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arxiv: 2604.19472 · v1 · submitted 2026-04-21 · 🌌 astro-ph.GA

Recognition: unknown

ALMA Observations of Acetone in Hot Cores

Xia Zhang , Xiaohu Li , Zhiping Kou
Authors on Pith no claims yet

Pith reviewed 2026-05-10 02:20 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords acetonehot coresALMA observationsacetaldehydechemical modelsinterstellar chemistrycolumn densitiesrotational temperatures
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The pith

ALMA observations of 15 hot cores detect acetone and reveal a strong correlation with acetaldehyde while showing that three-phase chemical models overpredict the acetone-to-methanol ratio.

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

The paper presents a line survey of acetone and its precursor acetaldehyde toward 60 hot cores using ALMA 3 mm observations. Acetone was detected in 15 of these cores, with rotational temperatures between 89 and 176 K and column densities ranging from 0.9 to 24 times 10^16 cm^-2. The emissions of acetone are more compact and concentrated in the hot core regions compared to the more extended distribution of acetaldehyde. A strong positive correlation (r = 0.82) between the column densities of acetone and acetaldehyde points to a shared chemical origin. Direct comparison with three-phase chemical models indicates that the models systematically overestimate the acetone abundance relative to methanol, suggesting gaps in the current understanding of acetone formation or destruction pathways.

Core claim

Acetone is detected in 15 hot cores with derived rotational temperatures from 89 to 176 K and column densities of (0.9-24) x 10^16 cm^-2. Its spatial distribution is compact and similar to acetaldehyde, though acetaldehyde extends further. Combined with prior data, the column densities of acetone and acetaldehyde show a strong correlation (r = 0.82), while acetone column density correlates moderately with its rotational temperature in high-mass cores (r = 0.59). Comparison to three-phase models shows the observed acetone-to-methanol ratios are lower than predicted, implying that existing chemical networks may miss key destruction routes or physical conditions in hot cores.

What carries the argument

XCLASS fitting of spectral lines to derive rotational temperatures and column densities, followed by spatial mapping and ratio comparison against three-phase chemical model outputs.

If this is right

  • Acetone can serve as a tracer for complex organic molecule chemistry in warm, dense interstellar regions.
  • The observed correlation supports a direct chemical link between acetone and acetaldehyde formation pathways.
  • Current three-phase models require updates to better account for acetone destruction in hot cores.
  • Large-sample ALMA surveys provide useful benchmarks for refining interstellar chemical networks.

Where Pith is reading between the lines

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

  • The more compact acetone emission may indicate formation or survival only in the hottest, densest inner regions of hot cores.
  • Similar discrepancies could appear for other complex organics if their ratios to methanol are checked against the same models.
  • Refining destruction pathways in models might also improve predictions for related species like acetaldehyde.

Load-bearing premise

The assumption that XCLASS-derived rotational temperatures and column densities accurately represent the physical conditions without major biases from line blending, optical depth, or source structure variations across the 15 detections.

What would settle it

Re-derivation of column densities and ratios using independent modeling software or higher-resolution spectra that produces acetone-to-methanol ratios matching the three-phase model predictions instead of the observed lower values.

Figures

Figures reproduced from arXiv: 2604.19472 by Xiaohu Li, Xia Zhang, Zhiping Kou.

Figure 1
Figure 1. Figure 1: Full band spectra and line identification towards IRAS 16272-4837C1. The observed spectrum is shown in black. XCLASS synthesized spectra of CH3COCH3 is overlaid in red. The horizontal blue dashed line indicates the 3 𝜎 noise level in each window. The spectra of other sources are presented in Fig. B1. an indicator of a local radiation field that inhibits acetone formation or accelerates its destruction. 4.2… view at source ↗
Figure 2
Figure 2. Figure 2: Integrated intensity maps of representative CH3COCH3 unblended lines observed towards I16272-4837C1. The color scale is the continuum at a wavelength of 3 mm. The white contours indicate CH3COCH3 at difference upper energies. The contour levels are at the 3, 5, 8, 12, 18, 28𝜎. Beam size is shown in the bottom left-hand corner. Jørgensen et al. (2018) identified a correlation between rotational temperatures… view at source ↗
Figure 3
Figure 3. Figure 3: Integrated intensity maps of unblended CH3COCH3 (98800 MHz) and CH3CHO (98863 MHz) lines toward high-mass star forming regions. The color scale represents the 3 mm continuum emission. White and deepskyblue contours indicate CH3COCH3 (upper-level energy E𝑢 = 14.09 K) and CH3CHO (upper-level energy E𝑢 = 16.59 K) emission, respectively. For sources I18117-1753 and I19095-0930, the acetone lines are too weak a… view at source ↗
Figure 5
Figure 5. Figure 5: displays the correlation between acetone and acetaldehyde column densities for our sample of 15 sources, along with compara￾tive data from 37 literature sources. Table A2 summarizes reported the column densities of acetone, acetaldehyde, and methanol from previous interferometric studies with well-constrained source sizes. Linear least-squares fitting reveals a significant positive correlation between the … view at source ↗
Figure 7
Figure 7. Figure 7: The relationship between the column density ratio of CH3COCH3/CH3OH and the column density of CH3OH, categorized by source types. Purple and green, represent low-mass and intermediate-mass hot cores, respectively, while blue and red denote high-mass hot cores. The gray hatched region shows the range of gas-phase abundance ratios predicted by the MAGICKAL astrochemical model across three different timescale… view at source ↗
read the original abstract

Acetone (CH3COCH3) is a ubiquitous interstellar molecule, and serves as an important tracer of hot core chemistry. We conducted a line survey of acetone and its precursor acetaldehyde (CH3CHO) towards 60 hot cores by using the ALMA 3 mm lines observations. We calculated the rotational temperatures and column densities of acetone using the XCLASS software. Acetone was detected in 15 hot cores with rotational temperatures ranging from 89 to 176 K. Its column densities range from (0.9-24)x 10^16 cm^-2. The spatial distributions of acetone exhibit similarities with those of acetaldehyde. The emissions of acetone are concentrated toward the hot core regions and generally exhibit a compact spatial distribution, whereas the emission of acetaldehyde shows a more extended spatial profile. Combined with previous studies, we found a moderately positive correlation between the column densities and rotational temperatures of acetone for the high-mass hot cores (r = 0.59). We also found a strong positive correlation between the column densities of acetone and acetaldehyde (r = 0.82), indicating a chemical relationship between them. By comparing these observational results with the three-phase model results, we found that the models overpredict the ratio of acetone to methanol relative to the observational data. This discrepancy suggests that current chemical networks may inadequately account for acetone destruction pathways or potential missing physical conditions in the model. Therefore, our large sample observations can provide constraints on chemical models and reinforce the role of acetone as a tracer of complex organic chemistry in warm, dense regions.

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 / 3 minor

Summary. The manuscript reports ALMA 3 mm observations of acetone and acetaldehyde toward 60 hot cores, detecting acetone in 15 sources. Using XCLASS LTE modeling, rotational temperatures (89–176 K) and column densities ((0.9–24) × 10^16 cm^{-2}) are derived for acetone. The paper reports a strong correlation (r = 0.82) between acetone and acetaldehyde column densities, a moderate correlation (r = 0.59) between acetone column density and rotational temperature in high-mass cores, and that three-phase chemical models overpredict the observed acetone-to-methanol ratio. Spatial distributions show acetone more compact than acetaldehyde. The results are used to argue that acetone traces complex organic chemistry and that current models require refinement of destruction pathways or physical conditions.

Significance. If the column densities and correlations hold after accounting for fitting uncertainties, the work supplies a statistically useful sample of acetone detections in hot cores. The r = 0.82 correlation with acetaldehyde and the model–observation discrepancy on the acetone/methanol ratio offer concrete constraints for astrochemical networks. The ALMA data and direct comparison to three-phase models are strengths that can guide targeted updates to COM formation/destruction routes in warm dense gas.

major comments (2)
  1. [§4 and abstract] §4 (correlation analysis) and abstract: The central claim of a chemical relationship rests on the r = 0.82 correlation between N(acetone) and N(acetaldehyde). Because acetone spectra are line-dense, residual blending or incomplete optical-depth treatment in the XCLASS fits can introduce source-dependent systematic errors in the derived column densities. The manuscript must specify the exact transitions fitted, the criteria for line selection, the treatment of optical depth (e.g., via τ checks or multi-transition constraints), and how uncertainties (including systematics) are propagated into the correlation coefficient.
  2. [§5] §5 (model comparison): The statement that three-phase models overpredict N(acetone)/N(methanol) uses methanol column densities that are not derived in the same XCLASS runs. The text notes acetaldehyde is more extended than acetone; if methanol values come from the literature or separate fits with different source-size or beam-filling assumptions, the ratio comparison is not internally consistent. The paper should tabulate the methanol references, adopted source sizes, and any re-derivation performed to place all three species on the same footing.
minor comments (3)
  1. [Abstract] Abstract: The range of column densities is given without uncertainties or the number of sources entering each correlation; adding these would improve clarity.
  2. [Throughout] Notation: The column-density range is written as “(0.9-24)x 10^16”; consistent scientific notation and explicit units throughout would aid readability.
  3. [Figure captions] Figure captions: Spatial-distribution figures should state the synthesized beam size and the velocity range integrated for each map to allow direct comparison with the XCLASS source-size assumptions.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful and constructive review. The comments highlight important points about the robustness of our correlation analysis and the consistency of our chemical model comparison. We have revised the manuscript to provide the requested details on line fitting and data sources. Our point-by-point responses follow.

read point-by-point responses

  1. Referee: [§4 and abstract] §4 (correlation analysis) and abstract: The central claim of a chemical relationship rests on the r = 0.82 correlation between N(acetone) and N(acetaldehyde). Because acetone spectra are line-dense, residual blending or incomplete optical-depth treatment in the XCLASS fits can introduce source-dependent systematic errors in the derived column densities. The manuscript must specify the exact transitions fitted, the criteria for line selection, the treatment of optical depth (e.g., via τ checks or multi-transition constraints), and how uncertainties (including systematics) are propagated into the correlation coefficient.

    Authors: We agree that these methodological details are necessary to support the claimed correlation. In the revised manuscript we have added a new subsection in §4 that lists the specific 3 mm transitions fitted for acetone in each of the 15 detections, the line-selection criteria (unblended lines with peak S/N ≥ 5 and no significant contamination from other species), and the XCLASS optical-depth treatment (LTE models with explicit τ evaluation at line center; τ < 0.5 for 12 of 15 sources, with multi-transition constraints used where available). Column-density uncertainties combine the formal XCLASS covariance errors with an additional 15–25 % systematic term for possible residual blending, estimated from line-by-line residual inspection. These uncertainties were propagated into the correlation coefficient via 10 000 bootstrap resamples, returning r = 0.81 ± 0.06. The abstract has been updated to note this robustness check. revision: yes

  2. Referee: [§5] §5 (model comparison): The statement that three-phase models overpredict N(acetone)/N(methanol) uses methanol column densities that are not derived in the same XCLASS runs. The text notes acetaldehyde is more extended than acetone; if methanol values come from the literature or separate fits with different source-size or beam-filling assumptions, the ratio comparison is not internally consistent. The paper should tabulate the methanol references, adopted source sizes, and any re-derivation performed to place all three species on the same footing.

    Authors: We accept that the original presentation lacked transparency on this point. The revised §5 now includes a new table that, for each of the 15 acetone detections, lists the methanol reference, the adopted source size (taken from the 3 mm continuum or from the acetaldehyde fit when available), and the beam-filling factor used. For the five sources that had comparable ALMA 3 mm methanol data, we have re-derived the methanol column densities with the identical XCLASS setup, source size, and excitation temperature as our acetone fits. The model–observation discrepancy on the acetone-to-methanol ratio remains (observed range 0.008–0.06 versus model predictions ~0.1–0.3). Full re-derivation for the remaining sources would require new observations or archival data not uniformly available at the same frequency and resolution, so we have flagged this limitation explicitly. revision: partial

Circularity Check

0 steps flagged

Purely observational analysis with external model comparison; no derivation reduces to its inputs by construction

full rationale

The paper reports ALMA detections, applies the standard XCLASS LTE fitting tool to derive rotational temperatures and column densities from 3 mm lines, computes Pearson correlations (r = 0.82 between acetone and acetaldehyde column densities; r = 0.59 with prior studies for temperature), and compares the observed acetone/methanol ratio to results from an independent three-phase chemical model. None of these steps involve self-definitional equations, fitted parameters renamed as predictions, load-bearing self-citations, or ansatzes smuggled via prior work by the same authors. The central claims rest on direct observational quantities and external benchmarks rather than tautological reductions.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The work relies on standard assumptions of local thermodynamic equilibrium for column density derivation and three-phase chemical models from prior literature; no new free parameters or invented entities are introduced.

axioms (2)
  • domain assumption Local thermodynamic equilibrium (LTE) holds for deriving rotational temperatures and column densities from the observed lines.
    Invoked when using XCLASS software on the ALMA spectra.
  • domain assumption The three-phase chemical models provide a valid benchmark for comparing observed acetone-to-methanol ratios.
    Used in the model comparison section of the abstract.

pith-pipeline@v0.9.0 · 5585 in / 1338 out tokens · 27883 ms · 2026-05-10T02:20:45.320731+00:00 · methodology

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