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An archival summary: 15 years of ALMA observations on disks and planet formation

T0 review · 1 major / 2 minor · reviewed 2026-06-29 · grok-4.3

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Pith's one-line read ALMA has observed 3933 independent coordinates in the disks and planet formation category as of early 2026.

desk verdict This is a straightforward archive summary that counts ALMA observations in one category but adds no new science. read the letter →

arxiv 2605.30023 v1 pith:ARCYFXXI submitted 2026-05-28 astro-ph.EP

Nicolas T. Kurtovic , Lizxandra Flores-Rivera , Laura M. Perez , Miguel Vioque , Myriam Benisty , Felipe Alarcón , Marcelo Barraza-Alfaro , Pietro Curone
show 10 more authors
Kiyoaki Doi Sierra Grant Haochang Jiang Akimasa Kataoka Feng Long Álvaro Ribas Anibal Sierra Lucas Stapper Milou Temmink Francesco Zagaría
This is my paper · ORCID
classification astro-ph.EP
keywords ALMAprotoplanetarydisksplanetformationarchivalobservationssubmillimeterastronomystar-formingregionsspectrallinesurveys
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

The paper compiles statistics on all ALMA observations assigned to the disks and planet formation category during the array's first 15 years of science operations. It reports the total of 3933 distinct sky positions and examines how those data are distributed in sky location, frequency bands, integration times, spectral lines, and angular resolution. The work highlights observations toward nearby star-forming regions and is presented to enable researchers to identify and reuse existing datasets for new questions about protoplanetary disks and planet formation.

What carries the argument

The archival compilation and parameter breakdown of all ALMA pointings assigned to the 'Disks and planet formation' category.

What would settle it

A complete re-examination of ALMA proposal and execution data showing that the true number of unique coordinates in this category differs by more than a few percent from 3933.

Watch

Extended reading notes

Core claim

As of the beginning of February 2026, ALMA had observed 3933 independent coordinates in the Disks and planet formation scientific category. These observations are analyzed according to their location in the sky, frequency coverage, exposure time, spectral line coverage, and angular resolution.

Load-bearing premise

The 3933 count accurately captures all independent observations assigned to the 'Disks and planet formation' scientific category without omissions, double-counting, or misclassification of targets.

Editorial extensions

If this is right

  • New studies of disk evolution and planet formation can draw on the full existing ALMA archive rather than requiring fresh observations.
  • The tabulated properties allow efficient selection of data subsets with required frequency coverage or angular resolution.
  • Emphasis on nearby star-forming regions focuses attention on the best-resolved disks for detailed planet-formation research.

Reading between the lines

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

  • Observing proposals could use the summary to avoid redundant coverage of already-observed fields.
  • Cross-matching the 3933 coordinates with optical or infrared catalogs could identify which disks have multi-wavelength follow-up already available.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

1 major / 2 minor

Summary. The manuscript is an archival summary of ALMA observations in the 'Disks and planet formation' scientific category over nearly 15 years of operations. It reports that as of the beginning of February 2026, ALMA had observed 3933 independent coordinates in this category. These are analyzed by sky location, frequency coverage, exposure time, spectral line coverage, and angular resolution, with emphasis on disks in nearby star-forming regions, and the authors encourage community use of the archival data for new questions.

Significance. If the reported count and derived statistics are accurate, the paper provides a useful reference resource that can help researchers identify and explore existing ALMA datasets in this field. Its value is primarily practical rather than theoretical, as it contains no new physical models, predictions, or statistical inferences.

major comments (1)
  1. [Abstract and data selection section] Abstract and § on data selection (implied by the count claim): the central factual claim of exactly 3933 independent coordinates depends on the archive query, category assignment, deduplication of coordinates, and exclusion criteria. Without an explicit description of the query parameters, date range, handling of multiple executions on the same target, or verification steps, the number cannot be independently reproduced or checked for omissions or misclassifications.
minor comments (2)
  1. [Results section] The manuscript should include at least one table or figure summarizing the breakdown by frequency band or spectral line to make the 'spectral line coverage' analysis concrete.
  2. [Methods] Clarify the definition of 'independent coordinates' early in the text (e.g., unique (RA, Dec) pairs after merging overlapping pointings).

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their review and recommendation of minor revision. The manuscript aims to serve as a practical archival reference, and we agree that improving the transparency of the data selection process will strengthen its utility. We address the single major comment below.

read point-by-point responses

  1. Referee: [Abstract and data selection section] Abstract and § on data selection (implied by the count claim): the central factual claim of exactly 3933 independent coordinates depends on the archive query, category assignment, deduplication of coordinates, and exclusion criteria. Without an explicit description of the query parameters, date range, handling of multiple executions on the same target, or verification steps, the number cannot be independently reproduced or checked for omissions or misclassifications.

    Authors: We agree that the central count of 3933 requires explicit documentation for reproducibility. The revised manuscript will add a dedicated subsection under Data Selection that specifies: (1) the precise ALMA Science Archive query parameters (including scientific category filter for 'Disks and planet formation', sky coordinates, and date range up to the beginning of February 2026); (2) the method for assigning and filtering by category; (3) the deduplication algorithm for independent coordinates (including angular separation threshold); (4) handling of multiple executions, projects, or scheduling blocks on the same target; and (5) any verification steps or cross-checks performed against the archive. This addition will allow independent reproduction of the reported statistics. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity; purely descriptive archival summary

full rationale

The paper is an archival data summary whose central claim is a factual count (3933 independent coordinates) of ALMA observations in one science category, plus descriptive statistics on sky position, frequency coverage, exposure time, spectral lines, and resolution. No derivations, predictions, fitted parameters, or theoretical models are present. The work contains no equations, no self-citation chains, and no load-bearing steps that reduce to inputs by construction. The only potential failure mode is the accuracy of the external archive query itself, which is independent of any internal circularity. This is a standard honest non-finding for a descriptive catalog paper.

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

This is a review and archival summary paper; no free parameters, axioms, or invented entities are introduced to support a central scientific claim.

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Cite this review

Pith. "Pith review of An archival summary: 15 years of ALMA observations on disks and planet formation." pith.science (2026). https://pith.science/paper/ARCYFXXI

@misc{pith2026260530023,
  author       = {Pith},
  title        = {Pith review of: An archival summary: 15 years of ALMA observations on disks and planet formation},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ARCYFXXI}},
  note         = {Machine review of arXiv:2605.30023}
}
read the original abstract

The Atacama Large (sub-)millimeter Array (ALMA) has been in scientific operations for almost 15 years. We celebrate this achievement by providing a summary of the ``Disks and planet formation'' scientific category, with an emphasis on the disks located in the nearby star-forming regions. As of the beginning of February 2026, ALMA had observed 3933 independent coordinates, which we analyzed by their location in the sky, frequency coverage, exposure time, spectral line coverage, and angular resolution. We encourage the community to explore new scientific questions that are made possible through the archival datasets.

Figures

Figures reproduced from arXiv: 2605.30023 by the authors.

Figure 1
Figure 1. — Distribution of coordinates observed as part of the scientific category “Disks and planet formation”. In the top panel, the color scaling shows the accumulated exposure time per coordinate, including all ALMA Bands and time on source from other categories. The dashed line shows the coordinates where the Declination is 0, separating northern from southern sky. In the central panel there is a cut out of the galactic… view at source ↗
Figure 2
Figure 2. — Distribution of coordinates observed as part of the scientific category “Disks and planet formation”, grouped by their estimated distance from Gaia DR3 parallaxes. Note that each panel has its own colorbar, with the exception of the disks with no parallax from Gaia. ALMA, we set a maximum distance of 5′′ between phase centers to be considered as the same target. This larger threshold also avoids duplications for b… view at source ↗
Figure 3
Figure 3. — Distribution of coordinates per ALMA Band, observed as part of the scientific category “Disks and planet formation”. The color scale shows the accumulated time in each specific Band, for each coordinate. following sections, the results relative to project codes are always shown only for those in the scientific category of “Disks and planet formation”. 3. RESULTS 3.1. By coordinates We identified a total of 3933 in… view at source ↗
Figures from the paper (20 more)
Figure 4
Figure 4. Figure 4: — Sources with the longest accumulated exposure time in the ALMA Archive, considering all observations taken with the 12 m array since ALMA Cycle 0. While the sources were selected among those in the “Disks and planet formation” science category, here we integrate the …
Figure 5
Figure 5. Figure 5: — Longest single observation on a single coordinate with a specific frequency setup, excluding existing complementary configuration time (i.e., equivalent to an individual entry in the ALMA archive). Bars are colored depending on their closest relevant scientific categ…
Figure 6
Figure 6. Figure 6: — Accumulated exposure time per ALMA Band for the nearby star-forming regions. The inset shows a zoom into the area between 0 and 10 hrs of accumulated exposure time. Corona Australis and Chameleon II have ≤ 2 hrs in all Bands different from Band 6 and 7. ISO-Oph 159 I…
Figure 7
Figure 7. Figure 7: — Distribution of time among sources in the most observed nearby star-forming regions. Targets that contribute to 50% of the observed time of each region are annotated. The colorbar is saturated at 25 hrs, representing sources with more accumulated time than the approx…
Figure 8
Figure 8. Figure 8: — Distribution of accumulated exposure time per stellar mass bin. Only sources with known stellar masses are included in this figure. On the top right of each panel we show the fraction of sources with known stellar masses that have been observed in each band. The numb…
Figure 9
Figure 9. Figure 9: — Distribution of Project ID (PID) codes by observed number of coordinates, as a function of associated number of publications (from zero to ten or more). of project codes being used in 2 or more publications. This increasing fraction of project codes reaching mul￾tipl…
Figure 10
Figure 10. Figure 10: — Completeness of emission lines observations per line, per region. We include observations of at least 12 min of exposure time, with a synthesized beam larger than 0.08′′, thus representing moderate or low angular resolutions. A fraction of 1.0 means that all the coo…
Figure 11
Figure 11. Figure 11: — Fraction of time observed in full TDM (all spectral windows in TDM), mixed (spectral windows in TDM or FDM mode in the same observation), and FDM (all spectral windows in FDM), only for observations in the “Disks and planet formation” scientific category. Left panel…
Figure 12
Figure 12. Figure 12: — Completeness of high angular resolution observations (beam smaller than 0.08′′) in dust continuum emission, in the most popular ALMA Bands. A fraction of 1.0 means that all the coordinates in a region have high angular resolution observations. In the upper panel, al…
Figure 14
Figure 14. Figure 14: — Distribution of time accumulated by source. For ref￾erence, the dashed dotted horizontal line shows the total time of project code 2016.1.00484.L, and the dotted blue line shows the slope of the distribution of project codes per coordinate. The top 50 sources (from …
Figure 15
Figure 15. Figure 15: — Distribution of publication per time ratio, as a function of the total exposure time of a project code. Left panel shows publications per hour, and right panel shows publications per square root of hour. The rectangles show the 68 percentile for each bin, and the er…
Figure 17
Figure 17. Figure 17: — Publication fraction for projects in the “Disks and planet formation” category, as a function of ALMA Cycle. The dashed lines in the background represent the 20%, 50% and 80% relative to the total number of projects for that cycle. 7 8 6 8.6% 5 7.9% 4 10.9% 3 9.4% 2…
Figure 18
Figure 18. Figure 18: — Number of ALMA Bands available for the coordinates of nearby star-forming regions. For example, 46.2% of coordinates in Ophiuchus have observations in only one Band, while 10.5% have observations in two Bands [PITH_FULL_IMAGE:figures/full_fig_p017_18.png]
Figure 19
Figure 19. Figure 19: — Distribution of time per Right Ascension in bins of 3 deg (12 min of RA), separated by scientific category. The top panel shows the RA stress, which peaks at RA=10 hrs, and has two minimum between 7-9 hrs and 19-22 hrs. The lower panel shows the fraction of time per…
Figure 20
Figure 20. Figure 20: — Distribution of accumulated exposure time per stellar mass bin, as in [PITH_FULL_IMAGE:figures/full_fig_p018_20.png]
Figure 21
Figure 21. Figure 21: — Completeness of observations above 12 min on source, per stellar mass bin. The fraction above each bar shows the number of objects with more than 12 min compared to the total number of objects in that mass range [PITH_FULL_IMAGE:figures/full_fig_p019_21.png]
Figure 22
Figure 22. Figure 22: — Collection of disks with wide high-contrast asymmetries in the dust continuum emission, shown at the same spatial scale based on the Gaia DR3 parallax. The colorscale is chosen arbitrarily to highlight the substructures. These images were presented in Yamaguchi et a…
Figure 23
Figure 23. Figure 23: — Collection of disks with localized asymmetries in the dust continuum emission, shown at the same spatial scale based on the Gaia DR3 parallax. The colorscale is chosen arbitrarily to highlight the substructures. These images were presented in Ragusa et al. (2021) (I…
Figure 24
Figure 24. Figure 24: — Collection of disks with spirals in the dust continuum emission, shown at the same spatial scale based on the Gaia DR3 parallax. The colorscale is chosen arbitrarily to highlight the substructures. These images were presented in Huang et al. (2018b) (IM Lup, Elias 2…
Figure 25
Figure 25. Figure 25: — Collection of disks with substructures in dust continuum emission, available in the literature. Each panel is 400 au in size, and the disks are scaled based on the Gaia DR3 parallax, ranging from largest to smallest continuum disk from top to bottom. Further details…

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Forward citations

Cited by 1 Pith paper

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