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arxiv: 1907.07791 · v1 · pith:MGXQ3SVCnew · submitted 2019-07-17 · 🌌 astro-ph.SR · astro-ph.GA

Organic complexity in protostellar disk candidates

Jennifer B. Bergner , Rafael Martin-Domenech , Karin I. Oberg , Jes K. Jorgensen , Elizabeth Artur de la Villarmois , Christian Brinch This is my paper

Pith reviewed 2026-05-24 19:49 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA
keywords hot corinoscomplex organic moleculesprotostellar disksALMA observationsSerpens clustermethanolchemical diversityClass 0/I protostars
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The pith

Hot corino chemistry appears in three of five protostellar disk candidates.

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

The paper reports ALMA observations of five low-mass Class 0/I protostellar disk candidates in the Serpens cluster. Three sources show emission from CH3OH along with CH3OCH3, CH3OCHO, and CH2CO, while two also show NH2CHO. This detection rate is presented as high relative to the known population of hot corinos. The results are used to argue for a possible connection between the structural conditions that form disks and those that produce hot corino chemistry. Column densities of 10^17 to 10^18 cm^{-2} and temperatures of 200-250 K are derived where methanol is seen, and the ratios of other oxygen-bearing molecules vary by two orders of magnitude across sources.

Core claim

Detecting hot corino-type chemistry in three of five sources represents a high occurrence rate given the relative sparsity of these sources in the literature, and this suggests a possible link between protostellar disk formation and hot corino formation. For sources with CH3OH detections, column densities of 10^{17}-10^{18} cm^{-2} and rotational temperatures of ~200-250 K are found. The CH3OH-normalized column density ratios of large, oxygen-bearing COMs in the Serpens sources and other hot corinos span two orders of magnitude, demonstrating a high degree of chemical diversity at the hot corino stage.

What carries the argument

ALMA line observations of CH3OH and other complex organic molecules used to classify sources as hot corinos and measure their column densities and temperatures.

If this is right

  • Hot corino chemistry may commonly accompany the formation of protostellar disks.
  • Chemical diversity among hot corinos is already large at the Class 0/I stage.
  • Resolved imaging of more objects is required to trace how different structural elements on disk scales produce this diversity.

Where Pith is reading between the lines

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

  • If the link holds, the organic inventory delivered to forming planets could be set early during the disk-assembly phase.
  • Differences in detection might trace variations in envelope mass, inclination, or evolutionary timing rather than absence of the chemistry.
  • Repeating the survey in other clusters would test whether the occurrence rate is universal or specific to the Serpens environment.

Load-bearing premise

The five chosen sources form an unbiased sample of low-mass Class 0/I disk candidates and the two non-detections are not caused by insufficient sensitivity or source-specific effects.

What would settle it

A uniform-sensitivity survey of a larger set of Class 0/I disk candidates that finds a substantially lower fraction with hot corino chemistry would falsify the claimed high occurrence rate.

Figures

Figures reproduced from arXiv: 1907.07791 by Christian Brinch, Elizabeth Artur de la Villarmois, Jennifer B. Bergner, Jes K. Jorgensen, Karin I. Oberg, Rafael Martin-Domenech.

Figure 1
Figure 1. Figure 1: Source overview showing the 1.3 mm dust continuum emission (top), C18O 2–1 line emission (middle), and CH3OH 51,4 – 41,3 line emission (bottom). Continuum contours are drawn at 5, 30, 100, 400×rms, and line contours are drawn at 5, 10, 30×rms. Color scales are normalized to each individual image, and emission below a 2×rms threshold is not shown. The synthesized beam is shown in the bottom left of each pan… view at source ↗
Figure 2
Figure 2. Figure 2: Moment zero maps of organic molecule lines in Ser-emb 1, Ser-emb 8, and Ser-emb 17. Contours are drawn at 5, 10, 20, 30×rms. Color scales are normalized to each individual image, and emission below a 2×rms threshold is not shown. The synthesized beam is shown in the bottom left of each panel. Velocity ranges and rms values for each panel can be found in Appendix A. Velocity-integrated intensities are measu… view at source ↗
Figure 3
Figure 3. Figure 3: CH3OH spectral lines in sources where CH3OH is detected. Blue lines show the spectra extracted from the continuum peak pixel, and shaded regions represent the rms. Red lines show Gaussian fits to the data; a dotted line in￾dicates that the feature is not significant above a 3σ level. Cτ is the optical depth correction factor and Ωa Ωs is the beam dilution factor, where Ωs and Ωa are the source and beam sol… view at source ↗
Figure 4
Figure 4. Figure 4: CH3OH population diagrams for Ser-emb 1, Ser-emb 8, and Ser-emb 17. Data and uncertainties are shown in black, and draws from the fit posteriors are shown in blue. Molecule Line Ser-emb 1 Ser-emb 8 Ser-emb 17 Int. intensity Beam dim. Int. intensity Beam dim. Int. intensity Beam dim. (mJy beam−1 (”) (mJy beam−1 (”) (mJy beam−1 (”) km s−1 ) km s−1 ) km s−1 ) CH3OH 51,4 127 ± 15 0.54 × 0.45 325 ± 34 0.55 × 0.… view at source ↗
Figure 5
Figure 5. Figure 5: Full spectrum extracted from the continuum peak pixel in Ser-emb 17 (grey line), along with synthetic spectra of the COMs studied in this work (colored lines) assuming the CH3OH rotational temperature [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Examples of spectra with line profiles suggestive of rotation (a, b), infall (b, c, d), and outflows (e). For clarity, only upper state quantum numbers are used to identify each line; refer to [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Comparison of organic molecule column density ratios with respect to methanol at different evolutionary stages. The Ser-emb sources are shown as blue squares. Column densities are derived for the continuum peak position, assuming the CH3OH rotational temperature TM; error bars show the column densities derived for TM ±75 K. Measured abundances in the cold outer envelopes of Class 0/I low-mass protostars ar… view at source ↗
Figure 8
Figure 8. Figure 8: Ser-emb 1 rotational diagram MCMC fit results. The corner plot is shown on the left and the walker chain on the right [PITH_FULL_IMAGE:figures/full_fig_p015_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Ser-emb 8 rotational diagram MCMC fit results. The corner plot is shown on the left and the walker chain on the right [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Ser-emb 17 rotational diagram MCMC fit results. The corner plot is shown on the left and the walker chain on the right. C. SPECTRAL LINE FITS Figures 11–14 show Gaussian fits to the observed lines of each COM, analogous to [PITH_FULL_IMAGE:figures/full_fig_p016_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: CH3OCH3 spectral lines. Blue lines show the spectra extracted from the continuum peak pixel, and shaded regions represent the rms. Red lines show Gaussian fits to the data [PITH_FULL_IMAGE:figures/full_fig_p016_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: CH3OCHO spectral lines. Blue lines show the spectra extracted from the continuum peak pixel, and shaded regions represent the rms. Red lines show Gaussian fits to the data [PITH_FULL_IMAGE:figures/full_fig_p017_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: NH2CHO spectral lines. Blue lines show the spectra extracted from the continuum peak pixel, and shaded regions represent the rms. Red lines show Gaussian fits to the data [PITH_FULL_IMAGE:figures/full_fig_p017_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: CH2CO spectra lines. Blue lines show the spectra extracted from the continuum peak pixel, and shaded regions represent the rms. Red lines show Gaussian fits to the data [PITH_FULL_IMAGE:figures/full_fig_p017_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Full spectrum extracted from the continuum peak pixel in Ser-emb 1 (grey line), along with synthetic spectra of the detected COMs (colored lines). Spectra are calculated assuming the CH3OH rotational temperature [PITH_FULL_IMAGE:figures/full_fig_p019_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Full spectrum extracted from the continuum peak pixel in Ser-emb 7 (grey line) [PITH_FULL_IMAGE:figures/full_fig_p020_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Full spectrum extracted from the continuum peak pixel in Ser-emb 8 (grey line), along with synthetic spectra of the detected COMs (colored lines). Spectra are calculated assuming the CH3OH rotational temperature [PITH_FULL_IMAGE:figures/full_fig_p021_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: Full spectrum extracted from the continuum peak pixel in Ser-emb 15 (grey line) [PITH_FULL_IMAGE:figures/full_fig_p022_18.png] view at source ↗
read the original abstract

We present ALMA observations of organic molecules towards five low-mass Class 0/I protostellar disk candidates in the Serpens cluster. Three sources (Ser-emb 1, Ser-emb 8, and Ser-emb 17) present emission of CH3OH as well as CH3OCH3, CH3OCHO, and CH2CO, while NH2CHO is detected in just Ser-emb 8 and Ser-emb 17. Detecting hot corino-type chemistry in three of five sources represents a high occurrence rate given the relative sparsity of these sources in the literature, and this suggests a possible link between protostellar disk formation and hot corino formation. For sources with CH3OH detections, we derive column densities of 10^{17}-10^{18} cm^{-2} and rotational temperatures of ~200-250 K. The CH3OH-normalized column density ratios of large, oxygen-bearing COMs in the Serpens sources and other hot corinos span two orders of magnitude, demonstrating a high degree of chemical diversity at the hot corino stage. Resolved observations of a larger sample of objects are needed to understand the origins of chemical diversity in hot corinos, and the relationship between different protostellar structural elements on disk-forming scales.

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

3 major / 1 minor

Summary. The manuscript presents ALMA observations of five low-mass Class 0/I protostellar disk candidates in the Serpens cluster. Detections of CH3OH along with CH3OCH3, CH3OCHO, and CH2CO are reported in three sources (Ser-emb 1, Ser-emb 8, Ser-emb 17), with NH2CHO in two of those; column densities of 10^{17}-10^{18} cm^{-2} and rotational temperatures of ~200-250 K are derived for CH3OH in the detected sources via LTE fits. The authors interpret the 3/5 detection rate as evidence of a high occurrence of hot corino chemistry, suggesting a possible link to protostellar disk formation, and note that CH3OH-normalized COM ratios across hot corinos span two orders of magnitude, indicating chemical diversity.

Significance. If the sample is representative and non-detections are chemically meaningful, the reported occurrence rate would indicate that hot corino chemistry is more common among Class 0/I disk candidates than the sparse existing literature suggests, strengthening the connection between disk formation and complex organic chemistry. The observed diversity in COM ratios would also motivate larger surveys to trace chemical evolution on disk-forming scales.

major comments (3)
  1. [Abstract] Abstract: The central claim that the 3/5 detection rate 'represents a high occurrence rate' and suggests a link to disk formation rests on the five sources forming an unbiased sample of disk candidates and the two non-detections reflecting chemical absence rather than sensitivity limits. No selection criteria, rms noise levels, or 3σ upper limits on CH3OH or other COMs are provided for the non-detections, leaving open the possibility that the rate is sensitivity-limited.
  2. [Abstract] Abstract: Column densities (~10^{17}-10^{18} cm^{-2}) and temperatures (~200-250 K) are reported only for detections, with no error bars, details on the LTE modeling (e.g., assumed source size, partition functions), baseline subtraction, or explicit checks against line misidentification or blending.
  3. [Abstract] Abstract: The statement that COM ratios 'span two orders of magnitude' demonstrating 'high degree of chemical diversity' is presented without a table or specific normalized values for the Serpens sources versus literature hot corinos, making the quantitative claim difficult to evaluate.
minor comments (1)
  1. [Abstract] The abstract refers to 'resolved observations of a larger sample' without clarifying whether this means spatially resolved data or simply a larger number of sources.

Simulated Author's Rebuttal

3 responses · 0 unresolved

Thank you for the opportunity to respond to the referee's report. We find the comments helpful and will revise the manuscript to address the concerns raised about the abstract. Below we respond point by point to the major comments.

read point-by-point responses

  1. Referee: The central claim that the 3/5 detection rate 'represents a high occurrence rate' and suggests a link to disk formation rests on the five sources forming an unbiased sample of disk candidates and the two non-detections reflecting chemical absence rather than sensitivity limits. No selection criteria, rms noise levels, or 3σ upper limits on CH3OH or other COMs are provided for the non-detections, leaving open the possibility that the rate is sensitivity-limited.

    Authors: We agree that the abstract would benefit from including these supporting details to allow readers to evaluate the detection rate. The manuscript describes the sample selection in Section 2 as the Class 0/I sources in Serpens with available high-resolution ALMA observations. In the revision, we will add the selection criteria, rms noise levels from the observations, and 3σ upper limits for CH3OH in the two non-detected sources to the abstract and/or a new table. This will enable assessment of whether the non-detections are due to sensitivity. revision: yes

  2. Referee: Column densities (~10^{17}-10^{18} cm^{-2}) and temperatures (~200-250 K) are reported only for detections, with no error bars, details on the LTE modeling (e.g., assumed source size, partition functions), baseline subtraction, or explicit checks against line misidentification or blending.

    Authors: The full details of the LTE modeling, including source size assumptions, partition functions, baseline subtraction procedures, and line identification checks, are provided in Section 3 of the manuscript. However, we acknowledge that the abstract is missing error bars and a brief mention of the modeling. In the revised version, we will include error bars on the column densities and temperatures, and add a concise description of the LTE approach to the abstract. revision: yes

  3. Referee: The statement that COM ratios 'span two orders of magnitude' demonstrating 'high degree of chemical diversity' is presented without a table or specific normalized values for the Serpens sources versus literature hot corinos, making the quantitative claim difficult to evaluate.

    Authors: We will revise the manuscript to include a table (Table X) that lists the specific CH3OH-normalized COM ratios for the three Serpens sources and compares them to values from the literature hot corinos. This table will be referenced in the abstract to support the claim that the ratios span two orders of magnitude, thereby demonstrating the chemical diversity. revision: yes

Circularity Check

0 steps flagged

No significant circularity in observational analysis

full rationale

The paper reports direct ALMA observations of organic molecules in five Serpens Class 0/I sources, with detections of CH3OH and other COMs in three sources. Column densities (10^{17}-10^{18} cm^{-2}) and rotational temperatures (~200-250 K) are derived from spectral line data using standard methods for the detected sources only. The occurrence-rate statement is simply the observed fraction (3/5) compared to literature sparsity, with no models, fitted parameters renamed as predictions, self-definitional loops, or load-bearing self-citations. No derivation chain reduces to its inputs by construction; results are empirical and self-contained.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Results rest on standard LTE assumptions for line excitation and the literature definition of hot corinos; column densities and temperatures are fitted parameters.

free parameters (2)
  • CH3OH column density = 10^17-10^18 cm^{-2}
    Fitted from observed line intensities under LTE assumption
  • rotational temperature = 200-250 K
    Fitted from multiple CH3OH transitions
axioms (2)
  • domain assumption Local thermodynamic equilibrium governs level populations in the emitting gas
    Standard assumption invoked when deriving column densities from molecular line data in dense protostellar environments
  • domain assumption Presence of CH3OH plus larger O-bearing COMs at ~200 K defines hot corino chemistry
    Definition drawn from prior literature and used to classify the three sources

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