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REVIEW 1 major objections 2 minor 100 references

Subarcsecond Multi-line Observations of NH$_3$ with VLA toward the Class 0 Source IRAS 16293-2422

T0 review · 1 major / 2 minor · reviewed 2026-06-28 · grok-4.3

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

Pith's one-line read High-energy ammonia lines trace 200-300 K gas near the protostars in IRAS 16293-2422.

desk verdict New VLA multi-line NH3 data for IRAS 16293-2422 is the real contribution, but the shock-versus-accretion heating claims rest on a two-component LTE model whose optical-depth and non-LTE assumptions are not obviously validated. read the letter →

arxiv 2606.00212 v1 pith:H755S7ZW submitted 2026-05-29 astro-ph.GA astro-ph.EPastro-ph.SR

Yoshihide Yamato , Yuri Aikawa , Kenji Furuya , John J. Tobin , Jes K. J{o}rgensen This is my paper
classification astro-ph.GAastro-ph.EPastro-ph.SR
keywords ammoniaprotostarsVLAobservationsmolecularlinesClass0sourcesIRAS16293-2422starformationchemistry
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

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.

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.

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.

Watch

Extended reading notes

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.

Load-bearing premise

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

Editorial extensions

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.

Reading between the lines

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.
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Editorial analysis

A structured set of objections, weighed in public.

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

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 · score 0.0 of 10

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.

Assumptions & free parameters 2 free parameters · 1 assumptions · 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.
assumptions (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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Cite this review

Pith. "Pith review of Subarcsecond Multi-line Observations of NH$_3$ with VLA toward the Class 0 Source IRAS 16293-2422." pith.science (2026). https://pith.science/paper/H755S7ZW

@misc{pith2026260600212,
  author       = {Pith},
  title        = {Pith review of: Subarcsecond Multi-line Observations of NH$_3$ with VLA toward the Class 0 Source IRAS 16293-2422},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/H755S7ZW}},
  note         = {Machine review of arXiv:2606.00212}
}
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.

Figures

Figures reproduced from arXiv: 2606.00212 by the authors.

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 emission, we per… view at source ↗
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. 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 for inte￾g… view at source ↗
Figures from the paper (12 more)
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 …
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_5.png]
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…
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…
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 sampl…
Figure 10
Figure 10. Figure 10: Same as [PITH_FULL_IMAGE:figures/full_fig_p012_10.png]
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 …
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…
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:fi…
Figure 14
Figure 14. Figure 14: Same as [PITH_FULL_IMAGE:figures/full_fig_p021_14.png]
Figure 15
Figure 15. Figure 15: Same as [PITH_FULL_IMAGE:figures/full_fig_p022_15.png]
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…

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Works this paper leans on

100 extracted references · 96 canonical work pages

  1. [1]

    On the nature of the compact sources in IRAS 16293-2422 seen in at centimeter to sub-millimeter wavelengths

    On the Nature of the Compact Sources in IRAS 16293-2422 Seen at Centimeter to Submillimeter Wavelengths. , keywords =. doi:10.3847/1538-4357/ab0c97 , archivePrefix =. 1903.02202 , primaryClass =

    work page Pith review arXiv doi:10.3847/1538-4357/ab0c97 1903

  2. [2]

    , keywords =

    Orbital and Mass Constraints of the Young Binary System IRAS 16293-2422 A. , keywords =. doi:10.3847/1538-4357/ab960b , archivePrefix =. 2005.11954 , primaryClass =

    work page doi:10.3847/1538-4357/ab960b 2005

  3. [3]

    , keywords =

    Substructures in the Disk-forming Region of the Class 0 Low-mass Protostellar Source IRAS 16293-2422 Source A on a 10 au Scale. , keywords =. doi:10.3847/1538-4357/abbe14 , archivePrefix =. 2010.01273 , primaryClass =

    work page doi:10.3847/1538-4357/abbe14 2010

  4. [4]

    Research Notes of the American Astronomical Society , year = 2018, month = Sep, volume =

    A Robust Method to Measure Centroids of Spectral Lines. Research Notes of the American Astronomical Society , year = 2018, month = Sep, volume =. doi:10.3847/2515-5172/aae265 , adsurl =

    work page doi:10.3847/2515-5172/aae265 2018

  5. [5]

    Chemical and Physical Picture of IRAS 16293-2422 Source B at a Sub-arcsecond Scale Studied with ALMA

    Chemical and Physical Picture of IRAS 16293-2422 Source B at a Sub-arcsecond Scale Studied with ALMA. , keywords =. doi:10.3847/1538-4357/aaa6c7 , archivePrefix =. 1801.04174 , primaryClass =

    work page Pith review arXiv doi:10.3847/1538-4357/aaa6c7

  6. [6]

    Infalling-Rotating Motion and Associated Chemical Change in the Envelope of IRAS 16293-2422 Source A Studied with ALMA

    Infalling-Rotating Motion and Associated Chemical Change in the Envelope of IRAS 16293-2422 Source A Studied with ALMA. , keywords =. doi:10.3847/0004-637X/824/2/88 , archivePrefix =. 1605.00340 , primaryClass =

    work page Pith review arXiv doi:10.3847/0004-637x/824/2/88

  7. [7]

    The ALMA-PILS survey: Isotopic composition of oxygen-containing complex organic molecules toward IRAS 16293-2422B

    The ALMA-PILS survey: isotopic composition of oxygen-containing complex organic molecules toward IRAS 16293-2422B. , keywords =. doi:10.1051/0004-6361/201731667 , archivePrefix =. 1808.08753 , primaryClass =

    work page Pith review arXiv doi:10.1051/0004-6361/201731667

  8. [8]

    K., Calcutt , H., et al

    The ALMA-PILS survey: inventory of complex organic molecules towards IRAS 16293-2422 A. , keywords =. doi:10.1051/0004-6361/201936299 , archivePrefix =. 2001.06400 , primaryClass =

    work page doi:10.1051/0004-6361/201936299 2001

Show all 100 references
  1. [9]

    , keywords =

    emcee: The MCMC Hammer. , keywords =. doi:10.1086/670067 , archivePrefix =. 1202.3665 , primaryClass =

    doi arXiv

  2. [10]

    Direct detection of infall onto source B and high-resolution kinematics of source A

    The first ALMA view of IRAS 16293-2422. Direct detection of infall onto source B and high-resolution kinematics of source A. , keywords =. doi:10.1051/0004-6361/201219589 , archivePrefix =. 1206.5215 , primaryClass =

    doi arXiv

  3. [11]

    , keywords =

    Detection of the Simplest Sugar, Glycolaldehyde, in a Solar-type Protostar with ALMA. , keywords =. doi:10.1088/2041-8205/757/1/L4 , archivePrefix =. 1208.5498 , primaryClass =

    doi arXiv

  4. [12]

    , keywords =

    ALMA 690 GHz Observations of IRAS 16293-2422B: Infall in a Highly Optically Thick Disk. , keywords =. doi:10.1088/2041-8205/764/1/L14 , archivePrefix =. 1301.3105 , primaryClass =

    doi arXiv

  5. [13]

    , keywords =

    Molecular Line Profile Fitting with Analytic Radiative Transfer Models. , keywords =. doi:10.1086/427141 , archivePrefix =. astro-ph/0410748 , primaryClass =

    doi arXiv

  6. [14]

    , keywords =

    A Chemical View of Protostellar-disk Formation in L1527. , keywords =. doi:10.1088/2041-8205/791/2/L38 , adsurl =

    doi

  7. [15]

    , keywords =

    Formation of a Keplerian Disk in the Infalling Envelope around L1527 IRS: Transformation from Infalling Motions to Kepler Motions. , keywords =. doi:10.1088/0004-637X/796/2/131 , archivePrefix =. 1410.0172 , primaryClass =

    doi arXiv

  8. [16]

    , keywords =

    Which molecule traces what: Chemical diagnostics of protostellar sources. , keywords =. doi:10.1051/0004-6361/202140692 , archivePrefix =. 2107.03696 , primaryClass =

    doi

  9. [17]

    , year = 2014, month = mar, volume =

    Change in the chemical composition of infalling gas forming a disk around a protostar. , year = 2014, month = mar, volume =. doi:10.1038/nature13000 , adsurl =

    2014 doi

  10. [18]

    Early Planet Formation in Embedded Disks (eDisk). III. A First High-resolution View of Submillimeter Continuum and Molecular Line Emission toward the Class 0 Protostar L1527 IRS. , keywords =. doi:10.3847/1538-4357/accf87 , archivePrefix =. 2306.15407 , primaryClass =

    doi

  11. [19]

    , keywords =

    A Cosmic Abundance Standard: Chemical Homogeneity of the Solar Neighborhood and the ISM Dust-Phase Composition. , keywords =. doi:10.1086/595618 , archivePrefix =. 0809.2403 , primaryClass =

    doi arXiv

  12. [20]

    , keywords =

    The Spitzer Ice Legacy: Ice Evolution from Cores to Protostars. , keywords =. doi:10.1088/0004-637X/740/2/109 , archivePrefix =. 1107.5825 , primaryClass =

    doi arXiv

  13. [21]

    Proceedings of the National Academy of Science , keywords =

    Elemental nitrogen partitioning in dense interstellar clouds. Proceedings of the National Academy of Science , keywords =. doi:10.1073/pnas.1200017109 , archivePrefix =. 1206.4905 , primaryClass =

    doi arXiv

  14. [22]

    , keywords =

    Tracing the atomic nitrogen abundance in star-forming regions with ammonia deuteration. , keywords =. doi:10.1093/mnras/sty553 , archivePrefix =. 1802.08494 , primaryClass =

    doi arXiv

  15. [23]

    , keywords =

    Kinematics of the Ammonia Disk Around the Protostar NGC 1333 IRAS 4A2. , keywords =. doi:10.1088/2041-8205/723/1/L34 , archivePrefix =. 1010.1996 , primaryClass =

    doi arXiv

  16. [24]

    , keywords =

    The First Interferometric Measurements of NH _ 2 D/NH _ 3 Ratio in Hot Corinos. , keywords =. doi:10.3847/1538-4357/ac9ea5 , archivePrefix =. 2210.16336 , primaryClass =

    doi

  17. [25]

    , keywords =

    Tracking the Ice Mantle History in the Solar-type Protostars of NGC 1333 IRAS 4. , keywords =. doi:10.3847/2041-8213/ac85af , archivePrefix =. 2208.00247 , primaryClass =

    doi

  18. [26]

    , keywords =

    Ammonia Imaging of the Disks in the NGC 1333 IRAS 4A Protobinary System. , keywords =. doi:10.1086/522116 , archivePrefix =. 0708.1039 , primaryClass =

    doi arXiv

  19. [27]

    , keywords =

    Hot Corinos Chemical Diversity: Myth or Reality?. , keywords =. doi:10.3847/2041-8213/ab8d41 , archivePrefix =. 2006.04484 , primaryClass =

    doi

  20. [28]

    , keywords =

    A revised distance to IRAS 16293-2422 from VLBA astrometry of associated water masers. , keywords =. doi:10.1051/0004-6361/201732093 , archivePrefix =. 1802.03234 , primaryClass =

    doi arXiv

  21. [29]

    First results from an unbiased submillimeter wavelength line survey of the Class 0 protostellar binary IRAS 16293-2422 with ALMA

    The ALMA Protostellar Interferometric Line Survey (PILS). First results from an unbiased submillimeter wavelength line survey of the Class 0 protostellar binary IRAS 16293-2422 with ALMA. , keywords =. doi:10.1051/0004-6361/201628648 , archivePrefix =. 1607.08733 , primaryClass =

    doi arXiv

  22. [30]

    , keywords =

    The Duplicity of IRAS 16293-2422: A Protobinary Star?. , keywords =. doi:10.1086/167156 , adsurl =

    doi

  23. [31]

    , keywords =

    Large Proper Motions in the Young Low-Mass Protostellar System IRAS 16293-2422. , keywords =

  24. [32]

    , keywords =

    IRAS 16293-2422: Proper Motions, Jet Precession, the Hot Core, and the Unambiguous Detection of Infall. , keywords =. doi:10.1086/432828 , archivePrefix =. astro-ph/0506435 , primaryClass =

    doi arXiv

  25. [33]

    , keywords =

    New Radio Sources and the Composite Structure of Component B in the Very Young Protostellar System IRAS 16293-2422. , keywords =. doi:10.1086/522568 , archivePrefix =. 0708.2420 , primaryClass =

    doi arXiv

  26. [34]

    , keywords =

    Confirmation of a Recent Bipolar Ejection in the Very Young Hierarchical Multiple System IRAS 16293-2422. , keywords =. doi:10.1088/0004-637X/712/2/1403 , archivePrefix =. 1002.2417 , primaryClass =

    doi arXiv

  27. [35]

    The case of IRAS 16293A

    Temperature profiles of young disk-like structures. The case of IRAS 16293A. , keywords =. doi:10.1051/0004-6361/201936839 , archivePrefix =. 1911.03495 , primaryClass =

    1911 doi

  28. [36]

    , keywords =

    Dust Hot Spots at 10 au Scales around the Class 0 Binary IRAS 16293-2422 A: A Departure from the Passive Irradiation Model. , keywords =. doi:10.3847/2041-8213/aca53a , archivePrefix =. 2212.08436 , primaryClass =

    doi

  29. [37]

    , keywords =

    A Simple Model of Spectral-Line Profiles from Contracting Clouds. , keywords =. doi:10.1086/310146 , adsurl =

    doi

  30. [38]

    , keywords =

    Infall, Outflow, Rotation, and Turbulent Motions of Dense Gas within NGC 1333 IRAS 4. , keywords =. doi:10.1086/323854 , archivePrefix =. astro-ph/0108022 , primaryClass =

    doi arXiv

  31. [39]

    , keywords =

    Exploring the dust grain size and polarization mechanism in the hot and massive Class 0 disk IRAS 16293-2422 B. , keywords =. doi:10.1051/0004-6361/202244628 , archivePrefix =. 2311.02521 , primaryClass =

    doi

  32. [40]

    ACS Earth and Space Chemistry , keywords =

    Thermal Desorption of Interstellar Ices: A Review on the Controlling Parameters and Their Implications from Snowlines to Chemical Complexity. ACS Earth and Space Chemistry , keywords =. doi:10.1021/acsearthspacechem.1c00357 , archivePrefix =. 2201.07512 , primaryClass =

    doi

  33. [41]

    , keywords =

    Discovery of a Hot Corino in the Bok Globule B335. , keywords =. doi:10.3847/2041-8205/830/2/L37 , archivePrefix =. 1610.03942 , primaryClass =

    doi arXiv

  34. [42]

    FAUST. VII. Detection of a Hot Corino in the Prototypical Warm Carbon-chain Chemistry Source IRAS 15398-3359. , keywords =. doi:10.3847/1538-4357/acc1e5 , archivePrefix =. 2303.03564 , primaryClass =

    doi

  35. [43]

    , keywords =

    Chemical and Physical Characterization of the Isolated Protostellar Source CB68: FAUST IV. , keywords =. doi:10.3847/1538-4357/ac77e7 , archivePrefix =. 2206.06603 , primaryClass =

    doi

  36. [44]

    , keywords =

    L483: Warm Carbon-chain Chemistry Source Harboring Hot Corino Activity. , keywords =. doi:10.3847/1538-4357/aa6300 , archivePrefix =. 1703.03653 , primaryClass =

    doi arXiv

  37. [45]

    , keywords =

    Chemical Differentiation and Temperature Distribution on a Few au Scale around the Protostellar Source B335. , keywords =. doi:10.3847/1538-4357/ac7ff4 , archivePrefix =. 2207.06721 , primaryClass =

    doi

  38. [46]

    Early Planet Formation in Embedded Disks (eDisk). VII. Keplerian Disk, Disk Substructure, and Accretion Streamers in the Class 0 Protostar IRAS 16544-1604 in CB 68. , keywords =. doi:10.3847/1538-4357/acdd7a , archivePrefix =. 2306.15443 , primaryClass =

    doi

  39. [47]

    Early Planet Formation in Embedded Disks (eDisk). IV. The Ringed and Warped Structure of the Disk around the Class I Protostar L1489 IRS. , keywords =. doi:10.3847/1538-4357/accd71 , archivePrefix =. 2306.15408 , primaryClass =

    doi

  40. [48]

    , keywords =

    Comprehensive Study of Thermal Desorption of Grain-surface Species by Accretion Shocks around Protostars. , keywords =. doi:10.3847/1538-4357/aa67df , adsurl =

    doi

  41. [49]

    , keywords =

    Evaporation of Grain-surface Species by Shock Waves in a Protoplanetary Disk. , keywords =. doi:10.1088/0004-637X/799/2/141 , archivePrefix =. 1412.1178 , primaryClass =

    doi arXiv

  42. [50]

    Sulfur chemistry

    Modeling accretion shocks at the disk-envelope interface. Sulfur chemistry. , keywords =. doi:10.1051/0004-6361/202141591 , archivePrefix =. 2107.09750 , primaryClass =

    doi

  43. [51]

    , keywords =

    The ALMA-PILS survey: 3D modeling of the envelope, disks and dust filament of IRAS 16293-2422. , keywords =. doi:10.1051/0004-6361/201731668 , archivePrefix =. 1712.06984 , primaryClass =

    doi arXiv

  44. [52]

    , keywords =

    The young protostellar disc in IRAS 16293-2422 B is hot and shows signatures of gravitational instability. , keywords =. doi:10.1093/mnras/stab2657 , archivePrefix =. 2109.06497 , primaryClass =

    doi

  45. [53]

    , keywords =

    The solar type protostar IRAS16293-2422: new constraints on the physical structure. , keywords =. doi:10.1051/0004-6361/200913112 , archivePrefix =. 1003.5774 , primaryClass =

    doi arXiv

  46. [54]

    Nature Astronomy , keywords =

    Evidence of ammonium salts in comet 67P as explanation for the nitrogen depletion in cometary comae. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0991-9 , archivePrefix =. 1911.13005 , primaryClass =

    1911 doi

  47. [55]

    Science , keywords =

    Ammonium salts are a reservoir of nitrogen on a cometary nucleus and possibly on some asteroids. Science , keywords =. doi:10.1126/science.aaw7462 , archivePrefix =. 2003.06034 , primaryClass =

    2003 doi

  48. [56]

    , keywords =

    Abundant ammonium hydrosulphide embedded in cometary dust grains. , keywords =. doi:10.1093/mnras/stac2440 , archivePrefix =. 2208.11396 , primaryClass =

    doi

  49. [57]

    arXiv e-prints , keywords =

    Ammonium hydrosulfide (NH4SH) as a potentially significant sulfur sink in interstellar ices. arXiv e-prints , keywords =. doi:10.48550/arXiv.2410.02860 , archivePrefix =. 2410.02860 , primaryClass =

    doi

  50. [58]

    , keywords =

    Kinetics and Mechanisms of the Acid-base Reaction Between NH _ 3 and HCOOH in Interstellar Ice Analogs. , keywords =. doi:10.3847/0004-637X/829/2/85 , archivePrefix =. 1608.00010 , primaryClass =

    doi arXiv

  51. [59]

    , keywords =

    Carbamic acid and carbamate formation in NH\ 3\ :CO\ 2\ ices - UV irradiation versus thermal processes. , keywords =. doi:10.1051/0004-6361:200810536 , adsurl =

    doi

  52. [60]

    , keywords =

    Experimental investigation of aminoacetonitrile formation through the Strecker synthesis in astrophysical-like conditions: reactivity of methanimine (CH _ 2 NH), ammonia (NH _ 3 ), and hydrogen cyanide (HCN). , keywords =. doi:10.1051/0004-6361/201117602 , adsurl =

    doi

  53. [61]

    , year = 2024, month = sep, volume =

    Sulphur storage in cold molecular clouds: the case of the NH _ 4 ^ + SH ^ - salt on interstellar dust grains. , year = 2024, month = sep, volume =. doi:10.1093/mnras/stae1747 , adsurl =

    2024 doi

  54. [62]

    The high-resolution ALMA and SMA view

    Warm water deuterium fractionation in IRAS 16293-2422. The high-resolution ALMA and SMA view. , keywords =. doi:10.1051/0004-6361/201220638 , archivePrefix =. 1211.6605 , primaryClass =

    doi arXiv

  55. [63]

    Nature Astronomy , keywords =

    An Ice Age JWST inventory of dense molecular cloud ices. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01875-w , archivePrefix =. 2301.09140 , primaryClass =

    doi

  56. [64]

    , keywords =

    A deep search for large complex organic species toward IRAS16293-2422 B at 3 mm with ALMA. , keywords =. doi:10.1051/0004-6361/202347832 , archivePrefix =. 2401.04760 , primaryClass =

    doi

  57. [65]

    , keywords =

    The Herschel view of the dense core population in the Ophiuchus molecular cloud. , keywords =. doi:10.1051/0004-6361/201936442 , archivePrefix =. 2001.11036 , primaryClass =

    2001 doi

  58. [66]

    , keywords =

    Linelists for NH\_3, NH\_2D, ND\_2H, and ND _ 3 with quadrupole coupling hyperfine components. , keywords =. doi:10.1051/0004-6361:20054136 , adsurl =

    doi

  59. [67]

    doi:10.1051/0004-6361/20054136e , adsurl =

    Erratum: Linelists for NH3, NH2D, ND2H, and ND3 with quadrupole coupling hyperfine components. doi:10.1051/0004-6361/20054136e , adsurl =

    doi

  60. [68]

    , keywords =

    CASA, the Common Astronomy Software Applications for Radio Astronomy. , keywords =. doi:10.1088/1538-3873/ac9642 , archivePrefix =. 2210.02276 , primaryClass =

    doi arXiv

  61. [69]

    , keywords =

    Submillimeter, millimeter and microwave spectral line catalog. , keywords =. doi:10.1016/S0022-4073(98)00091-0 , adsurl =

    doi

  62. [70]

    , keywords =

    Submillimeter-wave and far-infrared spectroscopy of high-J transitions of the ground and _ 2 =1 states of ammonia. , keywords =. doi:10.1063/1.3499911 , adsurl =

    doi

  63. [71]

    A multilevel study of ammonia in star-forming regions. III. Orion-KL. , keywords =

  64. [72]

    , keywords =

    Hot ammonia emission : kinetic temperature gradients in Orion-KL. , keywords =

  65. [73]

    , keywords =

    The detection of the (J, K) = (18, 18) line of NH3. , keywords =. doi:10.1051/0004-6361:20065591 , archivePrefix =. astro-ph/0609057 , primaryClass =

    doi arXiv

  66. [74]

    A multilevel study of ammonia in star forming regions. V. The SGR B2 region. , keywords =

  67. [75]

    , keywords =

    Empirical Temperature Measurement in Protoplanetary Disks. , keywords =. doi:10.3847/1538-4357/aaa481 , archiveprefix =. 1801.03478 , primaryclass =

    doi arXiv

  68. [76]

    Molecules with ALMA at Planet-forming Scales (MAPS). IV. Emission Surfaces and Vertical Distribution of Molecules. , keywords =. doi:10.3847/1538-4365/ac1439 , archiveprefix =. 2109.06217 , primaryclass =

    doi

  69. [77]

    , keywords =

    ALMA Observations of the Transition from Infall Motion to Keplerian Rotation around the Late-phase Protostar TMC-1A. , keywords =. doi:10.1088/0004-637X/812/1/27 , archivePrefix =. 1508.07013 , primaryClass =

    doi arXiv

  70. [78]

    , keywords =

    ALMA Observations of Infalling Flows toward the Keplerian Disk around the Class I Protostar L1489 IRS. , keywords =. doi:10.1088/0004-637X/793/1/1 , archivePrefix =. 1407.2699 , primaryClass =

    doi arXiv

  71. [79]

    The Perseus ALMA Chemistry Survey (PEACHES). I. The Complex Organic Molecules in Perseus Embedded Protostars. , keywords =. doi:10.3847/1538-4357/abdfd6 , archivePrefix =. 2101.11009 , primaryClass =

    doi

  72. [80]

    , keywords =

    The Chemical Nature of Orion Protostars: Are ORANGES Different from PEACHES? ORANGES II. , keywords =. doi:10.3847/1538-4357/ac5904 , archivePrefix =. 2202.13835 , primaryClass =

    doi

  73. [81]

    , keywords =

    Questioning the spatial origin of complex organic molecules in young protostars with the CALYPSO survey. , keywords =. doi:10.1051/0004-6361/201937352 , archivePrefix =. 2002.00592 , primaryClass =

    2002 doi

  74. [82]

    Complex organic molecules in low-mass protostars on Solar System scales. II. Nitrogen-bearing species. , keywords =. doi:10.1051/0004-6361/202039996 , archivePrefix =. 2104.03326 , primaryClass =

    doi

  75. [83]

    , keywords =

    The Circumstellar Structure of IRAS 16293-2422: C 18O, NH 3, and CO Observations. , keywords =. doi:10.1086/168523 , adsurl =

    doi

  76. [84]

    , keywords =

    Thermal desorption of circumstellar and cometary ice analogs. , keywords =. doi:10.1051/0004-6361/201322824 , archivePrefix =. 1406.0425 , primaryClass =

    doi arXiv

  77. [85]

    , keywords =

    Experimental study of the binding energy of NH _ 3 on different types of ice and its impact on the snow line of NH _ 3 and H _ 2 O. , keywords =. doi:10.1051/0004-6361/202245775 , archivePrefix =. 2311.18619 , primaryClass =

    doi

  78. [86]

    , keywords =

    Ingredients for solar-like systems: protostar IRAS 16293-2422 B versus comet 67P/Churyumov-Gerasimenko. , keywords =. doi:10.1093/mnras/stz2430 , archivePrefix =. 1908.11290 , primaryClass =

    1908 doi

  79. [87]

    Constraining the chemical tracers of young protostellar sources

    Early Planet Formation in Embedded Disks (eDisk): XX. Constraining the chemical tracers of young protostellar sources. , keywords =. doi:10.1051/0004-6361/202553721 , archivePrefix =. 2509.19158 , primaryClass =

    doi

  80. [88]

    , keywords =

    Sulfur oxides tracing streamers and shocks at low-mass protostellar disk─envelope interfaces. , keywords =. doi:10.1051/0004-6361/202554186 , archivePrefix =. 2507.22870 , primaryClass =

    doi

  81. [89]

    , keywords =

    HOPS-288: A Laboratory for Complex Organics in Proto-binary/Proto-multiple Systems. , keywords =. doi:10.3847/1538-4357/ae38e1 , archivePrefix =. 2601.08948 , primaryClass =

    doi

  82. [90]

    , keywords =

    Hot Corino Chemistry in the Class I Binary Source Ser-emb 11. , keywords =. doi:10.3847/1538-4357/ac26b9 , archivePrefix =. 2109.11512 , primaryClass =

    doi

  83. [91]

    The hot corino at the heart of the prototypical Class I protostar L1551 IRS5

    FAUST I. The hot corino at the heart of the prototypical Class I protostar L1551 IRS5. , keywords =. doi:10.1093/mnrasl/slaa130 , archivePrefix =. 2007.10275 , primaryClass =

    2007 doi

  84. [92]

    , keywords =

    Complex organics in IRAS 4A revisited with ALMA and PdBI: Striking contrast between two neighbouring protostellar cores. , keywords =. doi:10.1051/0004-6361/201630334 , archivePrefix =. 1707.03745 , primaryClass =

    doi arXiv

  85. [93]

    , keywords =

    The Critical Density and the Effective Excitation Density of Commonly Observed Molecular Dense Gas Tracers. , keywords =. doi:10.1086/680342 , archivePrefix =. 1501.01629 , primaryClass =

    doi arXiv

  86. [94]

    , keywords =

    Efficient Formation of Formaldehyde and Methanol by the Addition of Hydrogen Atoms to CO in H _ 2 O-CO Ice at 10 K. , keywords =. doi:10.1086/341412 , adsurl =

    doi

  87. [95]

    Physical Chemistry Chemical Physics (Incorporating Faraday Transactions) , year = 2011, month = jan, volume =

    FTIR study of ammonia formation via the successive hydrogenation of N atoms trapped in a solid N2 matrix at low temperatures. Physical Chemistry Chemical Physics (Incorporating Faraday Transactions) , year = 2011, month = jan, volume =. doi:10.1039/C1CP20645A , adsurl =

    2011 doi

  88. [96]

    , keywords =

    Low-temperature surface formation of NH _ 3 and HNCO: hydrogenation of nitrogen atoms in CO-rich interstellar ice analogues. , keywords =. doi:10.1093/mnras/stu2028 , archivePrefix =. 1705.09184 , primaryClass =

    doi arXiv

  89. [97]

    , keywords =

    Ice inventory towards the protostar Ced 110 IRS4 observed with the James Webb Space Telescope: Results from the Early Release Science Ice Age program. , keywords =. doi:10.1051/0004-6361/202451505 , archivePrefix =. 2411.19651 , primaryClass =

    doi

  90. [98]

    , keywords =

    Observations of the icy universe. , keywords =. doi:10.1146/annurev-astro-082214-122348 , archivePrefix =. 1501.05317 , primaryClass =

    doi arXiv

  91. [99]

    , keywords =

    Expanding the Ice Inventory of NGC 1333 IRAS 2A with INDRA Using JWST Observations: Tracing Organic Refractories and Beyond. , keywords =. doi:10.3847/1538-4365/ae112f , archivePrefix =. 2506.15358 , primaryClass =

    doi

  92. [100]

    , keywords =

    Elemental and molecular abundances in comet 67P/Churyumov-Gerasimenko. , keywords =. doi:10.1093/mnras/stz2086 , archivePrefix =. 1907.11044 , primaryClass =

    1907 doi

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Reviewed June 28, 2026 · model on record in the stance chip above.