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arxiv: 2606.00212 · v1 · pith:H755S7ZWnew · submitted 2026-05-29 · 🌌 astro-ph.GA · astro-ph.EP· astro-ph.SR

Subarcsecond Multi-line Observations of NH₃ with VLA toward the Class 0 Source IRAS 16293-2422

Yoshihide Yamato , Yuri Aikawa , Kenji Furuya , John J. Tobin , Jes K. J{\o}rgensen This is my paper

Pith reviewed 2026-06-28 21:41 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.EPastro-ph.SR
keywords ammoniaprotostarsVLA observationsmolecular linesClass 0 sourcesIRAS 16293-2422star formation chemistry
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The pith

High-energy ammonia lines trace 200-300 K gas near the protostars in IRAS 16293-2422.

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

The paper reports subarcsecond VLA observations of 17 NH3 inversion transitions spanning upper-state energies from 23 K to 1580 K toward the Class 0 binary system IRAS 16293-2422. High-energy lines appear compact near the protostars while low-energy lines are more extended, and a two-component model yields rotation temperatures of 200-300 K for the warmer gas. The authors attribute the hot component in source A to local shock heating and that in source B to mass accretion heating, based on spatial comparisons with prior ALMA data.

Core claim

Multi-transition NH3 observations at ~0.5 arcsecond resolution show that lines with upper-state energies above 1000 K selectively trace compact, warm gas with rotation temperatures of 200-300 K around each protostar. A two-component fit separates this inner hot gas from cooler extended material, and comparison with ALMA images indicates shock heating dominates in source A while accretion heating explains the hot gas in source B.

What carries the argument

Two-component rotation diagram model fitted to the intensities of the 17 NH3 lines to derive separate temperatures and column densities for warm inner and cool outer components.

If this is right

  • High-Eu NH3 lines serve as selective tracers of the innermost hot envelopes around other Class 0 sources.
  • Binary protostars can exhibit distinct heating processes in each component despite similar overall conditions.
  • Abundance ratios of NH3 to other ice-derived molecules constrain desorption and gas-phase chemistry in hot regions.

Where Pith is reading between the lines

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

  • The contrast between shock and accretion heating may reflect differences in outflow activity or disk accretion rates between the two sources.
  • Similar multi-line observations in other binaries could test whether shock heating correlates with observed outflow asymmetries.
  • The derived temperatures suggest that NH3 survives or reforms in regions hot enough to sublimate water ice.

Load-bearing premise

The two-component model captures the excitation conditions without significant optical depth effects or contributions from non-LTE processes.

What would settle it

If high-energy NH3 lines showed strong optical depth or if their locations failed to align with shock features seen in ALMA data, the attribution of heating mechanisms would not hold.

Figures

Figures reproduced from arXiv: 2606.00212 by Jes K. J{\o}rgensen, John J. Tobin, Kenji Furuya, Yoshihide Yamato, Yuri Aikawa.

Figure 1
Figure 1. Figure 1: shows the 1.2 cm continuum image of IRAS 16293-2422. Two emission components associated with source A and B are clearly resolved. While source B appears as compact, source A is highly structured with four possible emission components, whose overall morphology is consis￾tent with the previous VLA observations (e.g., A. Hernandez- ´ Gomez et al. ´ 2019). To characterize the properties of the continuum emissi… view at source ↗
Figure 2
Figure 2. Figure 2: Spectra of the observed NH3 transitions at the source positions of source A (bottom) and source B (top). The vertical red dotted line marks the approximate systemic velocity of the source (3 km s−1 ). Note that the blue-shifted side of the NH3 (5,4) lines are out of the spectral window coverage [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Stacked spectra of NH3 transitions with Eu > 1, 000 K in source A (left) and source B (right) that demonstrate the robust detection of high-excitation lines. The intensity scale is normalized by the noise levels of each spectrum. The vertical red dotted line marks the systemic velocity of each source. (R. Teague & D. Foreman-Mackey 2018) with no intensity threshold for pixel inclusion. The velocity ranges … view at source ↗
Figure 4
Figure 4. Figure 4: 1.2 cm continuum image (top left) and velocity-integrated intensity maps of observed NH3 transitions (others) toward source A. Only pixels with values greater than 3σ are shown, where σ is the rms value measured on the emission-free region of each map. The contours on each panel start from 3σ followed by a 1σ step. The red crosses indicate the positions of the protostars A1 and A2. B, we consider that the … view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Stacked velocity-integrated intensity maps (left) for each set of “warm” lines (Eu < 150 K) and “hot” lines (Eu > 1000 K), and their normalized spatial profiles along P.A. = 90. ◦0 (along the Right Ascension or beam minor axis; right). Beam size of the stacked maps and the scale bar of 50 au are indicated at the lower left and lower right of each map, respectively. The contours start from 3σ followed by 1σ… view at source ↗
Figure 8
Figure 8. Figure 8: Stacked spectrum of NH3 (5,1), (7,7) (6,3), (6,2), (8,6), and (9,7) lines toward source B, which shows a blue-skewed line profile. source B, where we derive an intermediate value of rotation temperature (∼ 200 K) and a column density consistent with the sum of those of the two components (Appendix C). 5. DISCUSSION 5.1. Comparison with the Previous Observations Here we compare the distributions of the NH3 … view at source ↗
Figure 9
Figure 9. Figure 9: Observed (gray) and modeled (blue) spectra at the offset positions of source A (0. ′′6 north-east). The modeled spectra are drawn for 100 samples randomly selected from the posterior chains. The vertical red dotted line marks the best-fit (median of the posterior sample) line center velocity [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Same as [PITH_FULL_IMAGE:figures/full_fig_p012_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Result of the model fit to the velocity-integrated intensities at the protostar positions of source A (left) and source B (right) in the form of rotation diagram. Random drawn from the posterior are shown in gray and the best-fit model that maximize the likelihood is plotted by the black dashed curve. The color represents the maximum optical depth among the two components for each inversion transition [P… view at source ↗
Figure 12
Figure 12. Figure 12: Stacked channel maps of the NH3 (2,2) and (3,3) emission in source A shown in units of S/N. Contours start at S/N = 3 and increase in steps of 2. Crimier, N., Ceccarelli, C., Maret, S., et al. 2010, A&A, 519, A65, doi: 10.1051/0004-6361/200913112 Danger, G., Borget, F., Chomat, M., et al. 2011, A&A, 535, A47, doi: 10.1051/0004-6361/201117602 Daranlot, J., Hincelin, U., Bergeat, A., et al. 2012, Proceeding… view at source ↗
Figure 13
Figure 13. Figure 13: Stacked channel maps of transitions with Eu > 1000 K in source A shown in units of S/N. Contours start at S/N = 3 and increase in steps of 2. −2 −1 0 1 2 2 1 0 −1 −2 R.A. offset (00) −2 −1 0 1 2 Dec. offset (00 ) 2 1 0 −1 −2 0 2 4 6 8 S/N Source B [PITH_FULL_IMAGE:figures/full_fig_p021_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Same as [PITH_FULL_IMAGE:figures/full_fig_p021_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: Same as [PITH_FULL_IMAGE:figures/full_fig_p022_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: Result of the single-component model fit to the veloci￾ty-integrated intensities at the protostar positions of source B in the form of rotation diagram. Random drawn from the posterior are shown in gray and the best-fit model that maximize the likelihood is plotted by the black dashed curve. The color represents the max￾imum optical depth among the two components for each inversion transition. Jørgensen, … view at source ↗
read the original abstract

Ammonia (NH$_3$) is one of the key volatiles that plays a central role in nitrogen chemistry and its evolution during the epoch of star and planet formation. We present subarcsecond ($\sim0.\!\!^{\prime\prime}5$) resolution observations of NH$_3$ molecular emission lines with Karl G. Jansky Very Large Array (VLA) toward the Class 0 multiple system IRAS 16293-2422 including source A and source B as major components. This comprises the most comprehensive set of NH$_3$ line observations in protostellar sources to date, which includes 17 inversion transitions with a wide range of upper state energies ($E_\mathrm{u}$) spanning from $\sim$23 K to $\sim$1,580 K. We detect spatially resolved emission of a number of transitions, and find that the high-$E_\mathrm{u}$ ($\gtrsim$1,000 K) lines show compact distributions in the vicinity of protostars while low-$E_\mathrm{u}$ ($\lesssim$150 K) lines exhibit more extended emission. Utilizing a two-component model, we constrain the rotation temperature and NH$_3$ column density for both source A and source B. The rotation temperature of the warmer component reaches $\sim$200-300 K, indicating that the high-$E_\mathrm{u}$ lines selectively trace the inner hot region. We suggest that this hot NH$_3$ gas in source A is originated from the local shock heating based on the comparison with the previous high-resolution ALMA observations, while that in source B could be explained by the mass accretion heating in the innermost hot region. We also briefly discuss the chemistry related to NH$_3$ based on the abundance ratios relative to major icy molecules derived using literature values.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 2 minor

Summary. The paper reports subarcsecond (~0.5") VLA observations of 17 NH3 inversion transitions (Eu ~23–1580 K) toward the Class 0 system IRAS 16293-2422. Spatially resolved emission shows high-Eu lines compact near the protostars and low-Eu lines more extended. A two-component LTE model yields rotation temperatures of ~200–300 K for the warm component in both source A and B, with NH3 column densities also constrained; the authors interpret the hot gas in A as shock-heated and in B as accretion-heated via comparison to prior ALMA data.

Significance. The dataset is the most comprehensive NH3 line set yet obtained toward a protostellar source. If the excitation modeling holds, the work supplies direct constraints on inner-region temperatures and offers a concrete test of competing heating mechanisms (shock vs. accretion) at subarcsecond scales, strengthening the link between NH3 excitation and nitrogen chemistry during the Class 0 phase.

major comments (1)
  1. [modeling approach (abstract and implied analysis section)] The two-component LTE fit to the 17 lines (abstract) is presented without reported checks for optical-depth corrections or non-LTE effects across the Eu range up to 1580 K. Because the warm-component T_rot ~200–300 K and the subsequent shock/accretion interpretation rest directly on this assumption, the lack of supporting diagnostics (e.g., line-ratio tests or RADEX comparisons) is load-bearing for the central claim.
minor comments (2)
  1. The abstract states that high-Eu lines are “selectively trace the inner hot region” but does not quantify beam-filling factors or report formal uncertainties on the derived T_rot values.
  2. Literature values for icy-molecule abundances are invoked for the chemistry discussion; the specific references and any assumptions about beam dilution should be stated explicitly.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review and for acknowledging the value of our NH3 dataset. We address the single major comment below.

read point-by-point responses

  1. Referee: The two-component LTE fit to the 17 lines (abstract) is presented without reported checks for optical-depth corrections or non-LTE effects across the Eu range up to 1580 K. Because the warm-component T_rot ~200–300 K and the subsequent shock/accretion interpretation rest directly on this assumption, the lack of supporting diagnostics (e.g., line-ratio tests or RADEX comparisons) is load-bearing for the central claim.

    Authors: We appreciate the referee drawing attention to the need for explicit validation of the LTE assumption. The two-component LTE model follows the standard approach used in prior NH3 studies of protostars, where the high densities (typically >10^6 cm^{-3}) near the sources support thermalization of the inversion transitions. The derived T_rot values are also consistent with independent temperature estimates from other species in the literature. That said, we agree that reporting supporting diagnostics would strengthen the manuscript. In the revised version we will add (i) estimates of line optical depths derived from the fitted column densities and (ii) a line-ratio consistency check between pairs of transitions with comparable Eu values. We will also briefly discuss why non-LTE effects are expected to be small for the warm component given the source densities. Full non-LTE modeling with RADEX lies outside the scope of this primarily observational work but is not required to support the reported temperatures. These additions will not change the main scientific conclusions. revision: yes

Circularity Check

0 steps flagged

No circularity; results derive from new VLA data and standard two-component LTE modeling

full rationale

The derivation chain consists of new subarcsecond VLA observations of 17 NH3 inversion lines (Eu 23-1580 K), detection of spatially resolved emission, and application of a standard two-component model to extract T_rot and column density. The warm-component T_rot ~200-300 K and heating-origin suggestions follow directly from these data plus comparison to independent prior ALMA maps. No self-definitional relations, fitted inputs renamed as predictions, load-bearing self-citations, or ansatz smuggling appear; the central results remain independent of the paper's own prior outputs.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The paper's central claims rest on the applicability of the two-component rotation diagram method to the observed lines and the interpretation of spatial distributions from comparison with prior data.

free parameters (2)
  • warmer component rotation temperature = ~200-300 K
    Derived from fitting the two-component model to the observed line intensities.
  • NH3 column density
    Constrained from the model but specific values not given in abstract.
axioms (1)
  • domain assumption The molecular emission can be modeled with two discrete temperature components in LTE
    Used to constrain parameters from the multi-line data.

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Reference graph

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