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arxiv: 2606.26044 · v1 · pith:CPDCN5ATnew · submitted 2026-06-24 · 🌌 astro-ph.GA · astro-ph.SR

Jets and Outflows in Young Stellar Objects with the SKAO

Giovanni Sabatini , Gemma Busquet , Carlos Carrasco-Gonz\'alez , Adriana Rodr\'iguez-Kamenetzky , Codella Claudio , Linda Podio , Antonio Mart\'inez-Henares , Josep Miquel Girart
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Marta De Simone Luca Cacciapuoti Guillem Anglada Lukasz Tychoniec Lisa Giani Manoj Puravankara Francesca Bacciotti Rafael Bachiller Eleonora Bianchi Guillermo Bl\'azquez-Calero Tyler L. Bourke Stefano Bovino Paola Caselli Francesco Cavallaro Cecilia Ceccarelli Elena Diaz-Marquez Stefano Facchini Antonio Garufi Greta Guidi Tomoya Hirota John D. Ilee Adriano Ingallinera Izaskun Jim\'enez-Serra Valerio Lattanzi Chin-Fei Lee Manuela Lippi Alessandro Lupi Liton Majumdar Mayank Narang Mayra Osorio Marco Padovani Jaime Pineda Isaac Radley Basmah Riaz Luis Felipe Rodr\'iguez Alvaro S\'anchez-Monge Alberto Sanna Silvia Spezzano Leonardo Testi Claudia Toci Alessio Traficante Himanshu Tyagi Grazia Maria Umana
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Pith reviewed 2026-06-25 19:07 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.SR
keywords jetswilldustoutflowsallowchemicalcrucialysos
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The pith

SKAO will enable high-resolution centimeter observations to probe jets and outflows near young stellar objects.

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

The paper argues that the SKA Observatory can supply the high angular resolution and sensitivity at centimeter wavelengths that current facilities lack for examining jets and outflows close to young stars. This matters because these structures remove angular momentum during star formation and shape the chemistry of their surroundings, but many details of acceleration, collimation, and chemical impact remain unknown. The review outlines how radio recombination lines will map three-dimensional jet motions when combined with proper motions, how polarized synchrotron emission will trace magnetic field strength and morphology at scales of a few au, how dust emission in cavities will reveal growth and transport between disk and envelope, and how shock observations will detect the release of grain mantles and new molecular species. If these capabilities perform as projected, SKAO data would connect small-scale launch processes to larger-scale environmental effects.

Core claim

The SKA-project will overcome the limitations of current mm/cm-facilities by enabling high-angular resolution and high-sensitivity cm-observations, crucial for probing jets/outflows near YSOs. Radio recombination lines, combined with proper motions, offer a unique opportunity to study the 3D-kinematics of jets. Non-thermal linearly polarised synchrotron emission will allow measuring magnetic field strength and morphology at unprecedented scales of a few au. Observations of dust emission in outflow cavities will allow studying how dust grows and is eventually transported from the disc to the envelope and back. Finally, the SKA-project will allow exploring the dust composition and chemical enr

What carries the argument

SKAO high-angular resolution and high-sensitivity cm-observations that target radio recombination lines, non-thermal polarized synchrotron emission, dust in outflow cavities, and shock-released chemical species.

If this is right

  • Radio recombination lines combined with proper motions will reveal the 3D-kinematics of jets.
  • Non-thermal polarized synchrotron emission will measure magnetic field strength and morphology at scales of a few au.
  • Dust emission in outflow cavities will show how dust grows and moves from the disc to the envelope and back.
  • Shock observations will detect long carbon chains, rings, and metal-bearing species released from grain mantles.
  • These cm-wave data will complement ALMA's sub-mm detections of organic molecules to build fuller chemical inventories.

Where Pith is reading between the lines

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

  • High-resolution magnetic field maps could directly test whether magnetic fields provide the dominant collimation mechanism for jets.
  • Combined SKAO-ALMA datasets might reveal how outflow shocks alter the overall molecular inventory from inner disk to outer envelope.
  • Detection of dust transport in cavities could quantify the efficiency with which material is recycled between disk and envelope during early star formation.
  • If signals prove weaker than expected, the review's case would require targeted simulations of emission strengths for specific YSO targets.
  • keywords:[

Load-bearing premise

The described emission processes will produce detectable signals at the scales and sensitivities projected for SKAO.

What would settle it

If SKAO observations of known YSO jets detect neither radio recombination lines with measurable proper motions nor polarized synchrotron emission at few-au scales, despite the claimed sensitivity gains over VLA and ALMA.

Figures

Figures reproduced from arXiv: 2606.26044 by Adriana Rodr\'iguez-Kamenetzky, Adriano Ingallinera, Alberto Sanna, Alessandro Lupi, Alessio Traficante, Alvaro S\'anchez-Monge, Antonio Garufi, Antonio Mart\'inez-Henares, Basmah Riaz, Carlos Carrasco-Gonz\'alez, Cecilia Ceccarelli, Chin-Fei Lee, Claudia Toci, Codella Claudio, Elena Diaz-Marquez, Eleonora Bianchi, Francesca Bacciotti, Francesco Cavallaro, Gemma Busquet, Giovanni Sabatini, Grazia Maria Umana, Greta Guidi, Guillem Anglada, Guillermo Bl\'azquez-Calero, Himanshu Tyagi, Isaac Radley, Izaskun Jim\'enez-Serra, Jaime Pineda, John D. Ilee, Josep Miquel Girart, Leonardo Testi, Linda Podio, Lisa Giani, Liton Majumdar, Luca Cacciapuoti, Luis Felipe Rodr\'iguez, Lukasz Tychoniec, Manoj Puravankara, Manuela Lippi, Marco Padovani, Marta De Simone, Mayank Narang, Mayra Osorio, Paola Caselli, Rafael Bachiller, Silvia Spezzano, Stefano Bovino, Stefano Facchini, Tomoya Hirota, Tyler L. Bourke, Valerio Lattanzi.

Figure 1
Figure 1. Figure 1: Left: Sketch of the extended disc wind and jet from a protostar. The wind launches from 4–40 au, while the jet originates at radii <0.20 au. The shell (gray cross-hatched) spans from the wind’s inner region to the jet-driven bow shock (adapted from Lee et al. 2021). Middle Panel: The HH 212 protostellar disc/jet system viewed by ALMA, revealing: (i) the SiO jet (blue and red contours), (ii) the C17O rotati… view at source ↗
Figure 2
Figure 2. Figure 2: Chemical stratification in the L1157-B1 shocked region as traced by the IRAM-NOEMA. (Left) Maps of NH2CO (41,4—31,3) and CO(1–0) emission (white contours; Gueth et al. 1996; Codella et al. 2017). (Right) Zoom-in of the B1 shocked region as traced by Formamide (colour), Methanol, Formaldehyde, deuterated Formaldehyde, and Acetaldehyde (Benedettini et al., 2013; Fontani et al., 2014; Codella et al., 2015, 20… view at source ↗
Figure 3
Figure 3. Figure 3: Full 5 cm view of the HH 80-81 jet. (a) Total intensity image of the radio jet, showing precession with dotted arrows; Herbig–Haro objects are labelled. The dashed lines indicate the region shown in (b). (b) Polarised emission is shown where the S/N is above 4 and total intensity S/N above 10. Green contours show total intensity at [10, 1000]𝜎 (with 𝜎 = 3 𝜇Jy beam−1 ). Circles mark the area shown in panel … view at source ↗
Figure 4
Figure 4. Figure 4: 𝐿R-𝐿bol correlation using data col￾lected from the literature. The dashed black line corresponds to the fit done to all radio jets in Anglada et al. (2018), while the solid black line is the fits using the whole sam￾ple. The red dotted line depicts the expected 𝐿R associated with the Lyman continuum flux of Hii regions powered by stars of different 𝐿bol. The black dashed horizontal line marks the 5𝜎 rms of… view at source ↗
Figure 5
Figure 5. Figure 5: MORELI predictions of the H82𝛼 RRL at 11.71 GHz. We show predictions for different combinations of wind 𝑀¤ loss and 𝑑 of the system, starting from the case of MWC 349A (left panel). The pale-blue region shows the 5𝜎 detection with SKA-Mid (see text), while the dark blue corresponds to the 5𝜎 detection with SKA-Mid (AA4) of the line intensity at a velocity of 100 km s−1 . Integration times from the SKAO Sen… view at source ↗
Figure 6
Figure 6. Figure 6: (Left) The protostellar shock L1157-B1 along the southern lobe of the outflow driven by L1157- mm. (Middle/right): Zoom-in around L1157-B1, where the abundance of several molecules is mapped; Metal-bearing molecules (e.g. SiO and SiS; middle) probe grain core sputtering; (right) HC3N is released from the grain mantles. Adapted from Podio et al. (2017) and Benedettini et al. (2013). 5.1 Cyanopolyynes as pro… view at source ↗
Figure 7
Figure 7. Figure 7: Predicted (LTE) line in￾tensities of cyanopolyynes in high￾mass protostellar outflows, obtained for 𝑇 = 20 K, FWHM = 4 km s−1 , and a filling factor of 1. We as￾sumed 𝑁(HC5N)=3×1015 cm2 (Hoque et al. 2025; HC3N/HC5N = 3), fol￾lowing Bianchi et al. (2023b) for the other cyanopolyynes. The horizontal dashed lines indicate the 3𝜎 predic￾tions of the SKAO sensitivity calcu￾lator at 12.5 GHz with the SKA-Mid AA… view at source ↗
Figure 8
Figure 8. Figure 8: (Left) The L1551 IRS5 Class I binary system from Sabatini et al. (2025). colour map: Thermal dust continuum emission at 3 mm (from the FAUST ALMA-LP) mapping the circumbinary disc and the dusty cavity walls structure. White contours mark the [3, 6, 10, 100]𝜎, with 𝜎 = 0.08 mJy beam−1 . Transparent red and blue areas: The red- and blue-shifted CO (2-1) outflow emission. (Right) Sketch illustrating how dust … view at source ↗
read the original abstract

Jets and outflows are ubiquitous phenomena associated with the formation of young stellar objects (YSOs). They play a crucial role in removing angular momentum from the accreting system and in regulating star-formation efficiency. Theoretical studies and observations with ALMA and VLA have shown that jets and winds may have a crucial role in promoting dust growth in the envelope-disc system and in shaping the physical and chemical properties of the surrounding environment. Despite these significant advances, many fundamental questions remain unanswered regarding the acceleration, collimation, and chemical impact of jets and outflows from YSOs. The SKA-project will overcome the limitations of current mm/cm-facilities by enabling high-angular resolution and high-sensitivity cm-observations, crucial for probing jets/outflows near YSOs. Radio recombination lines, combined with proper motions, offer a unique opportunity to study the 3D-kinematics of jets. Non-thermal linearly polarised synchrotron emission will allow measuring magnetic field strength and morphology at unprecedented scales of a few au. Observations of dust emission in outflow cavities will allow studying how dust grows and is eventually transported from the disc to the envelope and back. Finally, the SKA-project will allow exploring the dust composition and chemical enrichment in shocks, where sputtering/shattering of grains cause the release of their mantles and refractory cores in the gas-phase. Complementary to ALMA's detection of simple and complex organic molecules, the SKAO will probe, for the first time, long carbon chains/rings, several Cl-, Al-, Mg-, and other metal-bearing species (missed by current sub-mm facilities).

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

2 major / 1 minor

Summary. The manuscript presents a perspective on the scientific opportunities offered by the Square Kilometre Array Observatory (SKAO) for studying jets and outflows associated with young stellar objects (YSOs). It argues that SKAO's high-resolution and high-sensitivity cm-wave observations will address open questions in jet acceleration, collimation, and chemical impact by enabling observations of radio recombination lines for 3D kinematics, polarized synchrotron emission for magnetic fields, dust emission in cavities for dust growth, and shock-induced chemical enrichment including long carbon chains and metal-bearing species.

Significance. If the detectability assumptions hold, this work could guide future observational strategies with SKAO, complementing ALMA and VLA data on YSOs. However, the absence of quantitative modeling or simulations means the significance is primarily in outlining qualitative prospects rather than providing actionable predictions.

major comments (2)
  1. [Abstract] Abstract: The central assertion that the SKA-project 'will overcome the limitations of current mm/cm-facilities by enabling high-angular resolution and high-sensitivity cm-observations, crucial for probing jets/outflows near YSOs' is not supported by any quantitative estimates of expected fluxes, brightness temperatures, optical depths, or comparisons to SKA sensitivity and confusion limits for the listed processes (synchrotron emission, dust in cavities, RRLs, shock chemistry).
  2. Main text (paragraph on non-thermal emission and dust): The claims that linearly polarised synchrotron emission 'will allow measuring magnetic field strength and morphology at unprecedented scales of a few au' and that dust emission observations 'will allow studying how dust grows' rest on unverified extrapolation from ALMA/VLA results without error budgets, simulated visibilities, or predicted signal strengths at SKAO frequencies and resolutions.
minor comments (1)
  1. The manuscript alternates between 'SKA-project' and 'SKAO'; adopting consistent nomenclature would improve readability.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their review. We address the major comments point by point below, with proposed revisions to strengthen the quantitative grounding of the perspective while preserving its scope as a science case outline.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The central assertion that the SKA-project 'will overcome the limitations of current mm/cm-facilities by enabling high-angular resolution and high-sensitivity cm-observations, crucial for probing jets/outflows near YSOs' is not supported by any quantitative estimates of expected fluxes, brightness temperatures, optical depths, or comparisons to SKA sensitivity and confusion limits for the listed processes (synchrotron emission, dust in cavities, RRLs, shock chemistry).

    Authors: We agree that the abstract assertion would be strengthened by quantitative context. The manuscript is a perspective paper that extrapolates from published ALMA and VLA results on YSO jets rather than presenting new modeling. We will revise the abstract to moderate the phrasing and insert a concise paragraph (or subsection) providing order-of-magnitude flux and sensitivity estimates drawn from existing literature and SKA technical documentation, including references to sensitivity calculators and prior scaling studies for RRLs, synchrotron, and dust. revision: yes

  2. Referee: [—] Main text (paragraph on non-thermal emission and dust): The claims that linearly polarised synchrotron emission 'will allow measuring magnetic field strength and morphology at unprecedented scales of a few au' and that dust emission observations 'will allow studying how dust grows' rest on unverified extrapolation from ALMA/VLA results without error budgets, simulated visibilities, or predicted signal strengths at SKAO frequencies and resolutions.

    Authors: The referee correctly identifies that these statements rely on extrapolation. We will expand the relevant paragraphs to cite specific ALMA/VLA detections that demonstrate the relevant angular scales and polarization fractions, and add brief scaling arguments for expected polarized intensities and dust fluxes at SKA frequencies using published spectral indices. We will also explicitly note that detailed error budgets and visibility simulations lie beyond the scope of a perspective paper. This addresses the concern without altering the manuscript's qualitative focus. revision: partial

Circularity Check

0 steps flagged

No circularity: paper is a science-case review with no derivations or fitted predictions

full rationale

The manuscript contains no equations, no fitted parameters, no 'predictions' derived from models, and no derivation chain. It enumerates observational opportunities (RRLs, synchrotron, dust in cavities, shock chemistry) based on prior ALMA/VLA results but performs no quantitative detectability calculations or reductions that could be circular. All claims are forward-looking statements about SKAO capabilities; none reduce to self-definition, self-citation load-bearing, or renaming of inputs. This is the expected non-finding for a proposal-style paper.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a prospective science case paper with no mathematical derivations, fitted parameters, or new postulated entities. All content rests on prior literature about YSO jets and SKA capabilities.

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discussion (0)

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Works this paper leans on

244 extracted references · 226 canonical work pages · 2 internal anchors

  1. [1]

    doi: 10.1051/0004-6361/201833666. B. Albertazzi et al.Science, 346(6207):325–328, Oct

    work page doi:10.1051/0004-6361/201833666

  2. [2]

    F.O.Alves,W.H.T.Vlemmings,J.M.Girart,andJ.M.Torrelles.A&A,542:A14,June2012

    doi: 10.1126/science.1259694. F.O.Alves,W.H.T.Vlemmings,J.M.Girart,andJ.M.Torrelles.A&A,542:A14,June2012. doi: 10.1051/0004-6361/ 201118710. AMI Consortium et al.MNRAS, 410(4):2662–2678, Feb

    work page doi:10.1126/science.1259694

  3. [3]

    doi: 10.1111/j.1365-2966.2010.17644.x. P. Andre, T. Montmerle, and E. D. Feigelson.AJ, 93:1182, May

    work page doi:10.1111/j.1365-2966.2010.17644.x 2010

  4. [4]

    doi: 10.1086/114400. P. Andre, B. D. Deeney, R. B. Phillips, and J.-F. Lestrade.ApJ, 401:667, Dec

    work page doi:10.1086/114400

  5. [5]

    doi: 10.1086/172094. G. Anglada et al.ApJ, 395:494, Aug

    work page doi:10.1086/172094

  6. [6]

    doi: 10.1086/171670. G. Anglada et al.AJ, 116(6):2953–2964, Dec

    work page doi:10.1086/171670

  7. [7]

    doi: 10.1086/300637. G. Anglada, L. F. Rodríguez, and C. Carrasco-Gonzalez. InAdvancing Astrophysics with the Square Kilometre Array (AASKA14), page 121, Apr

    work page doi:10.1086/300637

  8. [8]

    G.Anglada,L.F.Rodríguez,andC.Carrasco-González.A&ARv,26(1):3,June2018

    doi: 10.22323/1.215.0121. G.Anglada,L.F.Rodríguez,andC.Carrasco-González.A&ARv,26(1):3,June2018. doi: 10.1007/s00159-018-0107-z. H. G. Arce and A. I. Sargent.ApJ, 646(2):1070–1085, Aug

    work page doi:10.22323/1.215.0121

  9. [9]

    doi: 10.1086/505104. H. G. Arce et al. In B. Reipurth, D. Jewitt, and K. Keil, editors,Protostars and Planets V, page 245, Jan

    work page doi:10.1086/505104

  10. [10]

    doi: 10.48550/arXiv.astro-ph/0603071. H. G. Arce et al.ApJL, 681(1):L21, July

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0603071

  11. [11]

    25 Jets & Outflows in YSOs with the SKAO Sabatini G

    doi: 10.1086/590110. 25 Jets & Outflows in YSOs with the SKAO Sabatini G. et al. F. Bacciotti, J. Eislöffel, and T. P. Ray.A&A, 350:917–927, Oct

    work page doi:10.1086/590110

  12. [12]

    doi: 10.1086/341725. F. Bacciotti et al.arXiv e-prints, art. arXiv:2501.03920, Jan

    work page doi:10.1086/341725

  13. [13]

    doi: 10.48550/arXiv.2501.03920. R. Bachiller and J. Cernicharo.A&A, 239:276, Nov

    work page doi:10.48550/arxiv.2501.03920

  14. [14]

    doi: 10.1086/310877. R. Bachiller, J. Martin-Pintado, and A. Fuente.A&A, 243:L21, Mar

    work page doi:10.1086/310877

  15. [16]

    doi: 10.1051/0004-6361/201424389. J. Bally.Astro. & Space Sci., 311(1-3):15–24, Oct

    work page doi:10.1051/0004-6361/201424389

  16. [17]

    doi: 10.1007/s10509-007-9531-7. J. Bally.ARA&A, 54:491–528,

    work page doi:10.1007/s10509-007-9531-7

  17. [18]

    doi: https://doi.org/10.1146/annurev-astro-081915-023341

    ISSN 1545-4282. doi: https://doi.org/10.1146/annurev-astro-081915-023341. M. R. Bate.MNRAS, 514(2):2145–2161, Aug

    work page doi:10.1146/annurev-astro-081915-023341

  18. [19]

    doi: 10.1093/mnras/stac1391. A. R. Bell.MNRAS, 182:147–156, Jan

    work page doi:10.1093/mnras/stac1391

  19. [20]

    doi: 10.1093/mnras/182.2.147. M. Benedettini et al.MNRAS, 381(3):1127–1136, Nov

    doi:10.1093/mnras/182.2.147

  20. [21]

    doi: 10.1111/j.1365-2966.2007.12300.x. M. Benedettini et al.MNRAS, 436(1):179–190, Nov

    work page doi:10.1111/j.1365-2966.2007.12300.x 2007

  21. [22]

    doi: 10.1093/mnras/stt1559. H. Beuther, R. Kuiper, and M. Tafalla.ARA&A, 63(1):1–44, Aug

    work page doi:10.1093/mnras/stt1559

  22. [23]

    doi: 10.1146/annurev-astro-013125-122023. A. Bhandare et al.A&A, 687:A158, July

    work page doi:10.1146/annurev-astro-013125-122023

  23. [24]

    doi: 10.1051/0004-6361/202449594. E. Bianchi et al.Faraday Discussions, 245:164–180, Sept. 2023a. doi: 10.1039/D3FD00018D. E. Bianchi et al.ApJ, 944(2):208, Feb. 2023b. doi: 10.3847/1538-4357/acb5e8. E. Bianchi et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361/202449594

  24. [25]

    doi: 10.1051/0004-6361/202451433. P. Bjerkeli et al.Nature, 540(7633):406–409, Dec

    work page doi:10.1051/0004-6361/202451433

  25. [26]

    doi: 10.1038/nature20600. G. Blázquez-Calero et al.Nature Astronomy, 10:105–123, Jan

    work page doi:10.1038/nature20600

  26. [27]

    doi: 10.1038/s41550-025-02716-2. M. Bouvier et al.MNRAS, 539(3):2380–2399, May

    work page doi:10.1038/s41550-025-02716-2

  27. [28]

    doi: 10.1093/mnras/staf631. S. Bovino et al.MNRAS, 495(1):L7–L11, June

    work page doi:10.1093/mnras/staf631

  28. [29]

    doi: 10.1093/mnrasl/slaa048. R. D. Boyden et al.ApJ, 983(1):81, Apr

    work page doi:10.1093/mnrasl/slaa048

  29. [30]

    doi: 10.3847/1538-4357/adbbcc. A. Bracco et al.A&A, 604:A52, Aug

    work page doi:10.3847/1538-4357/adbbcc

  30. [31]

    doi: 10.1051/0004-6361/201731117. S. Cabrit, A. Raga, and F. Gueth. In B. Reipurth and C. Bertout, editors,Herbig-Haro Flows and the Birth of Stars, volume 182 ofIAU Symposium, pages 163–180, Jan

    work page doi:10.1051/0004-6361/201731117

  31. [32]

    doi: 10.3847/1538-4357/ad0f17. L. Cacciapuoti et al.A&A, 700:A188, Aug

    work page doi:10.3847/1538-4357/ad0f17

  32. [33]

    doi: 10.1051/0004-6361/202554645. A. Caratti o Garatti et al.A&A, 691:A134, Nov. 2024a. doi: 10.1051/0004-6361/202451350. A. Caratti o Garatti et al.A&A, 691:A134, Nov. 2024b. doi: 10.1051/0004-6361/202451350. C. Carrasco-González et al.Science, 330(6008):1209, Nov

    work page doi:10.1051/0004-6361/202554645

  33. [34]

    doi: 10.1126/science.1195589. C. Carrasco-González et al.ApJL, 752(2):L29, June

    work page doi:10.1126/science.1195589

  34. [35]

    doi: 10.1088/2041-8205/752/2/L29. C. Carrasco-González et al.Science, 348(6230):114–117, Apr

    work page doi:10.1088/2041-8205/752/2/l29 2041

  35. [36]

    doi: 10.1126/science.aaa7216. C. Carrasco-González et al.ApJ, 883(1):71, Sept

    doi:10.1126/science.aaa7216

  36. [37]

    doi: 10.3847/1538-4357/ab3d33. C. Carrasco-González et al.ApJL, 914(1):L1, June

    work page doi:10.3847/1538-4357/ab3d33

  37. [38]

    doi: 10.3847/2041-8213/abf735. P. Caselli, T. W. Hartquist, and O. Havnes.A&A, 322:296–301, June

    work page doi:10.3847/2041-8213/abf735 2041

  38. [39]

    doi: 10.3847/1538-4357/aa961d. C. Ceccarelli et al. InProtostars and Planets VII, volume 534 ofAstronomical Society of the Pacific Conference Series, page 379, July

    doi:10.3847/1538-4357/aa961d

  39. [40]

    doi: 10.1086/432828. C. Codella, R. Bachiller, and B. Reipurth.A&A, 343:585–598, Mar

    work page doi:10.1086/432828

  40. [41]

    doi: 10.1051/0004-6361/200913340. C. Codella et al.A&A, 518:L112, July

    doi:10.1051/0004-6361/200913340

  41. [42]

    26 Jets & Outflows in YSOs with the SKAO Sabatini G

    doi: 10.1051/0004-6361/201014582. 26 Jets & Outflows in YSOs with the SKAO Sabatini G. et al. C. Codella et al.ApJL, 757:L9, Sept

    work page doi:10.1051/0004-6361/201014582

  42. [43]

    doi: 10.1088/2041-8205/757/1/L9. C. Codella et al.MNRAS, 449:L11–L15, Apr

    work page doi:10.1088/2041-8205/757/1/l9 2041

  43. [44]

    doi: 10.1093/mnrasl/slu204. C. Codella et al.A&A, 605:L3, Sept

    work page doi:10.1093/mnrasl/slu204

  44. [45]

    doi: 10.1051/0004-6361/201731249. C. Codella et al.A&A, 635:A17, Mar

    doi:10.1051/0004-6361/201731249

  45. [46]

    doi: 10.1051/0004-6361/201936725. C. Codella et al.A&A, 654:A52, Oct

    work page doi:10.1051/0004-6361/201936725

  46. [47]

    doi: 10.1051/0004-6361/202141485. C. Codella et al.A&A, 696:A219, Apr

    work page doi:10.1051/0004-6361/202141485

  47. [48]

    doi: 10.1051/0004-6361/202453621. M. Cohen, J. H. Bieging, and P. R. Schwartz.ApJ, 253:707–715, Feb

    work page doi:10.1051/0004-6361/202453621

  48. [49]

    doi: 10.1086/159671. C. P. Coughlan et al.ApJ, 834(2):206, Jan

    work page doi:10.1086/159671

  49. [50]

    doi: 10.3847/1538-4357/834/2/206. A. Coutens et al.A&A, 631:A58, Nov

    work page doi:10.3847/1538-4357/834/2/206

  50. [51]

    doi: 10.1051/0004-6361/201935340. S. Curiel, L. F. Rodriguez, J. M. Moran, and J. Canto.ApJ, 415:191, Sept

    work page doi:10.1051/0004-6361/201935340

  51. [52]

    doi: 10.1086/173155. S. Curiel, J. M. Girart, L. F. Rodríguez, and J. Cantó.ApJL, 582(2):L109–L113, Jan

    work page doi:10.1086/173155

  52. [53]

    doi: 10.1086/367631. S. Curiel et al.ApJ, 638(2):878–886, Feb

    doi:10.1086/367631

  53. [54]

    doi: 10.1086/498931. M. De Simone et al.A&A, 599:A121, Mar

    work page doi:10.1086/498931

  54. [55]

    doi: 10.1051/0004-6361/201630049. M. De Simone et al.A&A, 640:A75, Aug

    work page doi:10.1051/0004-6361/201630049

  55. [56]

    doi: 10.1051/0004-6361/201937004. A. de Valon et al.A&A, 668:A78, Dec

    doi:10.1051/0004-6361/201937004

  56. [57]

    doi: 10.1051/0004-6361/202141316. V. Delabrosse et al.A&A, 688:A173, Aug

    doi:10.1051/0004-6361/202141316

  57. [58]

    doi: 10.1051/0004-6361/202449176. E. Díaz-Márquez et al.A&A, 682:A180, Feb

    work page doi:10.1051/0004-6361/202449176

  58. [59]

    doi: 10.1051/0004-6361/202348085. A. K. Diaz-Rodriguez et al.ApJ, 930(1):91, May

    work page doi:10.1051/0004-6361/202348085

  59. [60]

    doi: 10.3847/1538-4357/ac3b50. C. Dickinson et al.New Astron. Rev., 80:1–28, Feb

    doi:10.3847/1538-4357/ac3b50

  60. [61]

    doi: 10.1016/j.newar.2018.02.001. M. M. Dunham et al.ApJ, 783(1):29, Mar

    work page doi:10.1016/j.newar.2018.02.001 2018

  61. [62]

    doi: 10.1088/0004-637X/783/1/29. S. A. Dzib et al.ApJ, 775(1):63, Sept

    work page doi:10.1088/0004-637x/783/1/29

  62. [63]

    doi: 10.1088/0004-637X/775/1/63. S. A. Dzib et al.ApJ, 834(2):139, Jan

    work page doi:10.1088/0004-637x/775/1/63

  63. [64]

    doi: 10.3847/1538-4357/834/2/139. L. E. Ellerbroek et al.A&A, 551:A5, Mar

    doi:10.3847/1538-4357/834/2/139

  64. [65]

    doi: 10.1051/0004-6361/201220635. J. Erkal et al.ApJ, 919(1):23, Sept

    doi:10.1051/0004-6361/201220635

  65. [66]

    doi: 10.3847/1538-4357/ac06c5. J. R. Feddersen et al.ApJ, 896(1):11, June

    work page doi:10.3847/1538-4357/ac06c5

  66. [67]

    doi: 10.3847/1538-4357/ab86a9. S. A. Federman et al.ApJ, 966(1):41, May

    doi:10.3847/1538-4357/ab86a9

  67. [68]

    doi: 10.3847/1538-4357/ad2fa0. R. Fedriani et al.Nat. Commun., 10:3630, Aug

    doi:10.3847/1538-4357/ad2fa0

  68. [69]

    doi: 10.1038/s41467-019-11595-x. A. Feeney-Johansson et al.ApJL, 885(1):L7, Nov

    work page doi:10.1038/s41467-019-11595-x

  69. [70]

    doi: 10.3847/2041-8213/ab4b56. M. Fernández-López et al.ApJ, 956(2):82, Oct

    work page doi:10.3847/2041-8213/ab4b56 2041

  70. [71]

    doi: 10.3847/1538-4357/ace786. F. Fontani et al.ApJL, 788:L43, June

    work page doi:10.3847/1538-4357/ace786

  71. [72]

    doi: 10.1088/2041-8205/788/2/L43. F. Fontani et al.A&A, 605:A57, Sept

    work page doi:10.1088/2041-8205/788/2/l43 2041

  72. [73]

    doi: 10.1051/0004-6361/201730527. A. Frank et al.Protostars and Planets VI, pages 451–474,

    work page doi:10.1051/0004-6361/201730527

  73. [74]

    doi: 10.2458/azu_uapress_9780816531240-ch020. R. S. Furuya et al.ApJSS, 144(1):71–134, Jan

    work page doi:10.2458/azu_uapress_9780816531240-ch020

  74. [75]

    doi: 10.1086/342749. M. Galametz et al.A&A, 632:A5, Dec

    work page doi:10.1086/342749

  75. [76]

    doi: 10.1051/0004-6361/201936342. G. Garay et al.ApJ, 459:193, Mar

    work page doi:10.1051/0004-6361/201936342

  76. [77]

    doi: 10.1086/176882. A. Garufi et al.A&A, 694:A290, Feb

    work page doi:10.1086/176882

  77. [78]

    doi: 10.1051/0004-6361/202452496. A. Garufi et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361/202452496

  78. [79]

    doi: 10.1051/0004-6361/201322541. L. Giani et al.MNRAS, 526(3):4535–4556, Dec

    doi:10.1051/0004-6361/201322541

  79. [80]

    doi: 10.1093/mnras/stad2892. L. Giani et al.MNRAS, 544(4):4043–4061, Dec

    doi:10.1093/mnras/stad2892

  80. [81]

    doi: 10.1093/mnras/staf1941. T. Giannini et al.ApJ, 814(1):52, Nov

    doi:10.1093/mnras/staf1941

Showing first 80 references.