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arxiv: 2604.22931 · v1 · submitted 2026-04-24 · 🌌 astro-ph.EP

Recognition: unknown

Emerging Diversity Among the Main-Belt Comets: Insights from JWST and Ground-Based Observations of 457P/Lemmon-PANSTARRS

John W. Noonan , Henry H. Hsieh , Michael S. P. Kelley , Dennis Bodewits , Jana Pittichova , Audrey Thirouin , Marco Micheli , Scott S. Sheppard
show 5 more authors
Colin O. Chandler Theodore Kareta Colin Snodgrass Richard E. Cannon Brian P. Murphy
Authors on Pith no claims yet

Pith reviewed 2026-05-08 09:15 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords main-belt cometsdust activitygas production upper limitsJWST spectroscopyvolatile depletionperihelion observations5:2 resonance
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The pith

Main-belt comet 457P shows clear dust activity but no detectable water or other gases in JWST spectra.

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

The paper presents new JWST and ground-based data on main-belt comet 457P, which was active around its 2020 and 2024 perihelia. Imaging confirmed dust ejection over extended periods, yet spectroscopy placed tight upper limits on emissions from water, carbon monoxide, carbon dioxide, and methanol. This non-detection stands in contrast to the water production measured in two other main-belt comets observed with the same instrument. The result indicates that volatile content or the processes driving activity may differ among these objects, especially for those on orbits closer to the Sun. Mapping such differences across the main belt will clarify how ices survive and become active in this region.

Core claim

Despite unambiguous dust activity in both ground-based and JWST images, no H2O, CO, CO2, or CH3OH lines were detected, yielding an upper limit of Q(H2O) less than 2x10^24 molecules per second, equivalent to 0.035 kg/s. Because 457P lies inside the 5:2 mean-motion resonance with Jupiter, it is the first main-belt comet with a smaller semi-major axis to receive such sensitive gas searches. The authors conclude that 457P is likely more depleted in volatiles than the outer-belt objects 238P and 358P, whose dust-to-gas ratios had been used to predict detectable gas levels.

What carries the argument

Upper limits on molecular production rates derived from non-detections in NIRSpec spectra, compared against expected gas output scaled from dust activity using ratios measured in other main-belt comets.

If this is right

  • Activity in main-belt comets is not uniform and may vary with orbital distance from the Sun.
  • Some objects may sustain dust ejection with lower volatile content than previously assumed.
  • Surveys that combine imaging with spectroscopy across a range of semi-major axes will distinguish between a continuous spectrum and distinct subclasses.
  • Ice survival models for the asteroid belt must incorporate objects that produce little or no detectable gas.

Where Pith is reading between the lines

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

  • Dust activity in 457P could be driven by less volatile ices or by non-sublimation processes such as rotational ejection of surface material.
  • The diversity of main-belt comet behavior implies that their parent bodies experienced different thermal histories or formed at different distances.
  • Targeted observations of inner main-belt active asteroids could test whether low gas output is common inside the 5:2 resonance.

Load-bearing premise

That the dust seen in 457P is driven by the same water-ice sublimation process that powers activity in the previously observed main-belt comets, so that gas production can be reliably predicted from the observed dust.

What would settle it

Detection of water or other gas lines at production rates above 2x10^24 molecules per second during a future active phase would show that 457P is not depleted relative to the other main-belt comets.

Figures

Figures reproduced from arXiv: 2604.22931 by Audrey Thirouin, Brian P. Murphy, Colin O. Chandler, Colin Snodgrass, Dennis Bodewits, Henry H. Hsieh, Jana Pittichova, John W. Noonan, Marco Micheli, Michael S. P. Kelley, Richard E. Cannon, Scott S. Sheppard, Theodore Kareta.

Figure 1
Figure 1. Figure 1: Left: NIRSpec Extracted Spectrum from 1.8 to 5.2 microns for each of our four dithers, compared to our initial Planetary Spectrum Generator model estimate for a bare pV =0.05, T = 220 K, r = 560m, nucleus at our NIRSpec observing geometry to illustrate the weak dust contribution. Due to the poor signal in Dither 3 we exclude it from our median combined spectrum that is used for analysis. Note that the vari… view at source ↗
Figure 2
Figure 2. Figure 2: Median composite images of 457P/Lemmon-PANSTARRS, aligned on the photocenter of the comet in each individual image, constructed from NIRCam data obtained using the (a) F200W and (b) F277W broadband filters, comprising 1031 s of total exposure time each. Labeled arrows indicate the directions of celestial north (N) and east (E), and the projected anti-Sun (−⊙) and negative heliocentric velocity (−v) vectors… view at source ↗
Figure 3
Figure 3. Figure 3: Relative reflectance spectrum for 457P/Lemmon-PANSTARRS after dividing by a solar reference spectrum and a linear continuum to highlight broad absorption bands. The spectrum has been binned by a factor of 35 to highlight the 3 µm absorption band. Note that the slight upwards trend near 4µm is due to increased thermal contribution (see view at source ↗
Figure 4
Figure 4. Figure 4: Results from MCMC modeling of H2O, with black spectra showing a subset of the MCMC models, and the red line highlighting our 3σ upper limit model for 2.0×1024 molecules s−1 . for 457P from Y. Kim et al. (2022) would require an albedo of pV =∼ 0.1. If we use our photometry-derived rn = 0.56 km for 457P (see Section 4.2.1), and assuming that our spectral slope applies from V to our bandpass, we find that pV … view at source ↗
Figure 5
Figure 5. Figure 5: Upper limit fits to JWST NIRSpec data for 457P for CO, CO2, and CH3OH, with production rates reported in view at source ↗
Figure 6
Figure 6. Figure 6: (a) Phase function fit for 457P’s inactive nucleus using an assumed value of G = 0.18 ± 0.28. (b) Phase func￾tion fit for 457P’s inactive nucleus allowing both H and G to vary freely. In both panels, the gray shaded region shows the range of potential photometric variation for a nucleus with a rotational lightcurve amplitude of A = 0.25 mag view at source ↗
Figure 7
Figure 7. Figure 7: Plot of Af ρ as a function of photometry aperture radius (solid blue line) in terms of arcseconds projected on the sky (bottom x-axis labels) and km at the distance of the comet (top x-axis labels) as measured for a composite image of 133P constructed from data obtained on UT 2024 October 27 by Gemini South, with a ρ −0.6 power law (dashed black line) shown for reference. The seeing (θs) from view at source ↗
Figure 8
Figure 8. Figure 8: Plots of (a) equivalent total absolute V -band magnitude and (b) Af ρ measured for 457P as functions of true anomaly. In panel (a), the dashed horizontal line shows the absolute V -band magnitude of 457P’s inactive nucleus of HV = 18.69 mag determined in this work (Section 4.2.1), and the gray-shaded area bounded by horizontal dotted lines indicates the range of potential brightness variations allowed by t… view at source ↗
Figure 9
Figure 9. Figure 9: Contour plots (using 8 logarithmically spaced contour levels ranging from the peak value of each image — 5.9 MJy/sr for F200W and 1.4 MJy/sr for F277W — to the background level — ∼ 0.7 MJy/sr for F200W and ∼ 0.4 MJy/sr for F277W — for each image) of the inner coma of 457P constructed from (a) F200W and (b) F277W NIRCam median composite images obtained on UT 2024 September 20, shown in Figures 2a and 2b, re… view at source ↗
Figure 10
Figure 10. Figure 10: Computed synchrones (top) and syndynes (bottom) for the observing geometry of our NIRCam ob￾servations with the FOV of our NIRSpec IFU observations (3. ′′×3. ′′), detailed in view at source ↗
Figure 11
Figure 11. Figure 11: Terminal dust velocities for particles between ad = 0.1 µm and ad = 1 cm for various active area radii with a total QH2O ≤ 0.06 kg s−1 , as calculated for 457P during our observations using the small-source approximation from D. Jewitt et al. (2014). Note that this limitation on total pro￾duction rate reduces the number density of H2O for larger active areas, in turn reducing gas pressure and terminal ve￾… view at source ↗
Figure 12
Figure 12. Figure 12: Relative reflectance spectra for 457P/Lemmon-PANSTARRS, the average sharp-type (ST) non-sharp type (NST) spectra, Cybele (A. S. Rivkin et al. 2022), 67P/Churyumov-Gerasimenko (A. Raponi et al. 2020), (142) Polana (A. Arredondo et al. 2025), and (101955) Bennu from OVIRS (V. E. Hamilton et al. 2022). We note that the redward edge of the 3 µm contains complex absorption features, similar to Cybele, 67P, and… view at source ↗
read the original abstract

We present JWST NIRSpec and NIRCam observations of 457P/Lemmon-PANSTARRS, a main-belt comet that displayed activity around its 2020 perihelion and that was observed to regain activity during its 2024 perihelion by a ground-based observing campaign. The previous successful measurements of water production from two main-belt comets by the JWST NIRSpec instrument confirmed the hypothesis that H2O reservoirs are responsible for activity in dynamically stable main-belt comets. However, the main-belt comets observed with JWST thus far, 238P/Read and 358P/PANSTARRS, occupy orbits in the outer main-belt, with main-belt comets with smaller semi-major axes not yet sensitively tested for H2O. We find that despite clearly displaying dust activity in both ground-based and JWST imaging over a broad period, there were no corresponding H2O, CO, CO2, or CH3OH emissions within sensitive upper limits; notable given 457P is the first main-belt comet with a semi-major axis within the 5:2 mean-motion resonance with Jupiter. We show that we were sensitive to production rates of gas predicted by the dust/gas ratios of 238P and 358P, and hypothesize that 457P may be more depleted than its companions; Q(H2O) must be less than 2x10^24 molecules/s, or 0.035 kg/s. Further surveying of main-belt comets across the parameter space of semi-major axis and eccentricity will shed light on whether 457P represents an edge member of a spectrum or a distinct subclass of main-belt comets.

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 reports JWST NIRSpec and NIRCam observations of main-belt comet 457P/Lemmon-PANSTARRS, which showed dust activity in both JWST and ground-based imaging around its 2024 perihelion. No H2O, CO, CO2, or CH3OH emissions were detected despite the dust activity, yielding an upper limit Q(H2O) < 2×10^24 molecules/s (0.035 kg/s). The authors note that 457P is the first MBC with semi-major axis inside the 5:2 Jupiter resonance and hypothesize that it is more volatile-depleted than the previously JWST-observed MBCs 238P and 358P, based on the non-detection being sensitive to gas rates expected from their dust/gas ratios.

Significance. If the sensitivity claim holds, the work demonstrates diversity in volatile content among MBCs and provides the first sensitive gas constraint for an inner-main-belt object, with implications for formation locations and activity drivers. The direct non-detection plus quantitative upper limit is a clear observational result that can be tested with future observations across the semi-major-axis range.

major comments (2)
  1. Abstract: the assertion that the observations were sensitive to gas production rates 'predicted by the dust/gas ratios of 238P and 358P' is load-bearing for the depletion hypothesis, yet the text provides no quantitative dust metrics (Afρ, mass-loss rate, or coma brightness) for 457P nor a direct numerical comparison to the prior objects. Without these values the scaling cannot be verified and the non-detection does not yet demonstrate greater depletion.
  2. The derivation of the Q(H2O) < 2×10^24 molecules/s upper limit requires explicit statement of the assumed dust-to-gas ratio, the specific line sensitivities used, and the error analysis from the non-detection; these details are needed to assess whether the limit is robust against variations in activity level or mechanism.
minor comments (2)
  1. The abstract should state the semi-major axis of 457P numerically to allow immediate comparison with 238P and 358P.
  2. Clarify the exact epochs of the JWST and ground-based observations relative to perihelion and to each other.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review. We agree that the manuscript would benefit from greater quantitative transparency in the abstract and methods to support the sensitivity and depletion claims. We address each major comment below and have revised the manuscript accordingly.

read point-by-point responses

  1. Referee: Abstract: the assertion that the observations were sensitive to gas production rates 'predicted by the dust/gas ratios of 238P and 358P' is load-bearing for the depletion hypothesis, yet the text provides no quantitative dust metrics (Afρ, mass-loss rate, or coma brightness) for 457P nor a direct numerical comparison to the prior objects. Without these values the scaling cannot be verified and the non-detection does not yet demonstrate greater depletion.

    Authors: We acknowledge that the abstract as originally written did not include the specific numerical dust metrics needed for immediate verification of the scaling. The main text does report Afρ and mass-loss rate estimates for 457P from both ground-based and JWST data, along with comparisons to other MBCs, but we agree these should be summarized in the abstract for clarity. We have revised the abstract to include the measured Afρ value for 457P and a direct numerical comparison to the dust production levels of 238P and 358P, thereby allowing readers to confirm that the non-detection is sensitive to the gas rates expected from those ratios. revision: yes

  2. Referee: The derivation of the Q(H2O) < 2×10^24 molecules/s upper limit requires explicit statement of the assumed dust-to-gas ratio, the specific line sensitivities used, and the error analysis from the non-detection; these details are needed to assess whether the limit is robust against variations in activity level or mechanism.

    Authors: We agree that the original text did not provide a fully self-contained derivation of the upper limit. In the revised manuscript we have expanded the relevant methods and results sections to explicitly state the dust-to-gas ratio adopted for the sensitivity calculation, the specific NIRSpec line sensitivities and integration times used for H2O, CO, CO2, and CH3OH, and the statistical error analysis (including the 3-sigma threshold applied to the non-detection). We also include a brief discussion of how the limit remains robust under reasonable variations in activity level or dust-to-gas ratio. revision: yes

Circularity Check

0 steps flagged

No circularity: direct observational upper limits from non-detections

full rationale

The paper reports JWST and ground-based imaging plus spectroscopy of 457P showing dust activity but no detectable H2O, CO, CO2 or CH3OH lines, yielding a direct upper limit Q(H2O) < 2e24 molecules/s. The statement that observations were sensitive to gas rates 'predicted by the dust/gas ratios of 238P and 358P' uses external prior measurements only for context and sensitivity scaling; it does not reduce the upper-limit claim to any fitted parameter, self-definition, or equation within this work. No derivations, ansatzes, or uniqueness theorems appear. The result is self-contained empirical non-detection.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Observational astronomy paper; no free parameters, axioms, or invented entities are introduced. The result rests on standard data analysis and comparison to prior published dust/gas ratios.

pith-pipeline@v0.9.0 · 5687 in / 1167 out tokens · 61988 ms · 2026-05-08T09:15:07.240232+00:00 · methodology

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