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Molecular inventory of a young eruptive star's environment -- Case study of the classical FU Orionis star V1057 Cyg

T0 review · 3 major / 4 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read The first wideband millimeter census of the eruptive star V1057 Cyg finds 35 molecular species in cold 8-15 K gas, and an outflow whose 15,000-22,000 year age shows it predates the current 1969-1970 outburst.

desk verdict Useful first wideband survey of a Class II FUor, but the single-dish beam sees a parsec-scale ridge as much as the star; treat the inventory as a line-of-sight census, not a disk chemistry result. read the letter →

arxiv 2501.14553 v1 pith:BDFNSRT3 submitted 2025-01-24 astro-ph.SR astro-ph.GA

Zs. M. Szabó , A. Belloche , K. M. Menten , Y. Gong , Á. Kóspál , P. Ábrahám , W. Yang , C. J. Cyganowski
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F. Wyrowski
This is my paper · ORCID
classification astro-ph.SRastro-ph.GA
keywords FUOrionisobjectseruptiveyoungstellarmolecularlinesurveyastrochemistrycircumstellarmatteroutflowspre-main-sequencestarscomplexorganicmolecules
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 reports the first wideband millimeter-wavelength spectral line survey of a Class II FU Orionis star, sweeping roughly 72 to 263 GHz toward V1057 Cyg with the IRAM 30-m telescope and adding targeted bands with APEX. The goal is to establish what molecules survive in the environment of a mature eruptive star, one that has been in outburst only since 1969-1970 but shows the highest peak accretion rate in its class. The survey detects 35 molecular species, including simple C-, N-, O-, and S-bearing molecules, deuterated species, molecular ions, carbon chains, and the complex organics CH3OH and CH3CN, in cold gas at 8-15 K. The 12CO(3-2) map reveals a bipolar outflow whose 15,000-22,000 year dynamical age far exceeds the duration of the current eruption, and whose position-velocity structure shows knots that may record past episodic ejections. If the survey is right, a Class II FUor can harbor a richer molecular inventory than generally supposed, and its outflow archives eruption history on a timescale of tens of thousands of years.

What carries the argument

The argument rides on three tools. The first is the wideband survey itself: the EMIR receiver with FFTS backends on the IRAM 30-m telescope covering roughly 72-263 GHz at 10-36 arcsec resolution, complemented by the APEX 12-m telescope with the nFLASH230, LAsMA, and SEPIA345 receivers at 219, 227, 291, and 344 GHz. The second is the pair of LTE analysis methods, Weeds synthetic-spectrum radiative transfer and population diagrams with beam-dilution and optical-depth corrections (the $C_\tau=\tau/(1-e^{-\tau})$ factor of Goldsmith & Langer 1999), which fix the gas at 8-15 K with column densities of $1.4\times10^{12}$ to $2.8\times10^{13}$ cm$^{-2}$ for methanol, formaldehyde, HC3N, CCS, H2CS, CS, and c-C3H2. The third is the $^{12}$CO(3-2) map and its position-velocity diagram, whose discrete knots serve as the fossil record of episodic ejection; the outflow age is estimated as $t_d = R_{\rm lobe}/(v'_{\max}\tan i)$ with $i = 62^\circ$, giving 15,000 years for the blue and 22,000 years for the red lobe.

What would settle it

An interferometric map of the region at about 1 arcsec resolution would settle the association: if the northern clump at roughly 15 arcsec and the southwestern ridge at about 1.8 arcmin resolve into kinematically distinct structures whose velocities do not connect to V1057 Cyg's envelope and outflow, the molecular inventory and abundances would not describe the FUor environment. On the outflow, resolving the 12CO lobes finely enough to measure proper motions or an internal velocity gradient would test the episodic interpretation, since a continuous outflow with an apparent dynamical age of about $10^{2}$ years would count against the 15,000-22,000 year reading while the current outburst began in 1969-1970.

Watch

Extended reading notes

Core claim

On the paper's own terms, the discovery is that V1057 Cyg, a classical FUor whose pre-outburst spectrum was that of a T Tauri star and which currently has the highest observed peak accretion rate in its class, displays a chemically rich environment despite its relatively evolved state: 35 molecular species (including isotopologues) detected across an almost continuous 72-263 GHz coverage plus selected higher bands with APEX. The emission is cold, with population-diagram rotational temperatures of 8.1-14.8 K and LTE column densities of $1.4\times10^{12}$ to $2.8\times10^{13}$ cm$^{-2}$, and most integrated-intensity maps trace a parsec-scale ridge with clumps offset about 15 arcsec north and 1.8 arcmin southwest of the star. The redshifted lobe of the molecular outflow is reported for the first time, and the position-velocity diagram of $^{12}$CO(3-2) shows discrete peaks (R1, R2, B1) and weak 'fingers' that the authors read, following the episodic jet-plus-bow-shock picture, as a fossil record of past ejection events. The outflow dynamical timescale of 15,000-22,000 years (adopting the disk inclination of 62 degrees) then implies the outflow cannot have been created by the ongoing outburst alone.

Load-bearing premise

The load-bearing premise is that every detected line comes from gas physically associated with V1057 Cyg and its immediate environment, rather than from foreground or background clouds along the line of sight; with single-dish beams of 10-36 arcsec (up to about 0.5 pc at 897 pc) and most emission peaks offset from the star, this association rests mainly on the coincidence of the lines' LSR velocities with the star's systemic velocity of 4.35 km/s.

Editorial extensions

If this is right

  • The outflow's 15,000-22,000 year dynamical age shows V1057 Cyg has experienced eruptive activity long before its 1969-1970 outburst, so the current eruption is only the latest event in a series.
  • With 35 detected species, V1057 Cyg establishes a line-rich baseline for Class II FUors, showing that evolved eruptive stars can retain molecules such as CH3OH, CH3CN, HC3N, and deuterated species at 8-15 K.
  • The cold temperatures and abundances one to two orders of magnitude below post-outburst chemical model predictions are consistent with the single-dish beam blending disk, envelope, and cloud emission, so the reported values describe the roughly 30 arcsec region rather than the disk alone.
  • The pc-scale ridge with clumps to the north and southwest, coincident with the dust ridge seen at 850 micron, implies V1057 Cyg may be forming within a small cluster or filament rather than in isolation.

Reading between the lines

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

  • If the outflow age of 15,000-22,000 years is typical of FUor environments, eruptive episodes may recur on a roughly 10^4-year timescale, and the chemistry measured today would carry the cumulative imprint of many heating events rather than of one eruption; similar single-dish surveys of other FUors could test this directly.
  • The detection of N2D+ and multiple deuterated species in a Class II source points to cold, CO-depleted gas, so deuterium fractionation may mark the freeze-out regions that future interferometers should target to constrain snow-line positions.
  • Because most integrated-intensity peaks sit offset from the star, the reported column densities are probably lower limits for the true envelope abundances; a testable consequence is that interferometric observations will recover warmer, denser emission on sub-arcsecond scales.
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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 / 4 minor

Summary. This paper reports the first wideband millimetre spectral line survey of the classical FU Orionis star V1057 Cyg. Using the IRAM 30-m telescope over 72–263 GHz and APEX at selected bands around 219, 227, 291, and 344 GHz, the authors detect 35 molecular species (including isotopologues) under a 3-sigma threshold with at least two transitions per species, identify lines against CDMS/JPL catalogues, and map several molecules. LTE Weeds modelling and population diagrams for CH3OH, H2CO, CCS, HC3N, H2CS, CS, and c-C3H2 yield rotational temperatures of 8.1–14.8 K and column densities of 1.4e12–2.8e13 cm^-2. The 12CO(3–2) map reveals a bipolar outflow with a dynamical timescale of 15,000–22,000 yr at the adopted inclination, and a position-velocity diagram shows knots and finger-like features interpreted as possible episodic ejection. The paper concludes that V1057 Cyg has a rich molecular inventory for a Class II FUor and motivates interferometric follow-up.

Significance. The observational dataset is a valuable community resource: it is the first near-continuous wideband millimetre survey of a Class II FUor, with a transparent detection threshold, catalogue-based line identification, and several explicitly acknowledged limitations. If the detected emission can be confidently associated with V1057 Cyg's circumstellar environment, the inventory of 35 species, including deuterated species, molecular ions, and complex organic molecules, would be an important benchmark for the chemical evolution of eruptive young stars and a useful complement to studies of younger FUors such as V883 Ori and L1551 IRS5. The outflow dynamical timescale and the evidence for a parsec-scale ridge provide concrete targets for interferometric follow-up. The significance is therefore contingent on resolving the source-association and LTE-modelling caveats identified below.

major comments (3)
  1. [3.2/3.3/3.4/4.4] The central claim that V1057 Cyg 'demonstrates rich chemistry for its evolutionary state' is not yet supported for the FUor itself because the large single-dish beams (10–36 arcsec, i.e., roughly 0.04–0.5 pc at 897 pc) blend disk, envelope, and extended cloud emission. The integrated intensity maps in Fig. 3 show that HCN, HNC, HC3N, HCO+, and N2H+ peak about 15 arcsec north and about 1.8 arcmin southwest, tracing a parsec-scale ridge, while the paper itself states in Sect. 3.4 that the single-dish data 'are likely capturing several components blended together, including disk, envelope, and surrounding cloud emission' and in Sect. 4.4 that 'it is uncertain what fraction of the measured flux is related to a more compact disk around the source and what is related to the extended ridge.' LSR-velocity agreement in Sect. 3.2 demonstrates common cloud membership, not co-spatiality with the star. A revision should either restrict the inventory and abundance claims to the V1057 Cyg line-of-sight and cloud environment, with comparisons made at matched spatial scales, or supply on-source versus off-source spectra and an explicit estimate of the ridge contribution at the stellar position.
  2. [3.4/3.5/Table 4] The quantitative LTE results for CH3OH and H2CS are used in Table 4 and in the abundance comparison with the Molyarova et al. (2018) models, but the manuscript admits in Sect. 3.4 that the LTE synthetic spectra do not reproduce some methanol transitions and in Sect. 3.5 that the best-fit Weeds model for CH3OH 'underestimates the line strength.' H2CS has Trot = 14.8 ± 9.5 K and a column density of (1.4 ± 1.5) x 10^12 cm^-2, so its formal uncertainty is larger than the quoted value. Because non-LTE modelling is explicitly out of scope, these abundances should be presented as order-of-magnitude estimates or upper limits, with systematic uncertainties from assumed source size and excitation propagated into the comparisons with chemical models.
  3. [3.1/Table 3/Table A.1] The detection criterion in Sect. 3.1 requires at least two detected transitions per molecule, but HDCO is listed in Table 3 as a detected species while Table A.1 appears to contain only a single secure HDCO transition (134.284 GHz). This is an internal inconsistency that affects the headline count of 35 species. Please either identify a second secure HDCO transition or reclassify HDCO as tentative, and apply the same multiplicity check to every species in Table 3.
minor comments (4)
  1. [Abstract] The sentence 'These maps a 12CO (3–2) position-velocity diagram provide insight into the past outburst activity of the source' is garbled and should be rewritten.
  2. [Table 6] Table 6 lists HC5N as detected toward V1057 Cyg, but HC5N does not appear in Table 3, and it lists CH3CCH toward V883 Ori without textual support in Sect. 4.3; please reconcile the table with the text and with the actual detections.
  3. [Throughout] The notation '3lsr' and 'p-3 diagram' appears repeatedly and should be typeset as v_LSR and p-v diagram, respectively, for consistency with standard usage.
  4. [Section 4.2/Fig. 6] The interpretation of the knots R1, R2, and B1 and the 'fingers' in the 12CO position-velocity diagram as evidence of episodic ejection should be framed more cautiously, since the features are seen with a large single-dish beam and without independent kinematic decomposition; the robust statement is the outflow dynamical timescale exceeding the current outburst duration.

Circularity Check

0 steps flagged · score 0.0 of 10

No circular reasoning found; the molecular parameters are fits presented as estimates and the central inventory and outflow claims rest on independent observations and external benchmarks.

full rationale

The paper does not present any derived quantity as a prediction that was secretly used as an input. The LTE (Weeds) models and population diagrams are explicitly described as providing 'initial estimates' (Sect. 3.4), with the source size, temperature, and column density adjusted until the best fit was achieved; the later statement that the two methods agree is therefore a calibration check, not an independent confirmation, and it is not used to support the central claims. The central results—35 detected species, rotational temperatures of 8–15 K, column densities of 1.4e12–2.8e13 cm^-2, and outflow dynamical times of 15,000–22,000 years—rest on line identifications against the CDMS and JPL catalogs, Gaussian fits to the observed spectra, and geometric measurements of the 12CO lobe extents and velocities. The systemic velocity (4.35 km/s) is adopted from Szabó et al. (2023a), a same-group ammonia observation, but this is a published, externally falsifiable measurement used as an input rather than derived from the present survey, so it does not make the argument circular. Likewise, the 897 pc distance (Bailer-Jones et al. 2018), the 62-degree inclination (Liu et al. 2018; Szabó et al. 2021), and the less-than-a-century outburst duration (Szabó et al. 2021) are prior observational constraints. Abundances are compared against external chemical models (Molyarova et al. 2018; Rab et al. 2017) and against other FUors, and the paper explicitly states that no clear chemical imprint of the outburst is seen on the scales traced by the single-dish data. The unresolved spatial-association issue, namely that the 10–36 arcsec beams and the offset peaks at about 15 arcsec and 1.8 arcmin could include foreground or surrounding cloud emission, is an acknowledged physical limitation that the authors discuss in Sects. 3.4 and 4.4; if foreground gas dominates, the inventory would be misattributed rather than circular. No equation in the paper defines a result in terms of the same result it is claimed to explain, and no load-bearing argument reduces to a self-citation chain.

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

The quantitative results (column densities, temperatures, abundances, outflow age) rest on a small set of modeling choices: LTE, a 25-30 arcsec emitting region, an H2 column density from Herschel SED fitting, and an adopted disk inclination for the outflow. The line inventory itself is independent of these choices. No new physical entities are introduced.

free parameters (4)
  • Source size for LTE analysis = 25 arcsec (HC3N), 30 arcsec (other molecules)
    Chosen by exploring 1.5-35 arcsec and finding best fits (Sect. 3.4); directly sets the beam dilution correction and scales all column densities and abundances.
  • Rotational temperature (per molecule) = 8.1-14.8 K
    Fitted from population diagrams and Weeds models (Table 4); presented as estimates, not independent predictions.
  • Total column density (per molecule) = 1.4e12 to 2.8e13 cm^-2
    Fitted from population diagrams and Weeds models (Table 4); affected by the assumed source size.
  • H2 column density for abundance normalization = 1.14-1.21e22 cm^-2
    Derived from Herschel SED fitting at 25-30 arcsec resolution (Sect. 3.4); used to convert molecular column densities to abundances, with about 10% uncertainty.
assumptions (4)
  • domain assumption Local thermodynamic equilibrium (LTE) for all modeled molecules
    Invoked in Sect. 3.4 for Weeds modeling and population diagrams; the paper notes CH3OH lines are not well matched and non-LTE modeling is beyond the scope of the work.
  • domain assumption Detected line emission is associated with V1057 Cyg and its environment
    Argued from LSR velocity coincidence in Sect. 3.2, but maps show peaks offset from the star and a parsec-scale ridge, so foreground or background contamination is not fully excluded.
  • domain assumption Spectroscopic rest frequencies from CDMS and JPL are accurate
    All line identifications rely on CDMS (Müller et al. 2005) and JPL (Pickett et al. 1998) catalogues without independent verification.
  • domain assumption Ballistic outflow age formula with adopted inclination
    Dynamical times use td = R_lobe / (v'_max tan i) with inclination adopted from literature (62 degrees, Liu et al. 2018; Szabó et al. 2021); Sect. 4.2 and Table 5.

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Cite this review

Pith. "Pith review of Molecular inventory of a young eruptive star's environment -- Case study of the classical FU Orionis star V1057 Cyg." pith.science (2026). https://pith.science/paper/BDFNSRT3

@misc{pith2026250114553,
  author       = {Pith},
  title        = {Pith review of: Molecular inventory of a young eruptive star's environment -- Case study of the classical FU Orionis star V1057 Cyg},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/BDFNSRT3}},
  note         = {Machine review of arXiv:2501.14553}
}
abstract

Studying accretion-driven episodic outbursts in YSOs is key to understanding the later stages of star and planet formation. FU Orionis-type objects form a YSO subclass, distinguished by rapid, multi-magnitude increases in brightness at optical and near-infrared wavelengths. These outbursts may significantly impact the chemistry and molecular composition around eruptive stars. However, no comprehensive millimeter-wavelength line survey exists for more evolved (Class II) sources, unlike optical and near-infrared coverage. We conducted the first wideband millimeter spectral line survey of V1057 Cyg, a low-mass eruptive FUor with the highest observed peak accretion rate in its class. Using the IRAM 30-m telescope, we surveyed the 72-263 GHz range and complemented this with targeted spectra at 219, 227, 291, and 344 GHz with the APEX 12-m telescope. We conducted radiative transfer and population diagram analyses to get first estimates of the excitation temperatures and column densities. Several molecular species trace large-scale structures, and the position-velocity diagram of $^{12}$CO suggest episodic outburst activity, with outflow dynamical timescales on the order of tens of thousands of years. We identified simple molecules (C-, N-, O-, and S-bearing), deuterated species, molecular ions, and complex organic molecules. With over 30 molecular species (including isotopologues) detected, V1057 Cyg demonstrates rich chemistry for its evolutionary state, compared to other younger (Class 0/I) FUors. V1057 Cyg is a good candidate for future interferometric studies to resolve emission structures, to possibly constrain molecular freeze-out, and detect water and complex organic molecules. Our results highlight the importance of millimeter line surveys in complementing optical/near-infrared studies, improving statistics on molecular inventories in eruptive stars and their environments.

Figures

Figures reproduced from arXiv: 2501.14553 by the authors.

Figure 1
Figure 1. Complete spectrum of V1057 Cyg obtained with the IRAM 30-m telescope, with selected lines labelled with the name of [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Selection of lines detected with the IRAM 30-m telescope, labelled with the molecular species name in blue; the other lines [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Integrated intensity maps of molecular lines obtained with the IRAM 30-m telescope. The red cross marks the position of [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figures from the paper (4 more)
Figure 3
Figure 3. Figure 3: Continued. 3.5. Population diagrams and abundances The transitions used for the population diagrams are well iso￾lated in the spectrum of V1057 Cyg, therefore it was not neces￾sary to discard any transitions owing to contamination by other species (a potential issue in…
Figure 4
Figure 4. Figure 4: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p010_4.png]
Figure 6
Figure 6. Figure 6: Position-velocity (p-3) diagram along the yellow line shown in [PITH_FULL_IMAGE:figures/full_fig_p011_6.png]
Figure 7
Figure 7. Figure 7: Population diagrams of: (a) CH3OH; (b) H2CO; (c) CCS; (d) HC3N, (e) H2CS; (f) CS; (g) c-C3H2. The black points (green in the case of CH3OH) represent the observations while the red points correspond to the Weeds synthetic spectra computed with the parameters given in …

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Works this paper leans on

120 extracted references · 56 canonical work pages

  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]

    C., Lada , C

    Adams , F. C., Lada , C. J., & Shu , F. H. 1987, , 312, 788

    1987

  4. [4]

    2013, , 766, 8

    Akimkin , V., Zhukovska , S., Wiebe , D., et al. 2013, , 766, 8

    2013

  5. [5]

    2010, , 518, L102

    Andr \'e , P., Men'shchikov , A., Bontemps , S., et al. 2010, , 518, L102

    2010

  6. [6]

    2023, , 677, L17

    Andreu , A., Coutens , A., Cruz-S \'a enz de Miera , F., et al. 2023, , 677, L17

    2023

  7. [7]

    Arce , H. G. & Goodman , A. A. 2001, , 551, L171

    2001

  8. [8]

    M., et al

    Audard , M., \'A brah \'a m , P., Dunham , M. M., et al. 2014, in Protostars and Planets VI, ed. H. Beuther , R. S. Klessen , C. P. Dullemond , & T. Henning , 387

    2014

Show all 120 references
  1. [9]

    Bailer-Jones , C. A. L., Rybizki , J., Fouesneau , M., Mantelet , G., & Andrae , R. 2018 a , , 156, 58

    2018

  2. [10]

    Bailer-Jones , C. A. L., Rybizki , J., Fouesneau , M., Mantelet , G., & Andrae , R. 2018 b , VizieR Online Data Catalog, I/347

    2018

  3. [11]

    & Menten , K

    Batrla , W. & Menten , K. M. 1988, , 329, L117

    1988

  4. [12]

    Bechis , K. P. & Lo , K. Y. 1975, , 201, 118

    1975

  5. [13]

    T., M \"u ller , H

    Belloche , A., Garrod , R. T., M \"u ller , H. S. P., et al. 2009, , 499, 215

    2009

  6. [14]

    Belloche , A., M \"u ller , H. S. P., Garrod , R. T., & Menten , K. M. 2016, , 587, A91

    2016

  7. [15]

    Belloche , A., M \"u ller , H. S. P., Menten , K. M., Schilke , P., & Comito , C. 2013, , 559, A47

    2013

  8. [16]

    K., et al

    Beuther , H., Schilke , P., Sridharan , T. K., et al. 2002, , 383, 892

    2002

  9. [17]

    J., Ceccarelli , C., et al

    Bianchi , E., Chandler , C. J., Ceccarelli , C., et al. 2020, , 498, L87

    2020

  10. [18]

    L., Contreras , Y., Dawson , J

    Breen , S. L., Contreras , Y., Dawson , J. R., et al. 2019, , 484, 5072

    2019

  11. [19]

    A., Belloche , A., Garrod , R

    Busch , L. A., Belloche , A., Garrod , R. T., M \"u ller , H. S. P., & Menten , K. M. 2024, , 681, A104

    2024

  12. [20]

    M., Evans , Neal J., I., Lester , D

    Butner , H. M., Evans , Neal J., I., Lester , D. F., Levreault , R. M., & Strom , S. E. 1991, , 376, 636

    1991

  13. [21]

    K., Bergin , E

    Calahan , J. K., Bergin , E. A., van't Hoff , M., et al. 2024 a , , 967, 158

    2024

  14. [22]

    K., Bergin , E

    Calahan , J. K., Bergin , E. A., van't Hoff , M., et al. 2024 b , , 967, 158

    2024

  15. [23]

    2012, , 538, A89

    Carter , M., Lazareff , B., Maier , D., et al. 2012, , 538, A89

    2012

  16. [24]

    2017, , 850, 176

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

    2017

  17. [25]

    2022, arXiv e-prints, arXiv:2206.13270

    Ceccarelli , C., Codella , C., Balucani , N., et al. 2022, arXiv e-prints, arXiv:2206.13270

    2022 arXiv

  18. [26]

    P., Shen , Z.-Q., Titmarsh , A., & Gan , C.-G

    Chen , X., Ellingsen , S. P., Shen , Z.-Q., Titmarsh , A., & Gan , C.-G. 2011, , 196, 9

    2011

  19. [27]

    A., Casassus , S., Tobin , J., et al

    Cieza , L. A., Casassus , S., Tobin , J., et al. 2016, , 535, 258

    2016

  20. [28]

    J., Lodato , G., Melnikov , S

    Clarke , C. J., Lodato , G., Melnikov , S. Y., & Ibrahimov , M. A. 2005, , 361, 942

    2005

  21. [29]

    Connelley , M. S. & Reipurth , B. 2018, , 861, 145

    2018

  22. [30]

    2023, , 945, 80

    Cruz-S \'a enz de Miera , F., K \'o sp \'a l , \'A ., \'A brah \'a m , P., et al. 2023, , 945, 80

    2023

  23. [31]

    2014, in Protostars and Planets VI, ed

    Dutrey , A., Semenov , D., Chapillon , E., et al. 2014, in Protostars and Planets VI, ed. H. Beuther , R. S. Klessen , C. P. Dullemond , & T. Henning , 317--338

    2014

  24. [32]

    P., Schlemmer , S., Schilke , P., Stutzki , J., & M \"u ller , H

    Endres , C. P., Schlemmer , S., Schilke , P., Stutzki , J., & M \"u ller , H. S. P. 2016, Journal of Molecular Spectroscopy, 327, 95

    2016

  25. [33]

    M., Hartmann , L., & Kenyon , S

    Evans , Neal J., I., Balkum , S., Levreault , R. M., Hartmann , L., & Kenyon , S. 1994, , 424, 793

    1994

  26. [34]

    R., & Brinch , C

    Feh \'e r , O., K \'o sp \'a l , \'A ., \'A brah \'a m , P., Hogerheijde , M. R., & Brinch , C. 2017, , 607, A39

    2017

  27. [35]

    J., Hillenbrand , L

    Fischer , W. J., Hillenbrand , L. A., Herczeg , G. J., et al. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Astronomical Society of the Pacific Conference Series, ed. S. Inutsuka , Y. Aikawa , T. Muto , K. Tomida , & M. Tamura , 355

    2023

  28. [36]

    Fridlund , C. V. M., Bergman , P., White , G. J., Pilbratt , G. L., & Tauber , J. A. 2002, , 382, 573

    2002

  29. [37]

    J., Ali , B., et al

    Furlan , E., Fischer , W. J., Ali , B., et al. 2016, , 224, 5

    2016

  30. [38]

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

    1999

  31. [39]

    D., Evans , Neal J., I., K \'o sp \'a l , \'A ., et al

    Green , J. D., Evans , Neal J., I., K \'o sp \'a l , \'A ., et al. 2013, , 772, 117

    2013

  32. [40]

    D., Hartmann , L., Calvet , N., et al

    Green , J. D., Hartmann , L., Calvet , N., et al. 2006, , 648, 1099

    2006

  33. [41]

    A ., Schilke , P., et al

    G \"u sten , R., Nyman , L. A ., Schilke , P., et al. 2006, , 454, L13

    2006

  34. [42]

    E., Heitsch , F., et al

    Hacar , A., Clark , S. E., Heitsch , F., 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 , 153

    2023

  35. [43]

    2017, , 606, A123

    Hacar , A., Tafalla , M., & Alves , J. 2017, , 606, A123

    2017

  36. [44]

    S., P \'e rez , S., Gonzalez-Ruilova , C., et al

    Hales , A. S., P \'e rez , S., Gonzalez-Ruilova , C., et al. 2020, , 900, 7

    2020

  37. [45]

    & Kenyon , S

    Hartmann , L. & Kenyon , S. J. 1996, , 34, 207

    1996

  38. [46]

    Herbig , G. H. 1966, Vistas in Astronomy, 8, 109

    1966

  39. [47]

    Herbig , G. H. 1977, , 217, 693

    1977

  40. [48]

    Herbig , G. H. 2009, , 138, 448

    2009

  41. [49]

    H., Petrov , P

    Herbig , G. H., Petrov , P. P., & Duemmler , R. 2003, , 595, 384

    2003

  42. [50]

    & van Dishoeck , E

    Herbst , E. & van Dishoeck , E. F. 2009, , 47, 427

    2009

  43. [51]

    A., Contreras Pe \ n a , C., Morrell , S., et al

    Hillenbrand , L. A., Contreras Pe \ n a , C., Morrell , S., et al. 2018, , 869, 146

    2018

  44. [52]

    1992, , 394, 539

    Hirahara , Y., Suzuki , H., Yamamoto , S., et al. 1992, , 394, 539

    1992

  45. [53]

    R., van Dishoeck , E

    Hogerheijde , M. R., van Dishoeck , E. F., Salverda , J. M., & Blake , G. A. 1999, , 513, 350

    1999

  46. [54]

    K., Belloche , A., & Garrod , R

    J rgensen , J. K., Belloche , A., & Garrod , R. T. 2020, , 58, 727

    2020

  47. [55]

    Kenyon , S. J. & Hartmann , L. W. 1991, , 383, 664

    1991

  48. [56]

    D., Kr \"a mer , I., et al

    Klein , B., Philipp , S. D., Kr \"a mer , I., et al. 2006, , 454, L29

    2006

  49. [57]

    2011, , 535, A125

    K \'o sp \'a l , \'A . 2011, , 535, A125

    2011

  50. [58]

    A., et al

    K \'o sp \'a l , \'A ., \'A brah \'a m , P., Acosta-Pulido , J. A., et al. 2016, , 596, A52

    2016

  51. [59]

    2017 a , , 836, 226

    K \'o sp \'a l , \'A ., \'A brah \'a m , P., Csengeri , T., et al. 2017 a , , 836, 226

    2017

  52. [60]

    2017 b , , 597, L10

    K \'o sp \'a l , \'A ., \'A brah \'a m , P., Westhues , C., & Haas , M. 2017 b , , 597, L10

    2017

  53. [61]

    M., \' A brah \' a m, P., et al

    K \' o sp \' a l, \' A ., Szab \' o , Z. M., \' A brah \' a m, P., et al. 2020, The Astrophysical Journal, 889, 148

    2020

  54. [62]

    2016, , 462, L61

    Kraus , S., Caratti o Garatti , A., Garcia-Lopez , R., et al. 2016, , 462, L61

    2016

  55. [63]

    D., Velusamy , T., Kuiper , T

    Langer , W. D., Velusamy , T., Kuiper , T. B. H., et al. 1995, , 453, 293

    1995

  56. [64]

    2024, , 966, 119

    Lee , J.-E., Kim , C.-H., Lee , S., et al. 2024, , 966, 119

    2024

  57. [65]

    2019, Nature Astronomy, 3, 314

    Lee , J.-E., Lee , S., Baek , G., et al. 2019, Nature Astronomy, 3, 314

    2019

  58. [66]

    Leemker , M., van't Hoff , M. L. R., Trapman , L., et al. 2021, , 646, A3

    2021

  59. [67]

    Levreault , R. M. 1988, , 67, 283

    1988

  60. [68]

    B., Dunham , M

    Liu , H. B., Dunham , M. M., Pascucci , I., et al. 2018, , 612, A54

    2018

  61. [69]

    Lo , K. Y. & Bechis , K. P. 1973, , 185, L71

    1973

  62. [70]

    Lo , K. Y. & Bechis , K. P. 1974, in Bulletin of the American Astronomical Society, Vol. 6, 221

    1974

  63. [71]

    W., Mundy , L

    Looney , L. W., Mundy , L. G., & Welch , W. J. 1997, , 484, L157

    1997

  64. [72]

    Y., Nikogossian , E

    Magakian , T. Y., Nikogossian , E. H., Movsessian , T., et al. 2013, , 432, 2685

    2013

  65. [73]

    2024, , 687, A195

    Marchand , P., Coutens , A., Scigliuto , J., et al. 2024, , 687, A195

    2024

  66. [74]

    2011, , 526, A47

    Maret , S., Hily-Blant , P., Pety , J., Bardeau , S., & Reynier , E. 2011, , 526, A47

    2011

  67. [75]

    A., & Sargent , A

    McMuldroch , S., Blake , G. A., & Sargent , A. I. 1995, , 110, 354

    1995

  68. [76]

    2022, , 659, A67

    Mercimek , S., Codella , C., Podio , L., et al. 2022, , 659, A67

    2022

  69. [77]

    2018, , 866, 46

    Molyarova , T., Akimkin , V., Semenov , D., et al. 2018, , 866, 46

    2018

  70. [78]

    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

  71. [79]

    M \"u ller , H. S. P., Thorwirth , S., Roth , D. A., & Winnewisser , G. 2001, , 370, L49

    2001

  72. [80]

    2022, , 515, 1774

    Nagy , Z., \'A brah \'a m , P., K \'o sp \'a l , \'A ., et al. 2022, , 515, 1774

    2022

  73. [81]

    2023, , 524, 3344

    Nagy , Z., Park , S., \'A brah \'a m , P., et al. 2023, , 524, 3344

    2023

  74. [82]

    H., Zurlo , A., P \'e rez , S., et al

    Nogueira , P. H., Zurlo , A., P \'e rez , S., et al. 2023, , 523, 4970

    2023

  75. [83]

    2020, , 900, 36

    Park , S., Lee , J.-E., Pyo , T.-S., et al. 2020, , 900, 36

    2020

  76. [84]

    2005, in SF2A-2005: Semaine de l'Astrophysique Francaise, ed

    Pety , J. 2005, in SF2A-2005: Semaine de l'Astrophysique Francaise, ed. F. Casoli , T. Contini , J. M. Hameury , & L. Pagani , 721

    2005

  77. [85]

    M., Poynter , R

    Pickett , H. M., Poynter , R. L., Cohen , E. A., et al. 1998, , 60, 883

    1998

  78. [86]

    Plambeck , R. L. & Menten , K. M. 1990, , 364, 555

    1990

  79. [87]

    L., Arce , H

    Plunkett , A. L., Arce , H. G., Mardones , D., et al. 2015, , 527, 70

    2015

  80. [88]

    P., Henning , T., Bouwman , J., Linz , H., & Lahuis , F

    Quanz , S. P., Henning , T., Bouwman , J., Linz , H., & Lahuis , F. 2007, , 658, 487

    2007

  81. [89]

    2017, , 604, A15

    Rab , C., Elbakyan , V., Vorobyov , E., et al. 2017, , 604, A15

    2017

  82. [90]

    A., Williams , J

    Ru \' z-Rodr \' guez , D., Cieza , L. A., Williams , J. P., et al. 2017 a , , 468, 3266

    2017

  83. [91]

    A., Williams , J

    Ru \' z-Rodr \' guez , D., Cieza , L. A., Williams , J. P., et al. 2017 b , , 466, 3519

    2017

  84. [92]

    A., Williams , J

    Ru \' z-Rodr \' guez , D. A., Williams , J. P., Kastner , J. H., et al. 2022, , 515, 2646

    2022

  85. [93]

    & Weintraub , D

    Sandell , G. & Weintraub , D. A. 2001, , 134, 115

    2001

  86. [94]

    P., et al

    Schmalzl , M., Kainulainen , J., Quanz , S. P., et al. 2010, , 725, 1327

    2010

  87. [95]

    Shirley , Y. L. 2015, , 127, 299

    2015

  88. [96]

    O., J rgensen , J

    St \"a uber , P., Benz , A. O., J rgensen , J. K., et al. 2007, , 466, 977

    2007

  89. [97]

    M., Gong , Y., Menten , K

    Szab \'o , Z. M., Gong , Y., Menten , K. M., et al. 2023 a , , 672, A158

    2023

  90. [98]

    M., Gong , Y., Yang , W., et al

    Szab \'o , Z. M., Gong , Y., Yang , W., et al. 2023 b , , 674, A202

    2023

  91. [99]

    M., K \'o sp \'a l , \'A ., \'A brah \'a m , P., et al

    Szab \'o , Z. M., K \'o sp \'a l , \'A ., \'A brah \'a m , P., et al. 2021, , 917, 80

    2021

  92. [100]

    M., K \'o sp \'a l , \'A ., \'A brah \'a m , P., et al

    Szab \'o , Z. M., K \'o sp \'a l , \'A ., \'A brah \'a m , P., et al. 2022, , 936, 64

    2022

  93. [101]

    2020, , 899, 130

    Szegedi-Elek , E., \'A brah \'a m , P., Wyrzykowski , ., et al. 2020, , 899, 130

    2020

  94. [102]

    2018, , 155, 101

    Takagi , Y., Honda , S., Arai , A., et al. 2018, , 155, 101

    2018

  95. [103]

    J., van't Hoff , M

    Tobin , J. J., van't Hoff , M. L. R., Leemker , M., et al. 2023, , 615, 227

    2023

  96. [104]

    van 't Hoff , M. L. R., Tobin , J. J., Trapman , L., et al. 2018, , 864, L23

    2018

  97. [105]

    2017, , 597, A25

    Velilla Prieto , L., S \'a nchez Contreras , C., Cernicharo , J., et al. 2017, , 597, A25

    2017

  98. [106]

    A., & J rgensen , J

    Visser , R., Bergin , E. A., & J rgensen , J. K. 2015, , 577, A102

    2015

  99. [107]

    1954, , 35, 74

    Wachmann , A. 1954, , 35, 74

    1954

  100. [108]

    1971 a , , 12, 312

    Welin , G. 1971 a , , 12, 312

    1971

  101. [109]

    1971 b , Information Bulletin on Variable Stars, 581, 1

    Welin , G. 1971 b , Information Bulletin on Variable Stars, 581, 1

    1971

  102. [110]

    C., Mac \' as , E., et al

    Wendeborn , J., Espaillat , C. C., Mac \' as , E., et al. 2020, , 897, 54

    2020

  103. [111]

    J., Fridlund , C

    White , G. J., Fridlund , C. W. M., Bergman , P., et al. 2006, , 651, L41

    2006

  104. [112]

    M., & Booth , R

    Winnberg , A., Graham , D., Walmsley , C. M., & Booth , R. S. 1981, , 93, 79

    1981

  105. [113]

    Woitke , P., Kamp , I., & Thi , W. F. 2009, , 501, 383

    2009

  106. [114]

    2016, , 586, A103

    Woitke , P., Min , M., Pinte , C., et al. 2016, , 586, A103

    2016

  107. [115]

    2017, Introduction to Astrochemistry: Chemical Evolution from Interstellar Clouds to Star and Planet Formation

    Yamamoto , S. 2017, Introduction to Astrochemistry: Chemical Evolution from Interstellar Clouds to Star and Planet Formation

    2017

  108. [116]

    2024, , 167, 66

    Yamato , Y., Notsu , S., Aikawa , Y., et al. 2024, , 167, 66

    2024

  109. [117]

    M., et al

    Yang , W., Gong , Y., Menten , K. M., et al. 2023, , 675, A112

    2023

  110. [118]

    2024, , 969, L6

    Zhou , W., Chen , Z., Jiang , Z., Feng , H., & Jiang , Y. 2024, , 969, L6

    2024

  111. [119]

    S., Schlafly , E

    Zucker , C., Speagle , J. S., Schlafly , E. F., et al. 2019, , 879, 125

    2019

  112. [120]

    2024, , 527, 7652

    Zwicky , L., Molyarova , T., Akimkin , V., et al. 2024, , 527, 7652

    2024

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