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FAUST XX. The chemical structure and temperature profile of the IRAS 4A2 hot corino at 20-50 au

T0 review · 3 major / 6 minor · reviewed 2026-08-09 · deepseek-v4-flash

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Pith's one-line read The paper claims that six complex organic molecules around the young protostar IRAS 4A2 are spatially segregated in nested shells, and that pairing each molecule's gas temperature with its emitting radius yields a gas temperature profile…

desk verdict First resolved iCOM segregation for IRAS 4A2 is solid and new; the q≈−1 temperature profile is a plausible but underconstrained interpretation that needs softening. read the letter →

arxiv 2501.19188 v1 pith:ZFJ2AJE3 submitted 2025-01-31 astro-ph.EP astro-ph.GAastro-ph.SR

J. Frediani , M. De Simone , L. Testi , L. Podio , C. Codella , C. J. Chandler , C. Ceccarelli , L. Loinard
show 15 more authors
A. López-Sepulcre B. Svoboda N. Sakai L. Chahine Y. Aikawa E. Bianchi M. Bouvier L. Cacciapuoti P. Caselli S. B. Charnley I. Jimenez-Serra D. Johnstone G. Sabatini Y. Shirley S. Yamamoto
This is my paper · ORCID
classification astro-ph.EPastro-ph.GAastro-ph.SR
keywords hotcorinosinterstellarcomplexorganicmoleculeschemicalsegregationgastemperatureprofileClass0protostarsIRAS4A2millimetredustabsorption
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

This paper uses millimetre interferometric observations of the young Class 0 protostar IRAS 4A2 to resolve, for the first time, the spatial arrangement of six complex organic molecules (methanol, methyl formate, acetaldehyde, ethanol, glycolaldehyde, and formamide) in the inner 50 au of its hot corino. The paper claims that these molecules are chemically segregated into nested shells, with methanol reaching out to about 40 au, methyl formate at about 36 au, acetaldehyde and ethanol at about 27-28 au, and glycolaldehyde and formamide confined to about 22-23 au. Combining the gas temperature each molecule probes with its measured emitting radius, the paper derives a gas temperature profile $T(r) \propto r^{-1}$ between 20 and 50 au. If correct, this profile is steeper than the $q \approx 0.4$-$0.5$ expected for an optically thin spherical collapsing envelope, hinting at a partially optically thick envelope or a gravitationally unstable disk-like structure. The result matters because it turns a handful of molecular lines into a direct radial thermometer of the earliest stages of star and planet formation.

What carries the argument

The load-bearing object is each iCOM used as a combined ruler and thermometer: a beam-deconvolved Gaussian fit to the integrated-intensity map of an isolated transition supplies the species' outer emitting radius, and a multi-line population analysis supplies the gas temperature and column density at that radius. A hot corino is a compact, hot, dense region around a young protostar rich in interstellar complex organic molecules (iCOMs, saturated carbon-bearing molecules with at least six atoms and including heteroatoms such as N or O). The chain that carries the argument is the pairing of these two per-species measurements; the power-law index $q$ comes from fitting temperature against radius for the four to five species whose excitation temperatures are reliably determined, with the formamide and acetaldehyde points treated separately because their temperatures could not be derived self-consistently.

What would settle it

A decisive check would be to map IRAS 4A2 at about 5-10 au resolution with deeper sensitivity and, for at least one species, across many transitions spanning a wide range of upper-state energies: if the gradient is real and thermal, the same $T(r)$ relation should be recovered within that single species, and the outer radii of the compact molecules should not grow with integration depth; if the compact molecules are merely rare, deeper maps would reveal them at larger radii and the apparent power-law index would move toward $q \approx 0.4$-$0.5$.

Watch

Extended reading notes

Core claim

The central claim, on the paper's own terms, is that the hot corino of IRAS 4A2 is chemically stratified at radii of 20 to 50 au. From 74 detected molecular lines the authors image each species and fit its emitting size with a beam-deconvolved two-dimensional Gaussian, and from a multi-line excitation analysis (non-LTE for methanol, LTE population or rotational diagrams for the others) they derive a gas temperature and column density for each species, correcting for both line opacity and foreground millimetre dust absorption. The measured radii increase from about 22-23 au for glycolaldehyde and formamide, through about 27-28 au for ethanol and acetaldehyde, to about 36 au for methyl formate and 40 au for methanol. Plotting each species' temperature against its emitting radius gives a power-law index $q = -1.0 \pm 0.2$ without the dust correction and $q = -0.8 \pm 0.2$ with it. The authors read this steep gradient as evidence that the inner envelope is not an optically thin spherical collapse, and they propose a partially optically thick envelope or a gravitationally unstable disk-like structure as the likely alternatives.

Load-bearing premise

The temperature profile rests on the assumption that the measured emitting radius of each molecule is the radius at which its line-derived excitation temperature actually equals the gas kinetic temperature, and not simply the radius down to which that molecule is abundant enough to be detected.

Editorial extensions

If this is right

  • If the steep profile is real, the standard picture of a hot corino as an optically thin spherical collapsing envelope needs revision at 20-50 au scales, and models should include partial dust opacity or rotationally supported, gravitationally unstable structure.
  • The observed chemical segregation means abundance gradients inside 50 au: methanol traces the outer zone while glycolaldehyde and formamide trace the hottest, densest inner zone, so chemical models must place these molecules at different sublimation radii even within a single hot corino.
  • Millimetre dust absorption raises derived gas temperatures by 50-100 K and column densities by roughly a factor of 1.6, so previous unresolved estimates of hot corino temperatures and abundances are likely biased low wherever such foreground absorption is ignored.
  • The measured $T(r) \propto r^{-1}$ relation gives a direct observational target for thermochemical models of embedded Class 0/I disks and envelopes, and similar measurements in other sources would show whether such steep gradients are common.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the alternative raised in the paper is true — that the compact species are simply less abundant and detectable only at smaller radii — then the inferred $q \approx -1$ profile would be an observational artefact rather than a physical temperature gradient; deeper integrations or searches in rarer isotopologues would flatten the apparent slope toward the standard envelope value.
  • The ordering of emitting radii (methanol outermost, glycolaldehyde and formamide innermost) suggests a testable correlation between each molecule's ice binding energy and its desorption radius; such a correlation could be checked once consistent binding energies are available for all six molecules.
  • The same dust-absorption correction is applied uniformly to all species although the absorption is measured on a fixed scale of about 0.26 arcsec; if the foreground dust opacity varies with radius, the correction should be applied radially, and that is testable with higher-resolution continuum and line data.
  • If a similar steep temperature profile is confirmed in other hot corinos, the default geometry for embedded Class 0 protostars may shift from spherical infall toward structures with significant mid-plane opacity or young disk rotation, with consequences for where and when planet-forming material first becomes warm.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. This paper uses ALMA/FAUST observations of IRAS 4A2 to measure the spatial extent of six iCOMs and to derive gas temperatures and column densities from multi-line analyses with opacity and foreground-dust corrections. The authors report a chemical segregation with outer radii increasing from ~22 au (NH2CHO, CH2OHCHO) to ~40 au (CH3OH), and combine per-species temperatures with these radii to infer T(r)∝r^q, q≈−1, over 20–50 au. The chemical segregation is the more robust result; the temperature profile relies on identifying each species' fitted radius with the location where its single-zone temperature applies.

Significance. The paper makes a strong observational contribution: the sizes are measured from multiple independent transitions per species, with image-plane and visibility-plane fits in agreement, and the analysis corrects for line opacity (population diagram) and foreground mm dust absorption. If the temperature-profile inference were secure, q≈−1 would be an important constraint on the inner-envelope structure of a Class 0 hot corino. However, the central inference is less secure than the abstract suggests, for the reasons detailed below.

major comments (3)
  1. [§4.2, Fig. 5] The central claim that T(r) ∝ r^q with q = −1.0 ± 0.2 (or −0.8 ± 0.2 with dust obscuration) assumes that the beam-deconvolved emitting radius r̄ of each species is the radial coordinate at which its measured gas temperature applies. This mapping is not established. In §3.1 the fitted radius is defined as the outer radius 'where the line optical depth is equal to or larger than 1', and the population-diagram analysis in App. D finds τ>1 for most lines. For optically thick lines, the apparent size is a projected τ≈1 surface whose radius depends on the species' abundance, upper-level column, and excitation, not purely on the local gas temperature. Consequently, an abundance/opacity ordering among the six iCOMs can produce the observed size–temperature anticorrelation even if all species share the same (or a shallower) temperature profile. The alternative 'different molecular abundances at limited sensitivity' is acknowledged in §3.1 but not eliminated; the fact that the compact species differ in size does not break the degeneracy because their abundances and opacities also differ. Although §4.2 calls the profile 'tentative', the abstract and conclusions present q≈−1 as a result, and the current analysis does not uniquely support it.
  2. [Table 1, §3.2, App. D] The fit in Fig. 5 uses only four independent points (CH3OH, HCOOCH3, CH3CH2OH, CH2OHCHO); CH3CHO is excluded because its line opacity could not be estimated self-consistently, and NH2CHO is excluded because its temperature is simply fixed to that of CH2OHCHO. Each temperature comes from a single-zone fit to the spectrum extracted at the continuum peak, with the emitting region entering only through a filling factor set by the species' fitted source size. T_i is therefore a region-averaged excitation temperature over the whole emitting area, not a temperature measured at radius r̄_i. Pairing T_i with r̄_i mixes a boundary radius with an area-averaged temperature, and this systematic is not included in the 1σ error bars on q. With four points and this systematic, the quoted uncertainties on q are substantially underestimated.
  3. [§4.1] The millimeter dust obscuration correction is load-bearing for the temperatures in Table 1 and hence for q. Section 4.1 applies a single scalar absorption factor (30% at 143 GHz, 50% at 243 GHz) estimated from prior CH3OH work to all six iCOMs at scales < 0.26 arcsec. The paper states this is an assumption, but the correction shifts gas temperatures by 50–100 K, and the uncertainty on the factors and any spatial variation of the foreground dust are not propagated into the T–r fit. A differential correction among species could flatten or steepen the inferred profile; at minimum the authors should state explicitly that q is tentative pending a spatially resolved foreground dust optical-depth measurement, or propagate the uncertainty.
minor comments (6)
  1. [Abstract] 'Besides of their prebiotic role' should read 'Besides their prebiotic role'.
  2. [§4.2] 'disantangle' should be 'disentangle', and 'A larger spectral resolution' should be 'A higher spectral resolution'.
  3. [§3.1] The reported slope for CH3CHO, '0.010± 0.0022± 0.005', appears to contain a typo; please clarify the uncertainties.
  4. [Fig. 2 caption] The caption says 'The grey solid lines indicate the linear fit performed on the derived radius', but no fit is shown for CH2OHCHO and NH2CHO; this should be stated explicitly.
  5. [Table 1] The header 'θ b source [arcsec]' appears garbled, and the text should clarify that these source sizes are adopted from §3.1 and used as fixed inputs in the analysis.
  6. [§3.2] The reduced chi-square symbol '˜χ2' is used before it is defined; define it at first use in §3.2 or refer forward to App. C.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the q≈−1 profile is an empirical correlation, not a forced derivation, and the chemical segregation is independent of the temperature fitting.

full rationale

The paper's central observational result, the chemical segregation of six iCOMs around IRAS 4A2, comes from direct image-plane and visibility-plane Gaussian fits of isolated lines chosen to have similar upper-state energies, so it does not depend on any fitted parameter from the temperature analysis and is self-contained. The temperature profile in Sect. 4.2 is an empirical correlation: each species contributes a measured (fitted) gas temperature and a measured (fitted) emitting radius, and the exponent q is the slope of a power-law fit to those four points. No equation in the paper forces q to be -1 by construction; it is a descriptive fit, not a prediction of an independent quantity from the same inputs. The only coupling is that the multi-line temperature fits adopt per-species source sizes that are directly related to the same beam-deconvolved radii used as the radial coordinate (App. D: 'The source size derived from image fitting is assumed for each species'; Tab. 1). This creates a modeling dependence, but the temperatures are still determined by independent line-intensity ratios and opacity corrections, so the plotted T-r relation is not a mathematical identity. The paper explicitly acknowledges the main physical alternative to the size-temperature interpretation in Sect. 3.1 ('Another possibility is that we are observing different molecular abundances at limited sensitivity') and describes the profile as 'tentatively derive[d]' in Sect. 4.2; these are correctness and interpretational caveats, not circular reasoning. The self-citation to De Simone et al. (2020a, 2022b) for the foreground millimeter-dust absorption is an empirical estimate from centimeter and millimeter observations; it shifts the temperatures by 50-100 K but leaves the profile steep (q = -1.0 without, -0.8 with absorption), so it is not load-bearing for the central claim. Overall, the derivation chain is self-contained and the flagged limitations do not amount to circularity.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

No new physical entities are introduced. The central claim depends on five assumptions and four adopted or fitted parameters (dust absorption factors, per-species source sizes, a fixed NH2CHO temperature, and fixed LVG setup values). The source size coupling is the main circularity contributor.

free parameters (4)
  • Foreground dust absorption factors = 30% at 143 GHz; 50% at 243 GHz
    Adopted from De Simone et al. 2020a and 2022b for IRAS 4A2 and applied uniformly to all iCOM line intensities at scales below 0.26 arcsec. The central T-r profile shifts from q = -1.0 to q = -0.8 depending on these factors.
  • Source size per species (theta_source) = 0.30 arcsec (CH3OH), 0.26 (HCOOCH3), 0.19 (CH3CH2OH), 0.15 (CH2OHCHO), 0.20 (CH3CHO), 0.16 (NH2CHO)
    Derived from 2D Gaussian fits of the same emission maps, then used as fixed input in the LVG and population diagram analyses. This couples the radius axis and the temperature derivation.
  • NH2CHO gas temperature = 197 K
    Fixed to the best-fit temperature of CH2OHCHO because NH2CHO lines span too small an energy range for a rotational diagram.
  • CH3OH LVG fixed parameters = A/E ratio = 1; ortho-to-para ratio = 3; linewidth = 4.5 km/s; source size = 0.3 arcsec
    Assumed in the non-LTE LVG fit in Appendix C. The paper states results do not change for linewidth +/- 0.5 km/s, but the other values are not varied.
assumptions (5)
  • domain assumption The molecular line emitting regions are in LTE, or their non-LTE departure is correctly captured by the applied collisional coefficients.
    Used in the population diagram analysis in Appendix D and for the non-LTE LVG analysis in Appendix C; high densities support LTE for most species, but radiative pumping of high-Eu lines is discussed and argued to be negligible.
  • domain assumption The measured rotational temperature equals the gas kinetic temperature in the emitting region.
    Assumed in Section 3.2 for all species; if radiative pumping is significant, the temperatures are biased.
  • domain assumption The foreground dust absorption values from De Simone et al. 2020a and 2022b apply to all iCOM lines at scales below 0.26 arcsec.
    Used in Section 4.1 to correct integrated line fluxes; if the dust absorption is not uniform across species or scales, the derived temperatures and column densities will shift.
  • domain assumption The 2D Gaussian fitted radius is a valid proxy for the radial distance from the protostar.
    The paper explicitly notes in Section 3.1 that the exact geometry cannot be unambiguously determined with a 2D Gaussian fit, yet the T-r profile in Section 4.2 uses these radii as radial coordinates.
  • domain assumption The emitting radius of each species is set by the temperature structure, not by abundance sensitivity.
    The alternative explanation, that less abundant species are simply detected only at smaller radii, is raised and argued against in Section 3.1 but not conclusively excluded. This premise is required to interpret the size-temperature correlation as a temperature profile.

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Cite this review

Pith. "Pith review of FAUST XX. The chemical structure and temperature profile of the IRAS 4A2 hot corino at 20-50 au." pith.science (2026). https://pith.science/paper/ZFJ2AJE3

@misc{pith2026250119188,
  author       = {Pith},
  title        = {Pith review of: FAUST XX. The chemical structure and temperature profile of the IRAS 4A2 hot corino at 20-50 au},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ZFJ2AJE3}},
  note         = {Machine review of arXiv:2501.19188}
}
abstract

Young low-mass protostars often possess hot corinos, compact, hot and dense regions bright in interstellar Complex Organic Molecules (iCOMs). Besides of their prebiotic role, iCOMs can be used as a powerful tool to characterize the chemical and physical properties of hot corinos. Using ALMA/FAUST data we aim to explore the iCOMs emission at < 50 au scale around the Class 0 prototypical hot corino IRAS 4A2. We imaged IRAS 4A2 in six abundant, common iCOMs (CH$_3$OH, HCOOCH$_3$, CH$_3$CHO, CH$_3$CH$_2$OH, CH$_2$OHCHO, and NH$_2$CHO), and derived their emitting size. The column density and gas temperature for each species were derived at 1$\sigma$ from a multi-line analysis by applying a non-LTE approach for CH$_3$OH, and LTE population or rotational diagram analysis for the other iCOMs. Thanks to the unique estimates of the absorption from foreground millimeter dust toward IRAS 4A2, we derived for the first time unbiased gas temperatures and column densities. We resolved the IRAS 4A2 hot corino finding evidence for a chemical spatial distribution in the inner 50 au, with the outer emitting radius increasing from ~ 22-23 au for NH$_2$CHO and CH$_2$OHCHO, followed by CH$_3$CH$_2$OH (~ 27 au), CH$_3$CHO (~ 28 au), HCOOCH$_3$ (~ 36 au), and out to ~ 40 au for CH$_3$OH. Combining our estimate of the gas temperature probed by each iCOM with their beam-deconvolved emission sizes, we inferred the gas temperature profile of the hot corino on scales of 20-50 au in radius, finding a power-law index $q$ of approximately -1. We observed, for the first time, a chemical segregation in iCOMs of the IRAS 4A2 hot corino, and derived the gas temperature profile of its inner envelope. The derived profile is steeper than when considering a simple spherical collapsing and optically-thin envelope, hinting at a partially optically-thick envelope or a gravitationally unstable disk-like structure.

Figures

Figures reproduced from arXiv: 2501.19188 by the authors.

Figure 1
Figure 1. Dust continuum and emission of selected iCOMs transitions towards IRAS 4A2. Left: 1.3 mm dust continuum emission in colour scale and grey contours. First contours and steps are 3σ (σ = 0.6 mJy beam−1 ). The cyan star marks the IRAS 4A2 dust peak, 3h29m10s .431 (R.A.) and +31◦13′32′′ .00 (Dec.). The beam is 0′′ .20 × 0 ′′ .14 (-26◦ ). Right: Dust continuum (gray scale) overlaid with moment 0 contours maps of CH3OH 16… view at source ↗
Figure 2
Figure 2. shows the beam-deconvolved radius (in au) for each isolated transition versus the line Eu. The iCOMs display differ￾ [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Non–LTE LVG fitting results for methanol (CH3OH) with (full color) and without (shaded) considering the contribution from mm fore￾ground dust absorption (see Sec. 3.2). Left: χ 2 minimisation for the total column density NCH3OH(A-type plus E-type). Middle: Density–temperature χ 2 contour plots showing 1σ confidence level, assuming the best-fit value of NCH3OH = 2×1018 cm−2 and a source size of 0′′ .3. The best-fit s… view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: LTE population diagrams (PD) of methyl formate (HCOOCH3), ethanol (CH3CH2OH), and glycolaldehyde (CH2OHCHO). For CH2OHCHO, we complemented our dataset (blue diamonds) with the dataset of Taquet et al. (2015) (green diamonds). The results are plot￾ted with (shaded) and …
Figure 5
Figure 5. Figure 5: T–r profile of IRAS 4A2. Gas temperatures are derived account￾ing for all transitions and for the mm dust obscuration (bottom). The colored data points mark the best-fit gas temperature derived for each species as a function of the average emitting radius ¯r. The emitt…

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Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. FAUST XXVI. The dust opacity spectral indices of protostellar envelopes bridge the gap between interstellar medium and disks

    astro-ph.SR 2025-06 conditional novelty 6.0 of 10

    Envelope dust opacity spectral indices of 11 protostars (9 new) bridge the ISM and disk regimes and confirm a previously suggested correlation with envelope mass.

Reference graph

Works this paper leans on

87 extracted references · 64 canonical work pages · cited by 1 Pith paper

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archiveprefix author booktitle chapter edition editor howpublished institution eprint journal key month note number organization pages publisher school series title type volume year label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts #0 'before.all := #1 ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION n.dashify 't := "" t empty not t #1 #1 substring "-" = t #1 #2 substring "--" = not "--" * t #2 global.max substring 't := t #1 #1 substring "-" = "-" * t #2 global.max substring 't := while if t #1 #1 substring * t #2 global.max substring 't := if while FUNCTION word.in bbl.in " " * FUNCTION format....

  3. [3]

    Adams , F. C. & Shu , F. H. 1986, , 308, 836

    1986

  4. [4]

    2002, EAS Publications Series, 3, 1

    Andr\'e , P. 2002, EAS Publications Series, 3, 1

    2002

  5. [5]

    2000, in Protostars and Planets IV, ed

    Andr\'e , P., Ward-Thompson , D., & Barsony , M. 2000, in Protostars and Planets IV, ed. V. Mannings , A. P. Boss , & S. S. Russell , 59

    2000

  6. [6]

    Andrews , S. M. & Williams , J. P. 2007, The Astrophysical Journal, 659, 705

    2007

  7. [7]

    Beckwith , S. V. W., Sargent , A. I., Chini , R. S., & Guesten , R. 1990, The Astronomical Journal, 99, 924

    1990

  8. [8]

    J., Maret , S., et al

    Belloche , A., Maury , A. J., Maret , S., et al. 2020, , 635, A198

    work page 2020

Show all 87 references
  1. [9]

    M., Turrini , D., Testi , L., Marzari , F., & Polychroni , D

    Bernab \`o , L. M., Turrini , D., Testi , L., Marzari , F., & Polychroni , D. 2022, , 927, L22

    2022

  2. [10]

    2022, , 928, L3

    Bianchi , E., L \'o pez-Sepulcre , A., Ceccarelli , C., et al. 2022, , 928, L3

    2022

  3. [11]

    A., Sutton , E

    Blake , G. A., Sutton , E. C., Masson , C. R., & Phillips , T. G. 1987, The Astrophysical Journal, 315, 621

    1987

  4. [12]

    2004, The Astrophysical Journal, 615, 354

    Bottinelli , S., Ceccarelli, C., Lefloch, B., et al. 2004, The Astrophysical Journal, 615, 354

    2004

  5. [13]

    2014, , 443, 3157

    Calcutt , H., Viti , S., Codella , C., et al. 2014, , 443, 3157

    2014

  6. [14]

    & Ceccarelli , C

    Caselli , P. & Ceccarelli , C. 2012, A&ARv, 20, 56

    2012

  7. [15]

    2004, in Astronomical Society of the Pacific Conference Series, Vol

    Ceccarelli , C. 2004, in Astronomical Society of the Pacific Conference Series, Vol. 323, Star Formation in the Interstellar Medium: In Honor of David Hollenbach, ed. D. Johnstone , F. C. Adams , D. N. C. Lin , D. A. Neufeeld , & E. C. Ostriker , 195

    2004

  8. [16]

    2023, in European Conference on Laboratory Astrophysics ECLA2020

    Ceccarelli , C. 2023, in European Conference on Laboratory Astrophysics ECLA2020. The Interplay of Dust, 3--16

    2023

  9. [17]

    2017, The Astrophysical Journal, 850, 176

    Ceccarelli, C., Caselli, P., Fontani, F., et al. 2017, The Astrophysical Journal, 850, 176

    2017

  10. [18]

    2000, A&A, 355, 1129

    Ceccarelli , C., Castets, A., Caux, E., et al. 2000, A&A, 355, 1129

    2000

  11. [19]

    2023, in Astronomical Society of the Pacific Conference Series, Vol

    Ceccarelli , C., Codella , C., Balucani , N., et al. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka , Y. Aikawa , T. Muto , K. Tomida , & M. Tamura , 379

    2023

  12. [20]

    J., & Tielens , A

    Ceccarelli , C., Hollenbach , D. J., & Tielens , A. G. G. M. 1996, The Astrophysical Journal, 471, 400

    1996

  13. [21]

    Ceccarelli , C., Maret , S., Tielens , A. G. G. M., Castets , A., & Caux , E. 2003, , 410, 587

    2003

  14. [22]

    2024, , 531, 2653

    Chahine , L., Ceccarelli , C., De Simone , M., et al. 2024, , 531, 2653

    2024

  15. [23]

    2001, The Astrophysical Journal, 553, 219

    Choi , M. 2001, The Astrophysical Journal, 553, 219

    2001

  16. [24]

    2021, Front

    Codella , C., Ceccarelli , C., Chandler , C., et al. 2021, Front. astron. space sci, 8, 227

    2021

  17. [25]

    2021, , 253, 40

    Collier , B., Krueger , K., Miller , I., et al. 2021, , 253, 40

    2021

  18. [26]

    Costain , C. C. & Dowling , J. M. 1960, , 32, 158

    1960

  19. [27]

    , Alonso-Albi, T

    Crimier , Ceccarelli, C. , Alonso-Albi, T. , et al. 2010, A&A, 516, A102

    2010

  20. [28]

    2009, A&A, 506, 1229–1241

    Crimier, N., Ceccarelli, C., Lefloch, B., & Faure, A. 2009, A&A, 506, 1229–1241

    2009

  21. [29]

    2020 a , , 896, L3

    De Simone , M., Ceccarelli , C., Codella , C., et al. 2020 a , , 896, L3

    2020

  22. [30]

    2022 a , , 935, L14

    De Simone , M., Ceccarelli , C., Codella , C., et al. 2022 a , , 935, L14

    2022

  23. [31]

    2022 b , Monthly Notices of the Royal Astronomical Society, 512, 5214

    De Simone , M., Codella, C., Ceccarelli, C., et al. 2022 b , Monthly Notices of the Royal Astronomical Society, 512, 5214

    2022

  24. [32]

    2020 b , , 640, A75

    De Simone , M., Codella , C., Ceccarelli , C., et al. 2020 b , , 640, A75

    2020

  25. [33]

    2017, , 599, A121

    De Simone , M., Codella , C., Testi , L., et al. 2017, , 599, A121

    2017

  26. [34]

    2024, , 686, L13

    De Simone , M., Podio , L., Chahine , L., et al. 2024, , 686, L13

    2024

  27. [35]

    Drouin, B. J. 2017, Journal of Molecular Spectroscopy, 340, 1

    2017

  28. [36]

    L., Alexander , M

    Dubernet , M. L., Alexander , M. H., Ba , Y. A., et al. 2013, , 553, A50

    2013

  29. [37]

    P., Schlemmer, S., Schilke, P., Stutzki, J., & Müller, H

    Endres, C. P., Schlemmer, S., Schilke, P., Stutzki, J., & Müller, H. S. 2016, Journal of Molecular Spectroscopy, 327, 95, new Visions of Spectroscopic Databases, Volume II

    2016

  30. [38]

    J., Valdivia , V., et al

    Galametz , M., Maury , A. J., Valdivia , V., et al. 2019, , 632, A5

    2019

  31. [39]

    B., Izquierdo , A

    Galv \'a n-Madrid , R., Liu , H. B., Izquierdo , A. F., et al. 2018, , 868, 39

    2018

  32. [40]

    2021, A&A, 648, A66

    Gieser, C., Beuther, H., Semenov, D., et al. 2021, A&A, 648, A66

    2021

  33. [41]

    2019, , 631, A142

    Gieser , C., Semenov , D., Beuther , H., et al. 2019, , 631, A142

    2019

  34. [42]

    Goldsmith , P. F. & Langer , W. D. 1999, , 517, 209

    1999

  35. [43]

    & van Dishoeck , E

    Herbst , E. & van Dishoeck , E. F. 2009, Annual Reviews of Astronomy and Astrophysics, 47, 427

    2009

  36. [44]

    2009, Journal of Molecular Spectroscopy, 255, 32

    Ilyushin, V., Kryvda, A., & Alekseev, E. 2009, Journal of Molecular Spectroscopy, 255, 32

    2009

  37. [45]

    Jacobsen , J rgensen, J. K. , van der Wiel, M. H. D. , et al. 2018, A&A, 612, A72

    2018

  38. [46]

    2012, The Astrophysical Journal, 753, 34

    Jiménez-Serra, I., Zhang, Q., Viti, S., Martín-Pintado, J., & de Wit, W.-J. 2012, The Astrophysical Journal, 753, 34

    2012

  39. [47]

    2014, in Protostars and Planets VI, ed

    Johansen , A., Blum , J., Tanaka , H., et al. 2014, in Protostars and Planets VI, ed. H. Beuther , R. S. Klessen , C. P. Dullemond , & T. Henning , 547--570

    2014

  40. [48]

    R., Lovas, F

    Johnson, D. R., Lovas, F. J., & Kirchhoff, W. H. 2009, Journal of Physical and Chemical Reference Data, 1, 1011

    2009

  41. [49]

    J., Sams , R

    Johnson , T. J., Sams , R. L., Profeta , L. T. M., et al. 2013, Journal of Physical Chemistry A, 117, 4096

    2013

  42. [50]

    Karska , Herczeg, G. J. , van Dishoeck, E. F. , et al. 2013, A&A, 552, A141

    2013

  43. [51]

    Kirchhoff, W. H. & Johnson, D. R. 1973, Journal of Molecular Spectroscopy, 45, 159

    1973

  44. [52]

    J., & Godefroid, M

    Kleiner, I., Lovas, F. J., & Godefroid, M. 1996, Journal of Physical and Chemical Reference Data, 25, 1113

    1996

  45. [53]

    Kristensen , van Dishoeck, E. F. , Bergin, E. A. , et al. 2012, A&A, 542, A8

    2012

  46. [54]

    & Nelson, A

    Kukolich, S. & Nelson, A. 1971, Chemical Physics Letters, 11, 383

    1971

  47. [55]

    Kurland, R. J. & Wilson, E. Bright, J. 2004, The Journal of Chemical Physics, 27, 585

    2004

  48. [56]

    Lada , C. J. 1987, in Star Forming Regions, ed. M. Peimbert & J. Jugaku , Vol. 115, 1

    1987

  49. [57]

    2021, , 917, L10

    Lebreuilly , U., Hennebelle , P., Colman , T., et al. 2021, , 917, L10

    2021

  50. [58]

    2023, arXiv e-prints, arXiv:2310.19672

    Lebreuilly , U., Hennebelle , P., Colman , T., et al. 2023, arXiv e-prints, arXiv:2310.19672

    2023 arXiv

  51. [59]

    2024, , 682, A30

    Lebreuilly , U., Hennebelle , P., Colman , T., et al. 2024, , 682, A30

    2024

  52. [60]

    2022, , 937, 10

    Lee , C.-F., Codella , C., Ceccarelli , C., & L \'o pez-Sepulcre , A. 2022, , 937, 10

    2022

  53. [61]

    , Neri, R

    L\'opez-Sepulcre , Sakai, N. , Neri, R. , et al. 2017, A&A, 606, A121

    2017

  54. [62]

    F., Morbidelli , A., & Guillot , T

    Manara , C. F., Morbidelli , A., & Guillot , T. 2018, , 618, L3

    2018

  55. [63]

    Mangum, J. G. & Shirley, Y. L. 2015, Publications of the Astronomical Society of the Pacific, 127, 266

    2015

  56. [64]

    Maret , S., Ceccarelli , C., Caux , E., Tielens , A. G. G. M., & Castets , A. 2002, A&A, 395, 573

    2002

  57. [65]

    J., Gong , M., Pineda , J

    Maureira , M. J., Gong , M., Pineda , J. E., et al. 2022, , 941, L23

    2022

  58. [66]

    J., Belloche , A., Andr \'e , P., et al

    Maury , A. J., Belloche , A., Andr \'e , P., et al. 2014, , 563, L2

    2014

  59. [67]

    2014, , 567, A32

    Miotello , A., Testi , L., Lodato , G., et al. 2014, , 567, A32

    2014

  60. [68]

    2001, A&A, 365, 440

    Motte & Andr\'e . 2001, A&A, 365, 440

    2001

  61. [69]

    u ller , H. S. P., Schl \

    M \"u ller , H. S. P., Schl \"o der , F., Stutzki , J., & Winnewisser , G. 2005, Journal of Molecular Structure, 742, 215

    2005

  62. [70]

    \"O berg , K. I. & Bergin , E. A. 2021, Phys. Rep., 893, 1

    2021

  63. [71]

    2022, , 935, 136

    Okoda , Y., Oya , Y., Imai , M., et al. 2022, , 935, 136

    2022

  64. [72]

    N., Loinard , L., Dzib , S

    Ortiz-Le \'o n , G. N., Loinard , L., Dzib , S. A., et al. 2018, , 869, L33

    2018

  65. [73]

    2023, Physics and chemistry of star formation : the dynamical ISM across time and spatial scales : proceedings of the 7th Chile-Cologne-Bonn-Symposium

    Ossenkopf-Okada, V., Schaaf, R., Breloy, I., & Stutzki, J. 2023, Physics and chemistry of star formation : the dynamical ISM across time and spatial scales : proceedings of the 7th Chile-Cologne-Bonn-Symposium

    2023

  66. [74]

    C., Brauer, C

    Pearson, J. C., Brauer, C. S., & Drouin, B. J. 2008, Journal of Molecular Spectroscopy, 251, 394, special issue dedicated to the pioneering work of Drs. Edward A. Cohen and Herbert M. Pickett on spectroscopy relevant to the Earth’s atmosphere and astrophysics

    2008

  67. [75]

    1998, Journal of Quantitative Spectroscopy and Radiative Transfer, 60, 883

    Pickett, H., POYNTER, R., COHEN, E., et al. 1998, Journal of Quantitative Spectroscopy and Radiative Transfer, 60, 883

    1998

  68. [76]

    & Flower , D

    Rabli , D. & Flower , D. R. 2010, , 406, 95

    2010

  69. [77]

    L., J rgensen , J

    Sch \"o ier , F. L., J rgensen , J. K., van Dishoeck , E. F., & Blake , G. A. 2002, A&A, 390, 1001

    2002

  70. [78]

    Sheehan , P. D. & Eisner , J. A. 2018, ApJ, 857, 18

    2018

  71. [79]

    2015, The Astrophysical Journal, 804, 81

    Taquet, V., López-Sepulcre, A., Ceccarelli, C., et al. 2015, The Astrophysical Journal, 804, 81

    2015

  72. [80]

    Tielens , A. G. G. M. 2005, The Physics and Chemistry of the Interstellar Medium

    2005

  73. [81]

    2024, The accuracy of ALMA estimates of young disk radii and masses

    Tung, N.-D., Testi, L., Lebreuilly, U., et al. 2024, The accuracy of ALMA estimates of young disk radii and masses. Predicted observations from numerical simulations

    2024

  74. [82]

    Turner , B. E. 1991, The Astrophysical Journal, Supplement, 76, 617

    1991

  75. [83]

    , Rosotti, Giovanni P

    Tychoniec , L., Manara, Carlo F. , Rosotti, Giovanni P. , et al. 2020, A&A, 640, A19

    2020

  76. [84]

    van 't Hoff , M. L. R., van Dishoeck, Ewine F. , J rgensen, Jes K. , & Calcutt, Hannah . 2020, A&A, 633, A7

    2020

  77. [85]

    2008, Journal of Molecular Spectroscopy, 251

    Xu, L.-H., Fisher, J., Lees, R., et al. 2008, Journal of Molecular Spectroscopy, 251

    2008

  78. [86]

    J., Zhao, B., et al

    Zamponi, J., Maureira, M. J., Zhao, B., et al. 2021, Monthly Notices of the Royal Astronomical Society, 508, 2583–2599

    2021

  79. [87]

    F., Speagle , J

    Zucker , C., Schlafly , E. F., Speagle , J. S., et al. 2018, , 869, 83

    2018

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