApJL, 793, L44, doi: 10.1088/2041-8205/793/2/L44

    2014 doi

  7. [15]

    E., Wong, I., & Belyakov, M

    Brown, M. E., Wong, I., & Belyakov, M. 2025, PSJ, 6, 22, doi: 10.3847/PSJ/ad9a60

    2025 doi

  8. [16]

    H., Baines, K

    Brown, R. H., Baines, K. H., Bellucci, G., et al. 2003, Icarus, 164, 461, doi: 10.1016/S0019-1035(03)00134-9

    2003 doi

  9. [17]

    2023, ApJL, 951, L33, doi: 10.3847/2041-8213/acdf5c

    Brunetto, R., Lantz, C., Fukuda, Y., et al. 2023, ApJL, 951, L33, doi: 10.3847/2041-8213/acdf5c

    2023 doi

  10. [18]

    A., Lamy, P

    Burns, J. A., Lamy, P. L., & Soter, S. 1979, Icarus, 40, 1

    1979

  11. [19]

    2024, JWST Calibration Pipeline, 1.14.0, Zenodo, doi: 10.5281/zenodo.10870758

    Bushouse, H., Eisenhamer, J., Dencheva, N., et al. 2024, JWST Calibration Pipeline, 1.14.0, Zenodo, doi: 10.5281/zenodo.10870758

    2024 doi

  12. [20]

    C., Reddy, V., Sharkey, B

    Cantillo, D. C., Reddy, V., Sharkey, B. N. L., et al. 2021, PSJ, 2, 95, doi: 10.3847/PSJ/abf63b

    2021 doi

  13. [21]

    2002, Icarus, 157, 456

    Yavrouian, A. 2002, Icarus, 157, 456

    2002

  14. [22]

    J., Nordheim, T

    Cartwright, R. J., Nordheim, T. A., Cruikshank, D. P., et al. 2020, ApJL, 902, L38, doi: 10.3847/2041-8213/abbdae

    2020 doi

  15. [23]

    J., Villanueva, G

    Cartwright, R. J., Villanueva, G. L., Holler, B. J., et al. 2024, The Planetary Science Journal, 5, 60

    2024

  16. [24]

    J., Hibbitts, C

    Cartwright, R. J., Hibbitts, C. A., Holler, B. J., et al. 2025, PSJ, 6, 125, doi: 10.3847/PSJ/adcab9

    2025 doi

  17. [25]

    A., & Brown, R

    Chamberlain, M. A., & Brown, R. H. 2004, Icarus, 172, 163, doi: 10.1016/j.icarus.2003.12.016

    2004 doi

  18. [26]

    2024, Monthly Notices of the Royal Astronomical Society, 527, 11327

    Chen, Z., Yang, K., & Liu, X. 2024, Monthly Notices of the Royal Astronomical Society, 527, 11327

    2024

  19. [27]

    F., Weaver, H

    Cheng, A. F., Weaver, H. A., Nguyen, L., et al. 2010, in 41st Annual Lunar and Planetary Science Conference, Lunar and Planetary Science Conference, 2549

    2010

  20. [28]

    A., Hiroi, T., Gaffey, M

    Cloutis, E. A., Hiroi, T., Gaffey, M. J., Alexander, C. M. O. D., & Mann, P. 2011a, Icarus, 212, 180, doi: 10.1016/j.icarus.2010.12.009

    2010 doi

  21. [29]

    A., Hudon, P., Hiroi, T., Gaffey, M

    Cloutis, E. A., Hudon, P., Hiroi, T., Gaffey, M. J., & Mann, P. 2011b, Icarus, 216, 309, doi: 10.1016/j.icarus.2011.09.009

    2011 doi

  22. [30]

    A., Pietrasz, V

    Cloutis, E. A., Pietrasz, V. B., Kiddell, C., et al. 2018, Icarus, 305, 203, doi: 10.1016/j.icarus.2018.01.015

    2018 doi

  23. [31]

    Colombo, G., & Franklin, F. A. 1971, Icarus, 15, 186, doi: 10.1016/0019-1035(71)90073-X ´Cuk, M., & Burns, J. A. 2004, Icarus, 167, 369, doi: 10.1016/j.icarus.2003.09.026 De Angelis, S., Ferrari, M., De Sanctis, M. C., et al. 2021, Journal of Geophysical Research (Planets), 12...

    1971

  24. [32]

    P., & Brown, R

    Emery, J. P., & Brown, R. H. 2003, Icarus, 164, 104, doi: 10.1016/S0019-1035(03)00143-X

    2003 doi

  25. [33]

    P., Burr, D

    Emery, J. P., Burr, D. M., & Cruikshank, D. P. 2011, AJ, 141, 25, doi: 10.1088/0004-6256/141/1/25

    2011 doi

  26. [34]

    F., Moore, M

    Ferrante, R. F., Moore, M. H., Spiliotis, M. M., & Hudson, R. L. 2008, ApJ, 684, 1210, doi: 10.1086/590362

    2008 doi

  27. [35]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, PASP, 125, 306, doi: 10.1086/670067

    2013 doi

  28. [36]

    2021, ARA&A, 59, 203, doi: 10.1146/annurev-astro-120920-010005

    Gladman, B., & Volk, K. 2021, ARA&A, 59, 203, doi: 10.1146/annurev-astro-120920-010005

    2021 doi

  29. [37]

    2018, Icarus, 306, 319, doi: 10.1016/j.icarus.2017.10.018

    Nogueira, E. 2018, Icarus, 306, 319, doi: 10.1016/j.icarus.2017.10.018

    2018 doi

  30. [38]

    2005, Icarus, 177, 570

    Gomis, O., & Strazzulla, G. 2005, Icarus, 177, 570

    2005

  31. [39]

    M., Mainzer, A

    Grav, T., Bauer, J. M., Mainzer, A. K., et al. 2015, ApJ, 809, 3, doi: 10.1088/0004-637X/809/1/3

    2015 doi

  32. [40]

    Grav, T., & Holman, M. J. 2004, ApJL, 605, L141, doi: 10.1086/420881

    2004 doi

  33. [41]

    J., Gladman, B

    Grav, T., Holman, M. J., Gladman, B. J., & Aksnes, K. 2003, Icarus, 166, 33, doi: 10.1016/j.icarus.2003.07.005

    2003 doi

  34. [42]

    2018, AJ, 155, 184, doi: 10.3847/1538-3881/aab49b

    Graykowski, A., & Jewitt, D. 2018, AJ, 155, 184, doi: 10.3847/1538-3881/aab49b

    2018 doi

  35. [43]

    2010, Reports on Progress in Physics, 73, 036801, doi: 10.1088/0034-4885/73/3/036801

    Greenberg, R. 2010, Reports on Progress in Physics, 73, 036801, doi: 10.1088/0034-4885/73/3/036801

    2010 doi

  36. [44]

    Nealson, K. H. 2009, Europa, 589

    2009

  37. [45]

    Harris, A. W. 1998, Icarus, 131, 291, doi: 10.1006/icar.1997.5865

    1998

  38. [46]

    A., & Porco, C

    Heppenheimer, T. A., & Porco, C. 1977, Icarus, 30, 385, doi: 10.1016/0019-1035(77)90173-7

    1977 doi

  39. [47]

    A., Jordan, J

    Hesse, M. A., Jordan, J. S., Vance, S. D., & Oza, A. V. 2022, Geophysical Research Letters, 49, e2021GL095416

    2022

  40. [48]

    M., Zolensky, M

    Hiroi, T., Pieters, C. M., Zolensky, M. E., & Lipschutz, M. E. 1993, Science, 261, 1016, doi: 10.1126/science.261.5124.1016

    1993

  41. [49]

    2022, Science Advances, 0, eadd8141, doi: 10.1126/sciadv.add8141

    Hopp, T., Dauphas, N., Abe, Y., et al. 2022, Science Advances, 0, eadd8141, doi: 10.1126/sciadv.add8141

    2022 doi

  42. [50]

    T., Benedix, G

    Howard, K. T., Benedix, G. K., Bland, P. A., & Cressey, G. 2011, GeoCoA, 75, 2735, doi: 10.1016/j.gca.2011.02.021

    2011 doi

  43. [51]

    S., Vilas, F., Larson, S

    Jarvis, K. S., Vilas, F., Larson, S. M., & Gaffey, M. J. 2000, Icarus, 145, 445, doi: 10.1006/icar.2000.6344

    2000

  44. [52]

    2007, ARA&A, 45, 261, doi: 10.1146/annurev.astro.44.051905.092459

    Jewitt, D., & Haghighipour, N. 2007, ARA&A, 45, 261, doi: 10.1146/annurev.astro.44.051905.092459

    2007 arXiv

  45. [53]

    2004, Jupiter: The planet, satellites and magnetosphere, 1, 485

    Johnson, R., Carlson, R., Cooper, J., et al. 2004, Jupiter: The planet, satellites and magnetosphere, 1, 485

    2004

  46. [54]

    Kelley, M. S. P., Hsieh, H. H., Bodewits, D., et al. 2023, Nature, 619, 720, doi: 10.1038/s41586-023-06152-y

    2023 doi

  47. [55]

    King, T. V. V., Clark, R. N., Calvin, W. M., Sherman, D. M., & Brown, R. H. 1992, Science, 255, 1551, doi: 10.1126/science.255.5051.1551

    1992

  48. [56]

    Kortenkamp, S. J. 2005, Icarus, 175, 409, doi: 10.1016/j.icarus.2004.11.020

    2005 doi

  49. [57]

    L., De Sanctis, M

    Kurokawa, H., Ehlmann, B. L., De Sanctis, M. C., et al. 2020, Journal of Geophysical Research (Planets), 125, e06606, doi: 10.1029/2020JE006606

    2020 doi

  50. [58]

    F., Morbidelli, A., Van Laerhoven, C., Gomes, R., & Tsiganis, K

    Levison, H. F., Morbidelli, A., Van Laerhoven, C., Gomes, R., & Tsiganis, K. 2008, Icarus, 196, 258, doi: 10.1016/j.icarus.2007.11.035

    2008 doi

  51. [59]

    J., et al

    Licandro, J., Pinilla-Alonso, N., Holler, B. J., et al. 2024, Nature Astronomy, doi: 10.1038/s41550-024-02417-2

    2024 doi

  52. [60]

    1993, Nature, 365, 819, doi: 10.1038/365819a0

    Malhotra, R. 1993, Nature, 365, 819, doi: 10.1038/365819a0

    1993 doi

  53. [61]

    J., Lin, H

    Markwardt, L., Holler, B. J., Lin, H. W., et al. 2023, arXiv e-prints, arXiv:2310.03998, doi: 10.48550/arXiv.2310.03998

    2023 doi arXiv

  54. [62]

    2022, AJ, 164, 167, doi: 10.3847/1538-3881/ac8d6b

    Marschall, R., Nesvorn´ y, D., Deienno, R., et al. 2022, AJ, 164, 167, doi: 10.3847/1538-3881/ac8d6b

    2022 doi

  55. [63]

    E., Binzel, R

    Marsset, M., DeMeo, F. E., Binzel, R. P., et al. 2020, ApJS, 247, 73, doi: 10.3847/1538-4365/ab7b5f

    2020 doi

  56. [64]

    K., Rocha, W

    McClure, M. K., Rocha, W. R. M., Pontoppidan, K. M., et al. 2023, Nature Astronomy, 7, 431, doi: 10.1038/s41550-022-01875-w

    2023 doi

  57. [65]

    a., Hansen, G., Clark, R

    McCord, T. a., Hansen, G., Clark, R. N., et al. 1998, Journal of Geophysical Research: Planets, 103, 8603

    1998

  58. [66]

    Y., Emery, J

    McSween, H. Y., Emery, J. P., Rivkin, A. S., et al. 2018, M&PS, 53, 1793, doi: 10.1111/maps.12947

    2018 doi

  59. [67]

    A., & Malhotra, R

    Minton, D. A., & Malhotra, R. 2009, Nature, 457, 1109, doi: 10.1038/nature07778

    2009 doi

  60. [68]

    2010, AJ, 140, 1391, doi: 10.1088/0004-6256/140/5/1391 Nesvorn´ y, D

    Tsiganis, K. 2010, AJ, 140, 1391, doi: 10.1088/0004-6256/140/5/1391 Nesvorn´ y, D. 2018, ARA&A, 56, 137, doi: 10.1146/annurev-astro-081817-052028 Nesvorn´ y, D., Dauphas, N., Vokrouhlick´ y, D., Deienno, R., & Hopp, T. 2024, Earth and Planetary Science Letters, 626, 118521, do...

    2010

  61. [69]

    Johnson, T. V. 2008, in The Solar System Beyond Neptune, ed. M. A. Barucci, H. Boehnhardt, D. P

    2008

  62. [70]

    E., Geballe, T

    Palumbo, M. E., Geballe, T. R., & Tielens, A. G. G. M. 1997, ApJ, 479, 839, doi: 10.1086/303905

    1997 doi

  63. [71]

    Pfalzner, S., Govind, A., & Wagner, F. W. 2024, ApJL, 972, L21, doi: 10.3847/2041-8213/ad63a6

    2024 doi

  64. [72]

    2021, Nature Astronomy, 6, 221, doi: 10.1038/s41550-021-01549-z

    Pilorget, C., Okada, T., Hamm, V., et al. 2021, Nature Astronomy, 6, 221, doi: 10.1038/s41550-021-01549-z

    2021 doi

  65. [73]

    N., et al

    Pinilla-Alonso, N., Brunetto, R., De Pr´ a, M. N., et al. 2024, Nature Astronomy, doi: 10.1038/s41550-024-02433-2

    2024 doi

  66. [74]

    2020, Science, 367, aaw7462, doi: 10.1126/science.aaw7462

    Poch, O., Istiqomah, I., Quirico, E., et al. 2020, Science, 367, aaw7462, doi: 10.1126/science.aaw7462

    2020 doi

  67. [75]

    B., Burns, J

    Pollack, J. B., Burns, J. A., & Tauber, M. E. 1979, Icarus, 37, 587, doi: 10.1016/0019-1035(79)90016-2

    1979 doi

  68. [76]

    C., West, R

    Porco, C. C., West, R. A., McEwen, A., et al. 2003, Science, 299, 1541, doi: 10.1126/science.1079462

    2003 doi

  69. [77]

    2020, Nature Astronomy, 4, 500, doi: 10.1038/s41550-019-0992-8

    Raponi, A., Ciarniello, M., Capaccioni, F., et al. 2020, Nature Astronomy, 4, 500, doi: 10.1038/s41550-019-0992-8

    2020 doi

  70. [78]

    Rauscher, B. J. 2024, PASP, 136, 015001, doi: 10.1088/1538-3873/ad1b36

    2024 doi

  71. [79]

    2006, Icarus, 185, 563

    Rivkin, A., Volquardsen, E., & Clark, B. 2006, Icarus, 185, 563

    2006

  72. [80]

    S., Emery, J

    Rivkin, A. S., Emery, J. P., Howell, E. S., et al. 2022, PSJ, 3, 153, doi: 10.3847/PSJ/ac7217

    2022 doi

  73. [81]

    S., Thomas, C

    Rivkin, A. S., Thomas, C. A., Wong, I., et al. 2025, PSJ, 6, 9, doi: 10.3847/PSJ/ad944c

    2025 doi

  74. [82]

    L., Bonev, B

    Saki, M., Gibb, E. L., Bonev, B. P., et al. 2020, AJ, 160, 184, doi: 10.3847/1538-3881/aba522

    2020 doi

  75. [83]

    L., Cloutis, E

    Schrader, D. L., Cloutis, E. A., Applin, D. M., et al. 2024, GeoCoA, 380, 48, doi: 10.1016/j.gca.2024.07.007

    2024 doi

  76. [84]

    Bottke, W. F. 2023, PSJ, 4, 223, doi: 10.3847/PSJ/ad0845

    2023 doi

  77. [85]

    Sharkey, B. N. L., Reddy, V., Sanchez, J. A., Izawa, M. R. M., & Emery, J. P. 2019, AJ, 158, 204, doi: 10.3847/1538-3881/ab46c0

    2019 doi

  78. [86]

    S., & Jewitt, D

    Sheppard, S. S., & Jewitt, D. C. 2003, Nature, 423, 261, doi: 10.1038/nature01584

    2003 doi

  79. [87]

    Trujillo, C. A. 2023, Research Notes of the American Astronomical Society, 7, 100, doi: 10.3847/2515-5172/acd766

    2023 doi

  80. [88]

    C., Holler, B

    Souza-Feliciano, A. C., Holler, B. J., Pinilla-Alonso, N., et al. 2024, A&A, 681, L17, doi: 10.1051/0004-6361/202348222

    2024 doi

  81. [89]

    J., Terada, H., Pyo, T.-S., & Kobayashi, N

    Takato, N., Bus, S. J., Terada, H., Pyo, T.-S., & Kobayashi, N. 2004, Science, 306, 2224, doi: 10.1126/science.1105427

    2004 doi

  82. [90]

    Takir, D., & Emery, J. P. 2012, Icarus, 219, 641, doi: 10.1016/j.icarus.2012.02.022

    2012 doi

  83. [91]

    P., McSween, H

    Takir, D., Emery, J. P., McSween, H. Y., et al. 2013, M&PS, 48, 1618, doi: 10.1111/maps.12171

    2013 doi

  84. [92]

    2019, Icarus, 333, 243, doi: 10.1016/j.icarus.2019.05.012

    Nakauchi, Y. 2019, Icarus, 333, 243, doi: 10.1016/j.icarus.2019.05.012

    2019 doi

  85. [93]

    N., Emery, J

    Takir, D., De Pra, M. N., Emery, J. P., et al. 2024, Low-Albedo and Inclination Asteroid Families as Tracers for Water and Organics in the Inner Solar System, JWST Proposal. Cycle 3, ID. #6384

    2024

  86. [94]

    2011, GeoCoA, 75, 6064, doi: 10.1016/j.gca.2011.07.038

    Tomeoka, K., & Ohnishi, I. 2011, GeoCoA, 75, 6064, doi: 10.1016/j.gca.2011.07.038

    2011 doi

  87. [95]

    K., & Brown, M

    Trumbo, S. K., & Brown, M. E. 2023, Science, 381, 1308

    2023

  88. [96]

    Tsiganis, K., Gomes, R., Morbidelli, A., & Levison, H. F. 2005, Nature, 435, 459, doi: 10.1038/nature03539

    2005 doi

  89. [97]

    G., Vuitton, V., Danger, G., et al

    Urso, R. G., Vuitton, V., Danger, G., et al. 2020, A&A, 644, A115, doi: 10.1051/0004-6361/202039528

    2020 doi

  90. [98]

    Vilas, F., & Hendrix, A. R. 2024, PSJ, 5, 34, doi: 10.3847/PSJ/ad150b

    2024 doi

  91. [99]

    Vilas, F., & Sykes, M. V. 1996, Icarus, 124, 483, doi: 10.1006/icar.1996.0224

    1996

  92. [100]

    2023, Science, 381, 1305

    Villanueva, G., Hammel, H., Milam, S., et al. 2023, Science, 381, 1305

    2023

  93. [101]

    J., Morbidelli, A., Raymond, S

    Walsh, K. J., Morbidelli, A., Raymond, S. N., O’Brien, D. P., & Mandell, A. M. 2011, Nature, 475, 206, doi: 10.1038/nature10201

    2011 doi

  94. [102]

    Noll, K. S. 2025, Probing the origin and interiors of Jupiter Trojans through the study of collisional fragments, JWST Proposal. Cycle 4, ID. #9078

    2025

  95. [103]

    Wong, I., & Brown, M. E. 2016, AJ, 152, 90, doi: 10.3847/0004-6256/152/4/90

    2016 doi

  96. [104]

    E., Emery, J

    Wong, I., Brown, M. E., Emery, J. P., et al. 2024, PSJ, 5, 87, doi: 10.3847/PSJ/ad2fc3

    2024 doi

  97. [105]

    A., Kurokawa, H., & Wu, Y

    Yu, J., Zhao, H., Cloutis, E. A., Kurokawa, H., & Wu, Y. 2024, Icarus, 411, 115951, doi: 10.1016/j.icarus.2024.115951

    2024

Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.