pith. sign in

arxiv: 2606.31746 · v1 · pith:HYYUIXJ4new · submitted 2026-06-30 · 🌌 astro-ph.SR

The CepA disk-outflow system at <=0.2'' or <=100au resolution

H. Beuther , C. Gieser , V. Aberham , J.M. Winters , R. Neri , A. Ahmadi , R. Kuiper , Th. Henning
show 16 more authors
H. Linz T. M\"oller V. Elbakyan L. Moscadelli D. Semenov J. Urquhart P. Klaassen M. Beltran \'A. S\'anchez-Monge T. Peters R. Galvan-Madrid S. Leurini S. Lumsden R.E. Pudritz A. Palau H. Zinnecker
This is my paper

Pith reviewed 2026-07-01 02:45 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords high-mass star formationaccretion disksfragmentationoutflowsCepheus Amillimeter interferometryToomre stability
0
0 comments X

The pith

High-resolution millimeter data resolve the CepA disk into multiple sub-structures consistent with fragments in an almost edge-on geometry that drive several outflows.

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

The observations map the CepA HW2 system at 1.3 mm with 0.2 arcsecond or 100 au resolution. The continuum image breaks the central source into several distinct peaks, while line emission traces both the disk kinematics and multiple bipolar outflows. A Toomre Q analysis using CH3CN temperatures and densities together with direct comparison to radiation-hydrodynamic simulations indicates the peaks are consistent with fragments inside a nearly edge-on disk. Detection of a second outflow pair from the same central position implies the protostar is at least a binary. The results show that both fragmentation and outflow multiplicity operate on the scales of the inner accretion disk.

Core claim

The mm continuum emission resolves the central disk candidate into several sub-structures. Conducting a Toomre Q stability analysis based on CH3CN and continuum data, and a comparison to 3D radiation hydrodynamic simulations shows that the data are consistent with an almost edge-on disk where the observed sub-structures may represent fragments within the disk. The CO and SiO spectral line data confirm a second bipolar outflow emanating from the central peak position, indicating that this central peak should host at least a binary if not even a higher order multiple system.

What carries the argument

NOEMA long-baseline 1.3 mm continuum and spectral-line imaging at <=100 au resolution combined with Toomre Q stability maps derived from CH3CN and dust data.

If this is right

  • Fragmentation can occur inside the inner accretion disks of high-mass protostars on scales below 100 au.
  • A single central peak can launch multiple distinct outflows when it contains a multiple stellar system.
  • CH3CN emission receives significant contributions from outflow shocks, limiting its use as a pure disk tracer.
  • High-mass star formation proceeds with multiplicity already established at the smallest disk scales.

Where Pith is reading between the lines

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

  • Similar disk-fragmentation signatures may appear in other nearby high-mass candidates once observed at comparable linear resolution.
  • The observed outflow multiplicity supplies an indirect but testable route to counting companions before they are spatially resolved.
  • If the fragments continue to accrete, they could produce a small cluster rather than a single high-mass star.

Load-bearing premise

The continuum sub-structures are physical fragments inside a single edge-on disk rather than separate objects or imaging artifacts.

What would settle it

Higher-resolution kinematic maps showing the sub-structures do not rotate with the disk velocity field or Toomre Q values remaining above unity across the entire structure.

Figures

Figures reproduced from arXiv: 2606.31746 by A. Ahmadi, A. Palau, \'A. S\'anchez-Monge, C. Gieser, D. Semenov, H. Beuther, H. Linz, H. Zinnecker, J.M. Winters, J. Urquhart, L. Moscadelli, M. Beltran, P. Klaassen, R.E. Pudritz, R. Galvan-Madrid, R. Kuiper, R. Neri, S. Leurini, S. Lumsden, Th. Henning, T. M\"oller, T. Peters, V. Aberham, V. Elbakyan.

Figure 1
Figure 1. Figure 1: Lower and upper sideband continuum-subtracted average spectra from the central extended disk-like structure with a radius [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Continuum data for CepA HW2. The left panel shows the large-scale overview of the 1.3 mm continuum data, and the [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: Optical depth τν map at 1.3 mm. The color scale shows the τν map and the contours outline the 1.3 mm continuum emis￾sion in 4σ steps. presents an intensity cut along its major axis as outlined in the right panel of [PITH_FULL_IMAGE:figures/full_fig_p005_4.png] view at source ↗
Figure 3
Figure 3. Figure 3: Intensity cut along the 1.3 mm continuum map as outlined [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Integrated intensity maps for selected molecules (integration range typically [ [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Overlay of CH3CN, 1.3 mm and outflow data. All three panels show in color and contours the CH3CN(123 − 113) first moment and 1.3 mm continuum maps. Contour levels are from 4σ to 20σ in 4σ steps and then continue in 100σ steps. The blue and red contours in the left and middle panel outline the east-west outflow in CO(2–1) (blue [-50,-30] km s−1 , red [20,40] km s−1 ) and SiO(5–4) (blue [-50,-30] km s−1 , re… view at source ↗
Figure 7
Figure 7. Figure 7: Position-velocity cuts along the line shown in [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Rotation temperature map from CH3CN(12k − 11k). The color scale shows the temperature map and the contours outline the 1.3 mm continuum emission in 4σ steps. A synthesized beam and linear scale bar are shown as well. 3.4.2. Temperature analysis In addition to the kinematic analysis, the CH3CN(12k −11k) data with k = 0...7 allow us to derive rotational temperatures pixel by pixel for the entire central disk… view at source ↗
Figure 9
Figure 9. Figure 9: Toomre Q maps for the CepA disk. The left panel shows the Toomre Q map us￾ing the CH3CN rotational temperature map as input, whereas the right panel presents the esti￾mated Toomre Q map assuming a temperature gradient T ∝ r −0.4 . The white contour shows the Q = 3 line. The black contours outline the 1.3 mm continuum emission in 4σ steps. Syn￾thesized beam and linear scale bars are shown in both panels. Th… view at source ↗
Figure 10
Figure 10. Figure 10: Post-processed 1.37 mm continuum images based on Ahmadi et al. (2019). The left panels show the fragmented disk at 10 and 80 deg inclination (top and bottom, re￾spectively, similar to [PITH_FULL_IMAGE:figures/full_fig_p010_10.png] view at source ↗
read the original abstract

Context: Although there has been significant progress, the physical properties and potential fragmentation of accretion disks around high-mass protostars remain poorly constrained. Aims: We characterize at high angular resolution one of the most nearby (~700pc) high-mass accretion disk candidates CepA HW2. Methods: Using the new long baseline array configuration (~1700m) of the Northern Extended Millimeter Array (NOEMA), we study CepA HW2 with a resolution of <=0.2'' or <=100au at 1.3mm in dust continuum and spectral line emission. Results: The mm continuum emission resolves the central disk candidate into several sub-structures. Conducting a Toomre Q stability analysis based on CH_3CN and continuum data, and a comparison to 3D radiation hydrodynamic simulations shows that the data are consistent with an almost edge-on disk where the observed sub-structures may represent fragments within the disk. The CO and SiO spectral line data confirm a second bipolar outflow (in addition to the well-known jet) emanating from the central peak position. This indicates that this central peak should host at least a binary if not even a higher order multiple system. The usually assumed dense gas tracer CH_3CN shows also contributions from the outflows which complicates further kinematic analysis of the disk. Conclusions: The high-resolution outflow-disk data of CepA reveal a multiply fragmented disk that drives several outflows. These observations enforce the picture of high-mass star formation where multiplicity and fragmentation can happen on the smallest spatial scales related to the inner accretion disks.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

1 major / 2 minor

Summary. The paper presents NOEMA long-baseline observations at 1.3 mm of the nearby high-mass protostar candidate CepA HW2, achieving ≤0.2'' (≤100 au) resolution. The continuum resolves the central source into several sub-structures. A Toomre Q analysis is performed using CH3CN line data for temperature and velocity dispersion together with continuum-derived surface densities; this is combined with a comparison to 3D radiation-hydrodynamic simulations. The authors conclude that the observations are consistent with an almost edge-on, multiply fragmented disk that drives at least two bipolar outflows (one previously known jet plus a new CO/SiO outflow), implying that the central peak hosts a binary or higher-order multiple system. The work argues that fragmentation and multiplicity can occur on the smallest scales associated with inner accretion disks around high-mass stars.

Significance. If the Toomre Q results and simulation comparison hold, the observations supply rare sub-100-au constraints on the structure and stability of a high-mass accretion disk, directly addressing the open question of whether and how fragmentation proceeds at the scales of the inner disk. The detection of a second outflow from the central peak is a clear observational advance that strengthens the case for early multiplicity.

major comments (1)
  1. [Results section] Results section (Toomre Q analysis): The central claim that the sub-structures represent gravitationally unstable fragments rests on Q < 1 values derived from CH3CN temperatures/velocity dispersions and continuum surface densities. The abstract itself states that CH3CN exhibits outflow contributions that complicate kinematic analysis of the disk. If the CH3CN emission used for the Q calculation includes outflow material rather than pure disk gas, both the local sound speed and the surface-density estimates become unreliable, undermining the inference of gravitational instability. No independent check (e.g., dust-only temperature map or optically thin isotopologue) is described that would isolate the disk contribution.
minor comments (2)
  1. [Observations section] The abstract and text repeatedly cite a resolution of “≤0.2'' or ≤100 au”; the exact synthesized beam size, position angle, and how the 700 pc distance converts to au should be stated explicitly in the observations section for reproducibility.
  2. [Results section] The comparison to 3D radiation-hydrodynamic simulations is mentioned but the specific simulation parameters, viewing angle, and quantitative metrics used for the match are not detailed; a brief table or figure panel showing the simulated vs. observed morphology would improve clarity.

Simulated Author's Rebuttal

1 responses · 1 unresolved

We thank the referee for the positive assessment of the significance of our NOEMA observations and for the constructive comment on the Toomre Q analysis. We address the point below.

read point-by-point responses

  1. Referee: [Results section] Results section (Toomre Q analysis): The central claim that the sub-structures represent gravitationally unstable fragments rests on Q < 1 values derived from CH3CN temperatures/velocity dispersions and continuum surface densities. The abstract itself states that CH3CN exhibits outflow contributions that complicate kinematic analysis of the disk. If the CH3CN emission used for the Q calculation includes outflow material rather than pure disk gas, both the local sound speed and the surface-density estimates become unreliable, undermining the inference of gravitational instability. No independent check (e.g., dust-only temperature map or optically thin isotopologue) is described that would isolate the disk contribution.

    Authors: We acknowledge the validity of this concern. The abstract explicitly notes that CH3CN shows outflow contributions that complicate kinematic analysis, and the Toomre Q values were derived from the CH3CN (12-11) data for temperature and velocity dispersion together with continuum-derived surface densities. The analysis is presented as one line of evidence that is consistent with fragmentation when combined with the 3D radiation-hydrodynamic simulation comparison. We agree that an independent verification isolating pure disk emission would strengthen the result. The current data set does not contain an optically thin isotopologue or a separate dust-temperature map. We will revise the manuscript to expand the discussion of uncertainties arising from possible outflow contamination in the CH3CN-derived quantities and to qualify the strength of the gravitational-instability conclusion accordingly. revision: partial

standing simulated objections not resolved
  • Independent check isolating disk-only CH3CN emission (e.g., via optically thin isotopologue or dust-only temperature map) is not available in the present observations.

Circularity Check

0 steps flagged

No significant circularity; analysis is data-driven and self-contained

full rationale

The paper reports new NOEMA observations at <=0.2'' resolution, resolves sub-structures in 1.3 mm continuum, applies standard Toomre Q calculation using measured CH3CN line widths/temperatures plus continuum surface densities, and compares the outcome to independent 3D radiation-hydrodynamic simulations. No equations reduce a claimed prediction to a fitted parameter by construction, no load-bearing self-citations are invoked to justify uniqueness or ansatzes, and the outflow contamination in CH3CN is explicitly flagged as a complication rather than hidden. The derivation chain therefore rests on external data and external simulations, not on re-labeling of its own inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Since only the abstract is available, the ledger is based on mentioned methods. The Toomre Q analysis likely involves derived quantities from data rather than free parameters. No new entities postulated.

axioms (2)
  • standard math Standard assumptions in millimeter interferometry data reduction and imaging
    Used to produce the continuum and line maps at 0.2'' resolution.
  • domain assumption CH3CN and continuum data can be used to compute Toomre Q for disk stability despite noted outflow contamination
    Invoked in the stability analysis in the Results section.

pith-pipeline@v0.9.1-grok · 5939 in / 1382 out tokens · 92154 ms · 2026-07-01T02:45:57.812152+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

95 extracted references · 95 canonical work pages · 3 internal anchors

  1. [1]

    2023, , 677, A171

    Ahmadi , A., Beuther , H., Bosco , F., et al. 2023, , 677, A171

    work page 2023

  2. [2]

    C., et al

    Ahmadi , A., Beuther , H., Mottram , J. C., et al. 2018, , 618, A46

    work page 2018

  3. [3]

    2019, , 632, A50

    Ahmadi , A., Kuiper , R., & Beuther , H. 2019, , 632, A50

    work page 2019

  4. [4]

    M., Huang , J., P \'e rez , L

    Andrews , S. M., Huang , J., P \'e rez , L. M., et al. 2018, , 869, L41

    work page 2018

  5. [5]

    2015, , 448, 1007

    Behrendt , M., Burkert , A., & Schartmann , M. 2015, , 448, 1007

    work page 2015

  6. [6]

    T., Cesaroni , R., Rivilla , V

    Beltr \'a n , M. T., Cesaroni , R., Rivilla , V. M., et al. 2018, , 615, A141

    work page 2018

  7. [7]

    Beltr \'a n , M. T. & de Wit , W. J. 2016, , 24, 6

    work page 2016

  8. [8]

    B., McKee , C

    Beuther , H., Churchwell , E. B., McKee , C. F., & Tan , J. C. 2007, in Protostars and Planets V, ed. B. Reipurth , D. Jewitt , & K. Keil , 165--180

    work page 2007

  9. [9]

    2021, , 649, A113

    Beuther , H., Gieser , C., Suri , S., et al. 2021, , 649, A113

    work page 2021

  10. [10]

    2025, , 63, 1

    Beuther , H., Kuiper , R., & Tafalla , M. 2025, , 63, 1

    work page 2025

  11. [11]

    C., Ahmadi , A., et al

    Beuther , H., Mottram , J. C., Ahmadi , A., et al. 2018 a , , 617, A100

    work page 2018

  12. [12]

    D., Vlemmings , W., et al

    Beuther , H., Soler , J. D., Vlemmings , W., et al. 2018 b , , 614, A64

    work page 2018

  13. [13]

    M., et al

    Beuther , H., Wyrowski , F., Menten , K. M., et al. 2022, , 665, A63

    work page 2022

  14. [14]

    & Tremaine , S

    Binney , J. & Tremaine , S. 2008, Galactic Dynamics: Second Edition (Princeton University Press)

    work page 2008

  15. [15]

    2019, , 629, A10

    Bosco , F., Beuther , H., Ahmadi , A., et al. 2019, , 629, A10

    work page 2019

  16. [16]

    A., Pineda , J

    Busch , L. A., Pineda , J. E., Caselli , P., et al. 2026, , 708, A315

    work page 2026

  17. [17]

    2021, , 914, L1

    Carrasco-Gonz \'a lez , C., Sanna , A., Rodr \' guez-Kamenetzky , A., et al. 2021, , 914, L1

    work page 2021

  18. [18]

    2019, , 627, A68

    Cesaroni , R., Beuther , H., Ahmadi , A., et al. 2019, , 627, A68

    work page 2019

  19. [19]

    M., & Zhang , Q

    Cesaroni , R., Galli , D., Lodato , G., Walmsley , C. M., & Zhang , Q. 2007, in Protostars and Planets V, ed. B. Reipurth , D. Jewitt , & K. Keil , 197--212

    work page 2007

  20. [20]

    2007, , 469, 207

    Comito , C., Schilke , P., Endesfelder , U., Jim \'e nez-Serra , I., & Mart \' n-Pintado , J. 2007, , 469, 207

    work page 2007

  21. [21]

    J., Moeckel , N., & Bally , J

    Cunningham , N. J., Moeckel , N., & Bally , J. 2009, , 692, 943

    work page 2009

  22. [22]

    A., Cant \'o , J., et al

    Curiel , S., Trinidad , M. A., Cant \'o , J., et al. 2002, , 564, L35

    work page 2002

  23. [23]

    M., Liu , M., Tan , J

    De Buizer , J. M., Liu , M., Tan , J. C., et al. 2017, , 843, 33

    work page 2017

  24. [24]

    Draine , B. T. 2011, Physics of the Interstellar and Intergalactic Medium (Princeton Series in Astrophysics)

    work page 2011

  25. [25]

    2022, , 663, A123

    Durjasz , M., Szymczak , M., Olech , M., & Bartkiewicz , A. 2022, , 663, A123

    work page 2022

  26. [26]

    M., Beltr \'a n , M

    Frau , P., Girart , J. M., Beltr \'a n , M. T., et al. 2010, , 723, 1665

    work page 2010

  27. [27]

    Gammie , C. F. 2001, , 553, 174

    work page 2001

  28. [28]

    2023, , 674, A160

    Gieser , C., Beuther , H., Semenov , D., et al. 2023, , 674, A160

    work page 2023

  29. [29]

    2021, , 648, A66

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

    work page 2021

  30. [30]

    2022, , 657, A3

    Gieser , C., Beuther , H., Semenov , D., et al. 2022, , 657, A3

    work page 2022

  31. [31]

    2019, , 631, A142

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

    work page 2019

  32. [32]

    2018, , 860, 119

    Ginsburg , A., Bally , J., Goddi , C., Plambeck , R., & Wright , M. 2018, , 860, 119

    work page 2018

  33. [33]

    A., Sanhueza , P., et al

    Ginsburg , A., McGuire , B. A., Sanhueza , P., et al. 2023, , 942, 66

    work page 2023

  34. [34]

    F., Sargent , A

    G \'o mez , J. F., Sargent , A. I., Torrelles , J. M., et al. 1999, , 514, 287

    work page 1999

  35. [35]

    F., Torrelles , J

    G \'o mez , J. F., Torrelles , J. M., Girart , J. M., et al. 2023, , 956, L45

    work page 2023

  36. [36]

    Hildebrand , R. H. 1983, , 24, 267

    work page 1983

  37. [37]

    Hughes , V. A. & Wouterloot , J. G. A. 1984, , 276, 204

    work page 1984

  38. [38]

    D., Cyganowski , C

    Ilee , J. D., Cyganowski , C. J., Brogan , C. L., et al. 2018, , 869, L24

    work page 2018

  39. [39]

    D., Cyganowski , C

    Ilee , J. D., Cyganowski , C. J., Nazari , P., et al. 2016, , 462, 4386

    work page 2016

  40. [40]

    2007, , 661, L187

    Jim \'e nez-Serra , I., Mart \' n-Pintado , J., Rodr \' guez-Franco , A., et al. 2007, , 661, L187

    work page 2007

  41. [41]

    G., Hoare , M

    Johnston , K. G., Hoare , M. G., Beuther , H., et al. 2020, , 896, 35

    work page 2020

  42. [42]

    G., Robitaille , T

    Johnston , K. G., Robitaille , T. P., Beuther , H., et al. 2015, , 813, L19

    work page 2015

  43. [43]

    Kenyon , S. J. & Hartmann , L. 1987, , 323, 714

    work page 1987

  44. [44]

    & Ostriker , E

    Kim , W.-T. & Ostriker , E. C. 2007, , 660, 1232

    work page 2007

  45. [45]

    E., Kuiper , R., Peters , T., & Banerjee , R

    Klassen , M., Pudritz , R. E., Kuiper , R., Peters , T., & Banerjee , R. 2016, , 823, 28

    work page 2016

  46. [46]

    M., Matzner , C

    Kratter , K. M., Matzner , C. D., Krumholz , M. R., & Klein , R. I. 2010, , 708, 1585

    work page 2010

  47. [47]

    Kumar , M. S. N., Palmeirim , P., Arzoumanian , D., & Inutsuka , S. I. 2020, , 642, A87

    work page 2020

  48. [48]

    Lang , K. R. 1992, Astrophysical Data I (Planets and Stars, X, 937 pp. 33 figs.. Springer-Verlag Berlin Heidelberg New York)

    work page 1992

  49. [49]

    2011, , 530, A12

    Leurini , S., Codella , C., Zapata , L., et al. 2011, , 530, A12

    work page 2011

  50. [50]

    B., Trapman , L., Monsch , K., et al

    Lovell , J. B., Trapman , L., Monsch , K., et al. 2025, , 989, 69

    work page 2025

  51. [51]

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

    work page 2001

  52. [52]

    F., Ansdell , M., Rosotti , G

    Manara , C. F., Ansdell , M., Rosotti , G. P., 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 , 539

    work page 2023

  53. [53]

    2005, , 628, L61

    Mart \' n-Pintado , J., Jim \'e nez-Serra , I., Rodr \' guez-Franco , A., Mart \' n , S., & Thum , C. 2005, , 628, L61

    work page 2005

  54. [54]

    T., Cesaroni , R., Kumar , M

    Maud , L. T., Cesaroni , R., Kumar , M. S. N., et al. 2019, , 627, L6

    work page 2019

  55. [55]

    2023, , 672, A88

    Mignon-Risse , R., Oliva , A., Gonz \'a lez , M., Kuiper , R., & Commer c on , B. 2023, , 672, A88

    work page 2023

  56. [56]

    2017, , 59, A7

    M \"o ller , T., Endres , C., & Schilke , P. 2017, , 59, A7

    work page 2017

  57. [57]

    B., Stapelfeldt , K

    Monsch , K., Lovell , J. B., Stapelfeldt , K. R., et al. 2026, , 996, 45

    work page 2026

  58. [58]

    2021, , 647, A114

    Moscadelli , L., Beuther , H., Ahmadi , A., et al. 2021, , 647, A114

    work page 2021

  59. [59]

    Protostellar Outflows at the EarliesT Stages (POETS). IX. Magnetohydrodynamic disk winds traced by SO and SO$_2$ in luminous protostars

    Moscadelli , L., Beuther , H., Sanna , A., et al. 2026, arXiv e-prints, arXiv:2606.11908

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  60. [60]

    J., Cesaroni , R., et al

    Moscadelli , L., Li , J. J., Cesaroni , R., et al. 2013, , 549, A122

    work page 2013

  61. [61]

    J., Menten , K

    Moscadelli , L., Reid , M. J., Menten , K. M., et al. 2009, , 693, 406

    work page 2009

  62. [62]

    2018, , 56, 41

    Motte , F., Bontemps , S., & Louvet , F. 2018, , 56, 41

    work page 2018

  63. [63]

    2025, , 694, A24

    Motte , F., Pouteau , Y., Nony , T., et al. 2025, , 694, A24

    work page 2025

  64. [64]

    C., Beuther , H., Ahmadi , A., et al

    Mottram , J. C., Beuther , H., Ahmadi , A., et al. 2020, , 636, A118

    work page 2020

  65. [65]

    Complex organic molecules and cosmic ray ionisation rate towards the massive protostar Cepheus A HW2

    Nielsen , E. W., Punanova , A., Wirstr \"o m , E., et al. 2026, arXiv e-prints, arXiv:2605.06767

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  66. [66]

    Offner , S. S. R., Moe , M., Kratter , K. M., 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 , 275

    work page 2023

  67. [67]

    Ohashi , N., Hayashi , M., Ho , P. T. P., Momose , M., & Hirano , N. 1996, , 466, 957

    work page 1996

  68. [68]

    A., Sanhueza , P., Oya , Y., et al

    Olguin , F. A., Sanhueza , P., Oya , Y., et al. 2026, , 999, 106

    work page 2026

  69. [69]

    Oliva , G. A. & Kuiper , R. 2020, , 644, A41

    work page 2020

  70. [70]

    & Henning , T

    Ossenkopf , V. & Henning , T. 1994, , 291, 943

    work page 1994

  71. [71]

    2009, , 508, 737

    Parise , B., Leurini , S., Schilke , P., et al. 2009, , 508, 737

    work page 2009

  72. [72]

    A., Curiel , S., Sridharan , T

    Patel , N. A., Curiel , S., Sridharan , T. K., et al. 2005, , 437, 109

    work page 2005

  73. [73]

    R., Hily-Blant , P., Gerin , M., & Teyssier , D

    Pety , J., Goicoechea , J. R., Hily-Blant , P., Gerin , M., & Teyssier , D. 2007, , 464, L41

    work page 2007

  74. [74]

    F., Ho , P

    Rodriguez , L. F., Ho , P. T. P., & Moran , J. M. 1980, , 240, L149

    work page 1980

  75. [75]

    F., Torrelles , J

    S \'a nchez-Monge , \'A ., G \'o mez , J. F., Torrelles , J. M., et al. 2025, , 543, 662

    work page 2025

  76. [76]

    2021, , 655, A72

    Sanna , A., Giannetti , A., Bonfand , M., et al. 2021, , 655, A72

    work page 2021

  77. [77]

    2017, , 603, A94

    Sanna , A., Moscadelli , L., Surcis , G., et al. 2017, , 603, A94

    work page 2017

  78. [78]

    2025, , 697, A206

    Sanna , A., Oliva , A., Moscadelli , L., et al. 2025, , 697, A206

    work page 2025

  79. [79]

    M., Contreras , Y., et al

    Schuller , F., Menten , K. M., Contreras , Y., et al. 2009, , 504, 415

    work page 2009

  80. [80]

    & Wolf , V

    Stecklum , B. & Wolf , V. 2025, arXiv e-prints, arXiv:2506.16519

    work page arXiv 2025

Showing first 80 references.