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arxiv: 2606.27289 · v1 · pith:5PWTQAJLnew · submitted 2026-06-25 · 🌌 astro-ph.SR · astro-ph.EP

Unveiling Complex Chemistry in Planet-forming Disks with the SKAO

Linda Podio , Lisa Giani , Catherine Walsh , Audrey Coutens , Izaskun Jim\'enez-Serra , Claudio Codella , Mar\'ia Jos\'e Maureira , Marta De Simone
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John D. Ilee Manuela Lippi Chin-Fei Lee Romane Le Gal Mayank Narang Giovanni Sabatini Eleonora Bianchi Elenia Pacetti Danai Polychroni Bihan Banerjee Paola Caselli Cecilia Ceccarelli Amin Farhang Antonio Garufi Greta Guidi Adriano Ingallinera Stavro L. Ivanovski Pamela Klaassen Ana L\'opez-Sepulcre Liton Majumdar Giulia Perotti Jaime E. Pineda Daniel J. Price Manoj Puravankara Pablo Rivi\`ere-Marichalar Alvaro S\'anchez-Monge Eugenio Schisano Paolo M. Simonetti Leonardo Testi Claudia Toci Diego Turrini Alessio Traficante Yinhao Wu
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Pith reviewed 2026-06-26 02:43 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EP
keywords protoplanetary disksastrochemistrycomplex moleculesplanet formationSKAdisk midplaneprebiotic molecules
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The pith

SKA will observe heavy molecules and prebiotic species in the obscured midplanes of planet-forming disks.

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

The paper establishes that the Square Kilometre Array will access centimeter wavelengths to detect lines from heavy carbon chains, rings, and prebiotic molecules. It will also reach molecular emission from the disk midplane and inner 30 astronomical units, areas hidden by dust at shorter wavelengths. This capability will reveal the chemical starting points for planet formation, supporting predictions of what planets and their atmospheres are made of. Linking these findings to exoplanet atmospheres and Solar System chemistry could clarify how planetary systems develop.

Core claim

The advent of SKA will open new domains in the field by observing emission lines from heavier molecules including heavy carbon chains and rings and prebiotic molecules with peak emission in the cm range. Moreover SKA will probe molecular emission from regions which are obscured by dust opacity at mm wavelengths hence from the disk midplane and often from the inner 30 au region. These observations will constrain the initial conditions for disk evolution and planet formation allowing us to predict the chemical composition of the forming planets and their atmospheres.

What carries the argument

Centimeter-wavelength line emission from complex molecules in dust-obscured disk regions.

If this is right

  • Constrain the initial chemical conditions for disk evolution and planet formation
  • Allow prediction of the chemical composition of forming planets and their atmospheres
  • Enable comparison with results on exoplanet atmospheres and chemistry of pristine Solar System bodies

Where Pith is reading between the lines

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

  • Such data could help determine how much prebiotic material is available during the earliest stages of planet growth
  • Observations might distinguish chemical differences between inner and outer disk regions that affect terrestrial versus giant planets
  • Integration with future exoplanet spectroscopy could test whether disk chemistry directly imprints on planetary atmospheres

Load-bearing premise

The heavier molecules and prebiotic species have their strongest emission lines in the centimeter wavelength range that SKA can access and that the array's sensitivity and resolution will allow detection in the midplane and inner disk despite dust and line confusion.

What would settle it

No detection of the expected lines from heavy carbon chains or prebiotic molecules in the inner 30 au of disks after targeted SKA observations.

Figures

Figures reproduced from arXiv: 2606.27289 by Adriano Ingallinera, Alessio Traficante, Alvaro S\'anchez-Monge, Amin Farhang, Ana L\'opez-Sepulcre, Antonio Garufi, Audrey Coutens, Bihan Banerjee, Catherine Walsh, Cecilia Ceccarelli, Chin-Fei Lee, Claudia Toci, Claudio Codella, Danai Polychroni, Daniel J. Price, Diego Turrini, Elenia Pacetti, Eleonora Bianchi, Eugenio Schisano, Giovanni Sabatini, Giulia Perotti, Greta Guidi, Izaskun Jim\'enez-Serra, Jaime E. Pineda, John D. Ilee, Leonardo Testi, Linda Podio, Lisa Giani, Liton Majumdar, Manoj Puravankara, Manuela Lippi, Mar\'ia Jos\'e Maureira, Marta De Simone, Mayank Narang, Pablo Rivi\`ere-Marichalar, Pamela Klaassen, Paola Caselli, Paolo M. Simonetti, Romane Le Gal, Stavro L. Ivanovski, Yinhao Wu.

Figure 1
Figure 1. Figure 1: Estimated dust optical depth profiles for the IRAS16293B Class 0 disk at different frequencies. The profile at 100 GHz is estimated using the 1.3-3mm spectral index profile following the methodology in Maureira et al. (2026). Profiles at 15.4 GHz and 4.6 GHz, frequencies observable with SKAO, are estimated by extrapolating the 100 GHz profile assuming that the dust emissivity follows a power law with frequ… view at source ↗
Figure 2
Figure 2. Figure 2: The HH 212 protostellar disk observed with ALMA. The white contours show methanol (CH3OH, left), and acetaldehyde (CH3CHO, middle) emission, while the dust continuum emission is shown in colour scale, with green contours indicating the 𝜏 = 1, 3 and 5 surfaces. iCOMs emission is detected in the disk atmosphere, above the 𝜏 = 5 surface, while the dusty disk midplane is obscured (sketch on the right). Adapted… view at source ↗
Figure 3
Figure 3. Figure 3: Left panel: Sketch of the V883 Ori outbursting protostar: the luminosity increase of the central source pushes the snowline outwards (from 80 au in the midplane to 160 au in the disk surface layers), releasing iCOMs in gas-phase at dust temperatures > 100 K. However, the dust continuum optical depth in the inner 40 au screens the emission from complex organics despite their expected high column densities a… view at source ↗
Figure 4
Figure 4. Figure 4: Predicted spectra for an outbursting disk with a 0.5′′ diameter, obtained with the CASSIS software (CASSIS has been developed by IRAP-UPS/CNRS: https://cassis.irap.omp.eu). The right panel presents a zoom (on the intensity scale) of the left panel. The isotopologues of H2CO are indicated in gray, while the ones of CH3OH are in green. The other iCOMs are shown in pink, and glycine is in blue. The excitation… view at source ↗
Figure 5
Figure 5. Figure 5: Continuum maps at 220 GHz (top) and integrated intensity (moment 0) maps of HC3N (bottom) in the disks observed by the ALMA Large Program MAPS (Ilee et al., 2021). The ellipses indicate the beam sizes (identical for all integrated intensity maps). The maps are normalized and the intensity is in logarithmic and linear scales for the continuum and integrated intensity (or moment 0) maps, respectively. 5 7.5 … view at source ↗
Figure 6
Figure 6. Figure 6: Left panel: Column densities of cyanopolyynes, HC2n+1N, in the dark cloud TMC-1, in the prestellar cores L1544, Lupus-1A, L483, in the protostars L1527 and IRAS 16293. Column densities are from: Bianchi et al. (2023); Giers et al. (2023); Giani et al. (2025b) (L1544); Jaber et al. (2014); Lindberg et al. (2016); Giani et al. (2025b) (IRAS16293); Oyama et al. (2020, and references therein) for the other sou… view at source ↗
Figure 7
Figure 7. Figure 7: Left panels: Modelled fractional abundance (with respect to H2) of HC7N as a function of radius, 𝑟, and height, 𝑧, for a model with C/O = 0.5 (top), and one with C/O = 1.5 (bottom). Middle panel: Vertically-integrated column density (cm−2 ) of cyanopolyynes (HCnN) as a function of radius, 𝑟, for the model with C/O = 0.5 (solid lines), and one with C/O = 1.5 (dashed lines). Right panel: Disk-integrated line… view at source ↗
Figure 8
Figure 8. Figure 8: Diagram depicting various methods to improve the signal-to-noise of line observations from Keplerian disks: (a) the Keplerian stacking method (e.g. Yen et al., 2016), and (b) application of a matched filter (based on Loomis et al., 2018). et al. 2013) provides a predictable template over which to search for weaker line emission. Using known properties of the disk, namely the inclination and position angle … view at source ↗
Figure 9
Figure 9. Figure 9: Water gas-phase abundance (green colour scale) and column density profile (N(H2O), red solid line) in the protoplanetary disk DM Tau. The figure shows the water abundance obtained using the water BE (5600K) and 𝑣des (2×10−12 s −1 ) from Wakelam et al. (2017) (top panel), and the BE and 𝑣des distributions computed in Tinacci et al. (2023b) (bottom panel). The physical structure (temperature and density) of … view at source ↗
Figure 10
Figure 10. Figure 10: Comparison of the [CH3OH]/[H2CO] and [CH3OH]/[NH3] abundance ratios in star forming clouds, hot corinos around Class 0 protostars, inner regions of Class II disks, and comets. Adapted from Lippi et al. (2024). have largely retained their protoplanetary disk compositions and structures. Thus, comparing their chemical composition to that of star- and planet-forming regions can provide important clues into t… view at source ↗
read the original abstract

The chemical composition of planets is inherited from that of the natal protoplanetary disk at the time of planet formation. In recent years, we have made huge progress in characterizing disk chemistry. (Sub-)millimeter interferometers, such as ALMA, allowed us to detect emission lines from simple to complex organic molecules and to probe their radial and vertical distribution in disks. On the other hand, JWST has started to unveil the composition of disk ices, and line emission from the innermost disk regions. The advent of SKA will open new domains in the field, by observing emission lines from heavier molecules including heavy carbon chains and rings, and prebiotic molecules with peak emission in the cm range. Moreover, SKA will probe molecular emission from regions which are obscured by dust opacity at mm wavelengths, hence from the disk midplane, and often from the inner 30 au region. These observations will constrain the initial conditions for disk evolution and planet formation, allowing us to predict the chemical composition of the forming planets and their atmospheres. Comparison with forthcoming results on exoplanet atmospheres and on the chemistry of pristine bodies in the Solar System will provide new hints on the origin and evolution of planetary systems including our own.

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 / 0 minor

Summary. The manuscript presents a forward-looking science case arguing that the Square Kilometre Array Observatory (SKAO) will enable observations of complex chemistry in protoplanetary disks by targeting emission lines from heavy carbon chains, rings, and prebiotic molecules whose peak emission falls in the cm wavelength range, while also accessing the disk midplane and inner ~30 au regions that are obscured by dust at mm wavelengths; these data would constrain initial chemical conditions for planet formation and link to exoplanet atmospheres and Solar System bodies.

Significance. If the underlying assumptions on line frequencies, abundances, and detectability hold, the case would usefully articulate SKAO's complementary niche relative to ALMA and JWST for tracing previously inaccessible chemical reservoirs, thereby strengthening the observational basis for chemical inheritance models in planet formation.

major comments (2)
  1. [Abstract] Abstract: the central claim that SKA will detect heavier molecules and prebiotic species rests on the unquantified assertion that their strongest lines lie in the cm range accessible to SKA; no line frequencies, laboratory references, or column-density estimates are supplied to ground this statement.
  2. [Abstract] Abstract: the assertion that SKA will probe molecular emission from the dust-obscured midplane and inner 30 au lacks any optical-depth calculations, specific molecular examples, or sensitivity estimates demonstrating that cm-wavelength observations overcome the stated mm-wavelength limitations.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which highlight areas where the abstract can be strengthened with additional detail. We address each point below and will revise the abstract in the resubmitted version.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that SKA will detect heavier molecules and prebiotic species rests on the unquantified assertion that their strongest lines lie in the cm range accessible to SKA; no line frequencies, laboratory references, or column-density estimates are supplied to ground this statement.

    Authors: We agree that the abstract would benefit from explicit examples to support the claim. The manuscript body references laboratory spectra and prior observations for relevant species. We will revise the abstract to include specific line frequencies (e.g., low-J transitions of heavy carbon chains such as HC9N near 5-10 GHz), cite the corresponding laboratory references, and provide order-of-magnitude column-density estimates extrapolated from existing ALMA disk detections. revision: yes

  2. Referee: [Abstract] Abstract: the assertion that SKA will probe molecular emission from the dust-obscured midplane and inner 30 au lacks any optical-depth calculations, specific molecular examples, or sensitivity estimates demonstrating that cm-wavelength observations overcome the stated mm-wavelength limitations.

    Authors: We acknowledge that the abstract presents this advantage qualitatively. The manuscript discusses reduced dust opacity at cm wavelengths relative to mm wavelengths. We will revise the abstract to include specific molecular examples, a brief reference to optical-depth arguments drawn from the literature, and sensitivity estimates based on SKA specifications compared with ALMA performance at comparable frequencies. revision: yes

Circularity Check

0 steps flagged

No significant circularity

full rationale

The manuscript is a forward-looking science case paper with no derivations, quantitative models, fitted parameters, or predictions. Claims about SKA capabilities for molecular lines rest on external domain knowledge rather than any internal chain that reduces to the paper's own inputs. No equations, self-citations as load-bearing premises, or renamings of results appear. This is the expected outcome for a prospective review-style document.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a perspective paper outlining future observational prospects with no mathematical model, fitted parameters, or new physical postulates.

pith-pipeline@v0.9.1-grok · 5954 in / 1215 out tokens · 78771 ms · 2026-06-26T02:43:40.198334+00:00 · methodology

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Works this paper leans on

145 extracted references · 143 canonical work pages

  1. [1]

    doi: 10.1126/sciadv. 1600285. A. Andreu et al.A&A, 677:L17, Sept

    work page doi:10.1126/sciadv

  2. [2]

    doi: 10.1051/0004-6361/202347484. A. M. Arabhavi et al.Science, 384(6700):1086–1090, June

    work page doi:10.1051/0004-6361/202347484

  3. [3]

    doi: 10.1126/science.adi8147. N. Arulanantham et al.AJ, 170(2):67, Aug

    work page doi:10.1126/science.adi8147

  4. [4]

    doi: 10.3847/1538-3881/addd01. A. Bacmann et al.A&A, 541:L12, May

    work page doi:10.3847/1538-3881/addd01

  5. [5]

    doi: 10.1051/0004-6361/201219207. N. Balucani, C. Ceccarelli, and V. Taquet.Monthly Notices of the Royal Astronomical Society: Letters, 449(1):L16–L20,

    work page doi:10.1051/0004-6361/201219207

  6. [6]

    doi: 10.3847/2041-8213/acf5ec. V. Bariosco et al.MNRAS, 539(1):82–94, May

    work page doi:10.3847/2041-8213/acf5ec 2041

  7. [7]

    doi: 10.1093/mnras/staf476. E. A. Bergin et al.ApJ, 831(1):101, Nov

    work page doi:10.1093/mnras/staf476

  8. [8]

    doi: 10.3847/0004-637X/831/1/101. E. A. Bergin et al.ApJ, 965(2):147, Apr

    work page doi:10.3847/0004-637x/831/1/101

  9. [9]

    doi: 10.3847/1538-4357/ad3443. L. M. Bernabò et al.ApJ, 927(2):L22, Mar

    work page doi:10.3847/1538-4357/ad3443

  10. [10]

    doi: 10.3847/2041-8213/ac574e. E. Bianchi et al.MNRAS, 498(1):L87–L92, Nov

    work page doi:10.3847/2041-8213/ac574e 2041

  11. [11]

    doi: 10.1093/mnrasl/slaa130. E. Bianchi et al.ApJ, 944(2):208, Feb

    work page doi:10.1093/mnrasl/slaa130

  12. [12]

    doi: 10.3847/1538-4357/acb5e8. E. Bianchi et al. InAdvancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.3847/1538-4357/acb5e8

  13. [13]

    doi: 10.2458/azu_uapress_ 9780816553631-ch015. L. Boitard-Crépeau et al.ApJ, 987(2):L25, July

    work page doi:10.2458/azu_uapress_

  14. [14]

    doi: 10.3847/2041-8213/ade5aa. A. S. Booth et al.Nature Astronomy, 5:684–690, Jan

    work page doi:10.3847/2041-8213/ade5aa 2041

  15. [15]

    doi: 10.1038/s41550-021-01352-w. A. S. Booth et al.AJ, 167(4):164, Apr. 2024a. doi: 10.3847/1538-3881/ad2700. A. S. Booth et al.AJ, 167(4):165, Apr. 2024b. doi: 10.3847/1538-3881/ad26ff. A. S. Booth et al.ApJ, 986(1):L9, June

    work page doi:10.1038/s41550-021-01352-w

  16. [16]

    doi: 10.3847/2041-8213/adc7b2. R. A. Booth and J. D. Ilee.MNRAS, 487(3):3998–4011, Aug

    work page doi:10.3847/2041-8213/adc7b2 2041

  17. [17]

    doi: 10.1093/mnras/stz1488. A. D. Bosman et al.ApJS, 257(1):7, Nov. 2021a. doi: 10.3847/1538-4365/ac1435. A. D. Bosman et al.ApJS, 257(1):15, Nov. 2021b. doi: 10.3847/1538-4365/ac1433. S. Bruderer, E. F. van Dishoeck, S. D. Doty, and G. J. Herczeg.A&A, 541:A91, May

    work page doi:10.1093/mnras/stz1488

  18. [18]

    doi: 10.1051/0004-6361/201118218. A. M. Burkhardt et al.ApJ, 913(2):L18, June

    work page doi:10.1051/0004-6361/201118218

  19. [19]

    doi: 10.3847/2041-8213/abfd3a. J. K. Calahan et al.ApJ, 975(2):170, Nov

    work page doi:10.3847/2041-8213/abfd3a 2041

  20. [20]

    doi: 10.3847/1538-4357/ad78d1. M. T. Carney et al.A&A, 605:A21, Sept

    work page doi:10.3847/1538-4357/ad78d1

  21. [21]

    doi: 10.1051/0004-6361/201629342. M. T. Carney et al.A&A, 623:A124, Mar

    work page doi:10.1051/0004-6361/201629342

  22. [22]

    doi: 10.1051/0004-6361/201834353. S. Cazaux et al.ApJ, 593(1):L51–L55, Aug

    work page doi:10.1051/0004-6361/201834353

  23. [23]

    doi: 10.1086/378038. C. Ceccarelli et al. In S. Inutsuka et al., editors,Protostars and Planets VII, volume 534 of Astronomical Society of the Pacific Conference Series, page 379, July

    work page doi:10.1086/378038

  24. [24]

    doi: 10.1051/0004-6361/202141156. Y. Chen et al.A&A, 690:A205, Oct

    work page doi:10.1051/0004-6361/202141156

  25. [25]

    doi: 10.1051/0004-6361/202450706. L. A. Cieza et al.Nature, 535(7611):258–261, July

    work page doi:10.1051/0004-6361/202450706

  26. [26]

    doi: 10.1038/nature18612. C. Codella et al. InAdvancing Astrophysics with the Square Kilometre Array (AASKA14), page 26 Chemistry of planet formation with SKAO Podio et al. 123, Apr

    work page doi:10.1038/nature18612

  27. [27]

    doi: 10.22323/1.215.0123. C. Codella et al.ACS Earth and Space Chemistry, 3(10):2110–2121, Oct

    work page doi:10.22323/1.215.0123

  28. [28]

    C.Codellaetal.FrontiersinAstronomyandSpaceSciences,8:227,Dec.2021

    doi: 10.1021/ acsearthspacechem.9b00136. C.Codellaetal.FrontiersinAstronomyandSpaceSciences,8:227,Dec.2021. doi: 10.3389/fspas. 2021.782006. M. P. Collings et al.MNRAS, 354(4):1133–1140, Nov

    work page doi:10.3389/fspas 2021

  29. [29]

    doi: 10.1111/j.1365-2966.2004. 08272.x. M. A. Corazzi et al.ApJ, 913(2):128, June

    work page doi:10.1111/j.1365-2966.2004 2004

  30. [30]

    doi: 10.3847/1538-4357/abf6d3. A. Coutens et al.A&A, 590:L6, May

    work page doi:10.3847/1538-4357/abf6d3

  31. [31]

    doi: 10.1051/0004-6361/201628612. I. J. M. Crossfield.ApJ, 952(1):L18, July

    work page doi:10.1051/0004-6361/201628612

  32. [32]

    doi: 10.3847/2041-8213/ace35f. F. Cruz-Sáenz de Miera et al.A&A, 696:A18, Apr

    work page doi:10.3847/2041-8213/ace35f 2041

  33. [33]

    doi: 10.1051/0004-6361/202451487. H. M. Cuppen et al.Space Science Reviews, 212(1-2):1–58, Oct

    work page doi:10.1051/0004-6361/202451487

  34. [34]

    doi: 10.3847/1538-4365/aac886. S. Dash et al.ApJ, 932(1):20, June

    work page doi:10.3847/1538-4365/aac886

  35. [35]

    doi: 10.3847/1538-4357/ac67f0. M. De Simone et al.ApJ, 896(1):L3, June

    work page doi:10.3847/1538-4357/ac67f0

  36. [36]

    doi: 10.3847/2041-8213/ab8d41. V. Delabrosse et al.A&A, 688:A173, Aug

    work page doi:10.3847/2041-8213/ab8d41 2041

  37. [37]

    doi: 10.1051/0004-6361/202449176. C. Dominik, C. Ceccarelli, D. Hollenbach, and M. Kaufman.ApJ, 635(1):L85–L88, Dec

    work page doi:10.1051/0004-6361/202449176

  38. [38]

    doi: 10.1086/498942. A. Dutrey et al.A&A, 704:A33, Nov

    work page doi:10.1086/498942

  39. [39]

    doi: 10.1051/0004-6361/202555641. B. Edwards et al.AJ, 157(6):242, June

    work page doi:10.1051/0004-6361/202555641

  40. [40]

    C.Eistrup,C.Walsh,andE.F.vanDishoeck.A&A,595:A83,Nov.2016

    doi: 10.3847/1538-3881/ab1cb9. C.Eistrup,C.Walsh,andE.F.vanDishoeck.A&A,595:A83,Nov.2016. doi: 10.1051/0004-6361/ 201628509. C.Eistrup,C.Walsh,andE.F.vanDishoeck.A&A,613:A14,May2018. doi: 10.1051/0004-6361/ 201731302. L.E.J.Eriksson,T.Ronnet,andA.Johansen.A&A,648:A112,Apr.2021.doi: 10.1051/0004-6361/ 202039889. L. Evans et al.ApJ, 982(1):62, Mar

    work page doi:10.3847/1538-3881/ab1cb9 2016

  41. [41]

    doi: 10.3847/1538-4357/adb287. A. M. A. Fadul et al.ApJ, 988(2):L44, Aug. 2025a. doi: 10.3847/2041-8213/adec6e. A. M. A. Fadul et al.AJ, 169(6):307, June 2025b. doi: 10.3847/1538-3881/adc998. S. Ferrero et al.ApJ, 904(1):11, Nov

    work page doi:10.3847/1538-4357/adb287 2041

  42. [42]

    doi: 10.3847/1538-4357/abb953. S. Ferrero et al.MNRAS, 516(2):2586–2596, Oct

    work page doi:10.3847/1538-4357/abb953

  43. [43]

    doi: 10.1093/mnras/stac2358. W. J. Fischer et al. In S. Inutsuka et al., editors,Protostars and Planets VII, volume 534 of Astronomical Society of the Pacific Conference Series, page 355, July

    work page doi:10.1093/mnras/stac2358

  44. [44]

    doi: 10.1051/0004-6361/202554807. J. Frediani et al.A&A, 695:A78, Mar

    work page doi:10.1051/0004-6361/202554807

  45. [45]

    doi: 10.1051/0004-6361/202452191. R. T. Garrod et al.ApJS, 259(1):1, Mar

    work page doi:10.1051/0004-6361/202452191

  46. [46]

    doi: 10.3847/1538-4365/ac3131. A. Garufi et al.A&A, 645:A145, Jan

    work page doi:10.3847/1538-4365/ac3131

  47. [47]

    doi: 10.1051/0004-6361/202039483. A. Garufi et al.A&A, 658:A104, Feb

    work page doi:10.1051/0004-6361/202039483

  48. [48]

    A.Garufietal

    doi: 10.1051/0004-6361/202141264. A.Garufietal. InAdvancingAstrophysicswiththeSKA–II(AASKAII).2026. arXivsearch: Report number AASKAII/Garufi01. D. Gasman et al.A&A, 694:A147, Feb

    work page doi:10.1051/0004-6361/202141264 2026

  49. [49]

    27 Chemistry of planet formation with SKAO Podio et al

    doi: 10.1051/0004-6361/202452152. 27 Chemistry of planet formation with SKAO Podio et al. K. Gerbig, C. T. Lenz, and H. Klahr.A&A, 629:A116, Sept

    work page doi:10.1051/0004-6361/202452152

  50. [51]

    , keywords =

    L. Giani et al.MNRAS, 537(4):3861–3883, Mar. 2025a. doi: 10.1093/mnras/staf189. L. Giani et al.MNRAS, staf1941, Nov. 2025b. ISSN 0035-8711. doi: 10.1093/mnras/staf1941. K. Giers et al.A&A, 676:A78, Aug

    work page doi:10.1093/mnras/staf189

  51. [52]

    doi: 10.1051/0004-6361/202346433. T. Grassi et al.A&A, 643:A155, Nov

    work page doi:10.1051/0004-6361/202346433

  52. [53]

    doi: 10.1051/0004-6361/202039087. S. Guilloteau et al.A&A, 700:L5, Aug

    work page doi:10.1051/0004-6361/202039087

  53. [54]

    doi: 10.1051/0004-6361/202554853. T. Henning et al.PASP, 136(5):054302, May

    work page doi:10.1051/0004-6361/202554853

  54. [55]

    doi: 10.1088/1538-3873/ad3455. E. Herbst and E. F. van Dishoeck.ARA&A, 47(1):427–480, Sept

    work page doi:10.1088/1538-3873/ad3455

  55. [56]

    doi: 10.1093/mnras/218.4.761. A. Houge et al.A&A, 699:A227, July

    work page doi:10.1093/mnras/218.4.761

  56. [57]

    doi: 10.1051/0004-6361/202555164. J. D. Ilee et al.ApJS, 257(1):9, Nov

    work page doi:10.1051/0004-6361/202555164

  57. [58]

    doi: 10.3847/1538-4365/ac1441. J. D. Ilee, C. Walsh, and J. K. Calahan.AJ, 171(1):3, Jan

    work page doi:10.3847/1538-4365/ac1441

  58. [59]

    doi: 10.3847/1538-3881/ae100e. A. A. Jaber, C. Ceccarelli, C. Kahane, and E. Caux.ApJ, 791:29, Aug

    work page doi:10.3847/1538-3881/ae100e

  59. [60]

    A.JohansenandM.Lambrechts.AnnualReviewofEarthandPlanetarySciences, 45(1):359–387, Aug

    doi: 10.3847/1538-4365/ad9450. A.JohansenandM.Lambrechts.AnnualReviewofEarthandPlanetarySciences, 45(1):359–387, Aug

    work page doi:10.3847/1538-4365/ad9450

  60. [61]

    doi: 10.1146/annurev-earth-063016-020226. J. K. Jørgensen et al.A&A, 595:A117, Nov

    work page doi:10.1146/annurev-earth-063016-020226

  61. [62]

    doi: 10.1051/0004-6361/201628648. J. K. Jørgensen et al.A&A, 620:A170, Dec

    work page doi:10.1051/0004-6361/201628648

  62. [63]

    doi: 10.1051/0004-6361/201731667. I. Kamp et al.Faraday Discussions, 245:112–137, Sept

    work page doi:10.1051/0004-6361/201731667

  63. [64]

    doi: 10.1039/D3FD00013C. J. Kanwar et al.A&A, 689:A231, Sept

    work page doi:10.1039/d3fd00013c

  64. [65]

    doi: 10.1051/0004-6361/202450078. Á. Kóspál et al.ApJS, 256(2):30, Oct

    work page doi:10.1051/0004-6361/202450078

  65. [66]

    doi: 10.3847/1538-4365/ac0f09. S. Krijt et al.ApJ, 990(2):L72, Sept

    work page doi:10.3847/1538-4365/ac0f09

  66. [67]

    doi: 10.3847/2041-8213/adfbe3. C. J. Law et al.ApJS, 257(1):3, Nov

    work page doi:10.3847/2041-8213/adfbe3 2041

  67. [68]

    doi: 10.3847/1538-4365/ac1434. R. Le Gal et al.ApJ, 876(1):72, May

    work page doi:10.3847/1538-4365/ac1434

  68. [69]

    doi: 10.3847/1538-4357/ab1416. R. Le Gal et al.ApJS, 257(1):12, Nov

    work page doi:10.3847/1538-4357/ab1416

  69. [70]

    doi: 10.3847/1538-4365/ac2583. C.-F. Lee et al.Nature Astronomy, 1:0152, July 2017a. doi: 10.1038/s41550-017-0152. C.-F. Lee et al.Science Advances, 3(4):e1602935, Apr. 2017b. doi: 10.1126/sciadv.1602935. C.-F. Lee et al.ApJ, 843(1):27, July 2017c. doi: 10.3847/1538-4357/aa7757. C.-F.Lee,C.Codella,Z.-Y.Li,andS.-Y.Liu.ApJ,876(1):63,May2019a. doi: 10.3847/1...

    work page doi:10.3847/1538-4365/ac2583

  70. [71]

    doi: 10.3847/1538-4357/ac8c28. J.-E. Lee et al.Nature Astronomy, 3:314–319, Feb. 2019b. doi: 10.1038/s41550-018-0680-0. N. F. W. Ligterink et al.A&A, 647:A87, Mar

    work page doi:10.3847/1538-4357/ac8c28

  71. [72]

    doi: 10.1051/0004-6361/202039619. N. F. W. Ligterink et al.Physical Chemistry Chemical Physics (Incorporating Faraday Transac- tions), 27(37):19630–19641, Sept

    work page doi:10.1051/0004-6361/202039619

  72. [73]

    doi: 10.1039/D5CP02278A. Z.-Y. D. Lin et al.MNRAS, 501(1):1316–1335, Feb

    work page doi:10.1039/d5cp02278a

  73. [74]

    doi: 10.1093/mnras/staa3685. Z.-Y. D. Lin et al.ApJ, 951(1):9, July

    work page doi:10.1093/mnras/staa3685

  74. [75]

    doi: 10.3847/1538-4357/acd5c9. J. E. Lindberg, S. B. Charnley, and M. A. Cordiner.ApJ, 833(1):L14, Dec

    work page doi:10.3847/1538-4357/acd5c9

  75. [76]

    2041-8213/833/1/L14

    doi: 10.3847/ 28 Chemistry of planet formation with SKAO Podio et al. 2041-8213/833/1/L14. M. Lippi et al.ApJ, 970(1):L5, July

    2041

  76. [77]

    doi: 10.3847/2041-8213/ad5a6d. J.-C. Loison et al.MNRAS, 437(1):930–945, Jan

    work page doi:10.3847/2041-8213/ad5a6d 2041

  77. [78]

    doi: 10.1093/mnras/stt1956. R. A. Loomis et al.AJ, 155(4):182, Apr

    work page doi:10.1093/mnras/stt1956

  78. [79]

    doi: 10.3847/1538-3881/aab604. R. A. Loomis et al.ApJ, 893(2):101, Apr

    work page doi:10.3847/1538-3881/aab604

  79. [80]

    doi: 10.3847/1538-4357/ab7cc8. R. A. Loomis et al.Nature Astronomy, 5:188–196, Jan

    work page doi:10.3847/1538-4357/ab7cc8

  80. [81]

    doi: 10.1038/s41550-020-01261-4. A. López-Sepulcre et al.A&A, 606:A121, Oct

    work page doi:10.1038/s41550-020-01261-4

Showing first 80 references.