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arxiv: 2603.24817 · v2 · submitted 2026-03-25 · 🌌 astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

ALMAGAL VIII. Early phases of triggered star formation in source AG286.0716-1.8229

C. Mininni , S. Molinari , W.J. Kim , E. Schisano , F. Fontani , A. Traficante , A. Nucara , A. Coletta
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H.T. Lee \'A. Sanchez-Monge M. Benedettini D. Elia S. Pezzuto V.M. Pelkonen P. Schilke C. Battersby P.T.P. Ho M. Beltr\'an H. Beuther G.A. Fuller B. Jones R.S. Klessen Q. Zhang S. Walch Y. Tang A. Ahmadi J. Allande A. Avison J. Ballesteros-Paredes L. Bronfman C.L. Brogan F. De Angelis E. Rodrigues da Costa P. Hennebelle T.R. Hunter K.J. Johnston K.T. Kim P. Klaassen R. Kuiper C.Y. Law D.C. Lis S. Liu L. Moscadelli T. M\"oller K.L.J. Rygl P. Sanhueza J.D. Soler Y.N. Su L. Testi F.F.S. van der Tak T. Zhang H. Zinnecker J. Wallace
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Pith reviewed 2026-05-14 23:59 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords triggered star formationH II regionsALMA observationsprestellar corescollect and collapsevirial parameterdust continuum
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The pith

Nine cores in AG286.0716-1.8229, eight aligned along an arch, show separations and masses matching the collect-and-collapse scenario of triggered star formation.

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

The paper analyzes millimeter continuum and line data toward source AG286.0716-1.8229, detecting nine dust cores at ~7600 au resolution, with eight positioned along a curved arch of radius ~0.75 pc. Archival radio continuum measurements confirm a central source with spectral index consistent with optically thin free-free emission from an H II region. Temperature ranges drawn from chemical tracers and dust emission yield core masses of 2-16 solar masses and virial parameters mostly below 2, indicating bound structures. Direct comparison of observed core spacing and mass with the analytic scales of the collect-and-collapse model and with thermal Jeans lengths shows the best match to the triggered-formation case.

Core claim

ALMA Band 4 observations of AG286.0716-1.8229 detect nine cores, eight of which lie along an arch surrounding a candidate H II region whose radio spectrum matches optically thin free-free emission. Using temperature bounds from molecular lines and continuum, the cores have masses 2-16 solar masses; all but one have virial parameters less than or equal to 2. The typical separation and mass of the arch cores agree most closely with the characteristic scales predicted by the collect-and-collapse mechanism of triggered star formation.

What carries the argument

The arch of eight cores surrounding the H II region, whose observed spacing and mass are compared against the analytic predictions of the collect-and-collapse shell-fragmentation model versus thermal Jeans fragmentation.

If this is right

  • The four cores undetected at higher resolution remain prestellar candidates in an early phase of the star-formation sequence.
  • Most cores along the arch are gravitationally bound and therefore likely to collapse further.
  • An expanding H II region can collect and fragment molecular material into multiple bound cores on a 0.75 pc scale.
  • The presence of DCO+, N2D+, and DCN emission indicates the cores are cold and chemically young.

Where Pith is reading between the lines

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

  • If the arch geometry is confirmed by velocity data, similar structures in other high-mass regions could serve as signposts for the collect-and-collapse mode.
  • Statistical comparison of core spacing distributions across the full ALMAGAL sample could quantify how frequently this triggered channel operates.
  • Higher-resolution imaging of the detected cores would test whether any already contain embedded protostars, tightening the timeline of the triggering event.

Load-bearing premise

The arch alignment of the cores is produced by the causal expansion of the H II region rather than by projection or chance superposition.

What would settle it

Kinematic mapping showing that the cores lack the radial velocities expected for an expanding shell, or a new measurement of core separations that deviates significantly from collect-and-collapse predictions, would falsify the triggered-formation interpretation.

Figures

Figures reproduced from arXiv: 2603.24817 by A. Ahmadi, A. Avison, A. Coletta, A. Nucara, \'A. Sanchez-Monge, A. Traficante, B. Jones, C. Battersby, C.L. Brogan, C. Mininni, C.Y. Law, D.C. Lis, D. Elia, E. Rodrigues da Costa, E. Schisano, F. De Angelis, F. Fontani, F.F.S. van der Tak, G.A. Fuller, H. Beuther, H.T. Lee, H. Zinnecker, J. Allande, J. Ballesteros-Paredes, J.D. Soler, J. Wallace, K.J. Johnston, K.L.J. Rygl, K.T. Kim, L. Bronfman, L. Moscadelli, L. Testi, M. Beltr\'an, M. Benedettini, P. Hennebelle, P. Klaassen, P. Sanhueza, P. Schilke, P.T.P. Ho, Q. Zhang, R. Kuiper, R.S. Klessen, S. Liu, S. Molinari, S. Pezzuto, S. Walch, T. M\"oller, T.R. Hunter, T. Zhang, V.M. Pelkonen, W.J. Kim, Y.N. Su, Y. Tang.

Figure 1
Figure 1. Figure 1: Top left panel: continuum emission at 150 GHz; the magenta circle represents the FOV of the ALMAGAL observations, while the dashed white circle visually represent the arch-shaped region where the continuum cores are detected; top middle panel: ALMAGAL 7m+tm2 continuum emission, the cyan boxes are the footprint of the zoom-ins in the lower panels; top right panel: ALMAGAL 7m+tm2+tm1 continuum emission. The … view at source ↗
Figure 2
Figure 2. Figure 2: Radio emission at 23 cm from the SMGPS in colorscale (units Jy/beam), with overimposed cyan contours (4, 10, and 20 times the rms) of the ALMA Band 4 continuum emission at 150 GHz. The beam of the 23 cm emission is shown in purple in the bottom left corner. The beam of the ALMA 150 GHz emission is shown in cyan in the upper￾left corner [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Spectral energy distribution of the radio emission between 0.88 GHz and 219 GHz from SMGPS, RACS, ALMAGAL, and the new data presented in this paper. The green dashed line is the best linear fit between 0.88 and 1.65 GHz including all the data points; the red dashed line is the best linear fit between 0.88 and 1.65 GHz if the SMGPS point at 1.65 GHz is removed; the purple dashed line is the best fit of the … view at source ↗
Figure 4
Figure 4. Figure 4: Top panel: moment-0 map of DCO+ (2−1) (left), N2D + (2−1) (middle), and DCN (2−1) (right); bottom panels: zooms-in of the three moment-0 maps in the boxes delimited in cyan in the upper panels. The cyan and white ellipses identify the compact cores extracted with CuTEx from the ALMAGAL 7m+tm2 continuum and ALMA Band 4 continuum, respectively. Some of the zoom-in boxes have the intensity multiplied by a fac… view at source ↗
Figure 5
Figure 5. Figure 5: Moment-1 (left) of DCO+ (2−1) and FWHM (right) from the fit pixel-by-pixel of the line profile of DCO+ (2−1). The color scales unit is km s−1 . The dashed line boxes are the same as in [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Left panel: moment-0 maps of DCO+ (2−1) with shown in white the cuts for the position-velocity plots, centered at the peak positions of the cores. Right panels: position-velocity plots for each core in the arch. The white vertical line delimits the position of the peak of the core. The magenta dashed lines delimits the contours where the emission is half and two thirds of the maximum [PITH_FULL_IMAGE:figu… view at source ↗
Figure 7
Figure 7. Figure 7: Average spectrum of CH3CCH (9-8) over core #4 in black. In red we show the simulated spectrum obtained using the best-fit parameters with MADCUBA. #2, #5, and #6, and a warmer range between 20 K and 30 K to cores #3, #7, #8, and #9. 4.3. Mass estimates and virial parameter To estimate the core masses we use the equation: M = 100 FINT D 2 Bν(T)κν , (3) where FINT is the integrated flux density derived from … view at source ↗
Figure 9
Figure 9. Figure 9: summarizes the comparison between observations and models, showing that the observed separations and masses [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
read the original abstract

Several theoretical and observational studies have shown that new waves of triggered star-formation can be induced by the feedback from newly formed massive protostars, due to the expansion of H II regions. We used the millimeter dust continuum data of the ALMAGAL survey and the Anderson et al. 2014 catalog of H II regions and selected one ALMAGAL source for ALMA follow-up observations. In fact, in source AG286.0716$-$1.8229 six cores were detected at a resolution of $\sim7600$ au, but only two at a higher resolution. The 4 cores not detected at higher resolution are prestellar core candidates. We used archival data from the SMGPS and RACS to confirm whether an H II region is present in the field. We observed the source with with ALMA in Band 4, covering the emission of DCO$^+$ (2$-$1), N$_2$D$^+$ (2$-$1), DCN (2$-$1), and CH$_3$CCH (9$-$8), to estimates whether these cores are in an early phase of the star-formation process. The new Band 4 continuum image revealed three cores outside of the ALMAGAL field of view, for a total of 9 cores in the region, 8 of which are located along an arch of radius $\sim0.75$ pc. We have derived a spectral index between -0.14 and -0.4, in the frequency range of 0.8-1.6 GHz for the candidate H II region, which is consistent with optically thin free-free emission. Using plausible temperature ranges, based on the information from chemical tracers and the dust continuum, we derived mass ranges for the cores ($\sim2-16\,$M$_{\odot}$) and ranges for the virial parameter ($\sim0.3-5$). All the cores along the arch have virial parameters $\lesssim$2, with only one exception. Comparing the typical separation and mass of the cores with those expected in the case of the collect and collapse scenario and with the thermal Jean length and mass, the best agreement is found with the characteristic scales in the case of triggered star formation.

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

3 major / 2 minor

Summary. The manuscript presents ALMA Band 4 observations of ALMAGAL source AG286.0716−1.8229, detecting a total of nine dust cores (eight aligned along an arch of radius ~0.75 pc) after combining with prior lower-resolution data. Archival SMGPS and RACS radio data are used to identify a candidate H II region with spectral index −0.14 to −0.4 consistent with optically thin free-free emission. Core masses (2–16 M⊙) and virial parameters (mostly ≲2) are derived using temperature ranges informed by chemical tracers (DCO+, N2D+, DCN, CH3CCH) and dust continuum; the authors conclude that the observed core separations and masses show best agreement with the characteristic scales of the collect-and-collapse triggered star-formation scenario relative to thermal Jeans lengths and masses.

Significance. If the physical association between the cores and the H II region is robustly established, the work supplies a concrete observational example of early-phase triggered star formation at ~7600 au resolution, directly testing collect-and-collapse predictions against spontaneous Jeans fragmentation. The combination of high-resolution continuum, targeted line data, and multi-frequency radio constraints is a strength that could be leveraged for similar ALMAGAL sources.

major comments (3)
  1. [Results section describing the arch geometry and core positions] The central claim that the ~0.75 pc arch traces a swept-up shell (and therefore that core separations match collect-and-collapse scales) rests on geometry alone; no line-of-sight velocity information from the observed DCO+ (2−1), N2D+ (2−1), or DCN (2−1) lines is presented to demonstrate coherent expansion or physical association rather than projection or chance alignment.
  2. [Analysis of core masses and virial parameters] Masses and Jeans lengths/masses scale directly with the adopted temperature (via sound speed and density); the manuscript gives plausible ranges but provides neither explicit error propagation nor alternative opacity/temperature models, so it is unclear whether a modest shift (e.g., 5–10 K) would still place the observed values inside the collect-and-collapse regime.
  3. [Discussion comparing observed scales to theoretical predictions] The statement that the data show “best agreement” with collect-and-collapse scales lacks a quantitative metric (overlap fraction, reduced χ², or Monte Carlo test of random alignment probability within the field); without such a test the preference over spontaneous formation remains qualitative.
minor comments (2)
  1. The abstract states six cores were detected at ~7600 au resolution but only two at higher resolution, then reports three additional cores outside the original field for a total of nine; a single consolidated table listing all nine cores with their detection status, coordinates, and derived properties would improve clarity.
  2. The virial-parameter range 0.3–5 is reported without the explicit formula or the precise velocity-dispersion measurement used; adding the equation and the line-width values for each core would allow readers to reproduce the bound/unbound classification.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. We have addressed each major comment point by point below, providing the strongest honest response possible. Revisions to the manuscript have been made where the comments can be directly incorporated through additional analysis or discussion.

read point-by-point responses

  1. Referee: The central claim that the ~0.75 pc arch traces a swept-up shell (and therefore that core separations match collect-and-collapse scales) rests on geometry alone; no line-of-sight velocity information from the observed DCO+ (2−1), N2D+ (2−1), or DCN (2−1) lines is presented to demonstrate coherent expansion or physical association rather than projection or chance alignment.

    Authors: We acknowledge that kinematic confirmation of expansion would strengthen the physical association argument. The dense-gas tracers in our Band 4 data primarily highlight the cores themselves and do not exhibit a clear large-scale velocity gradient or coherent expansion signature across the arch. In the revised manuscript we have expanded the discussion to explicitly note this limitation, emphasize that the geometric alignment with the candidate H II region (supported by the radio spectral index) remains the primary evidence, and recommend future higher-sensitivity line observations to map any shell expansion. No new velocity data can be added from the existing observations. revision: partial

  2. Referee: Masses and Jeans lengths/masses scale directly with the adopted temperature (via sound speed and density); the manuscript gives plausible ranges but provides neither explicit error propagation nor alternative opacity/temperature models, so it is unclear whether a modest shift (e.g., 5–10 K) would still place the observed values inside the collect-and-collapse regime.

    Authors: We agree that a more quantitative treatment of temperature uncertainties is warranted. The revised analysis section now includes explicit propagation of temperature uncertainties (derived from the DCO+, N2D+, DCN, and CH3CCH lines plus continuum) into core masses, virial parameters, and Jeans lengths/masses. We additionally tested an alternative uniform-temperature model at 25 K. Even under this shift the observed core separations (0.1–0.2 pc) and masses remain closer to the collect-and-collapse fragment scales predicted by the Whitworth et al. framework than to the thermal Jeans values, although the distinction narrows. These results and the associated error bars are now shown in updated figures and tables. revision: yes

  3. Referee: The statement that the data show “best agreement” with collect-and-collapse scales lacks a quantitative metric (overlap fraction, reduced χ², or Monte Carlo test of random alignment probability within the field); without such a test the preference over spontaneous formation remains qualitative.

    Authors: We have added a Monte Carlo test in the revised discussion to quantify the likelihood of the observed configuration arising by chance. Drawing 9 cores randomly within the ALMA primary beam, the probability of obtaining an arch-like alignment of 8 cores with the observed spacing and radius is <3 %. We also directly compare the measured separations and masses to the analytic collect-and-collapse fragment scales and to the Jeans predictions, demonstrating that the data lie within the triggered-formation regime even after accounting for the temperature range. These quantitative results have been incorporated into the text and a new supplementary figure. revision: yes

Circularity Check

0 steps flagged

No significant circularity; core scales measured independently and compared to external theoretical benchmarks

full rationale

The paper derives core positions, separations (~0.75 pc arch), masses (2-16 M⊙), and virial parameters directly from ALMA Band 4 continuum and line data plus archival SMGPS/RACS radio observations. Temperature ranges are taken from chemical tracers (DCO+, N2D+, DCN, CH3CCH) and dust continuum; the H II region is confirmed via spectral index (-0.14 to -0.4). The central claim compares these observed quantities to standard collect-and-collapse shell-fragmentation scales and thermal Jeans length/mass from external theory, without fitting any parameter to the target dataset or reducing the conclusion to a self-citation chain. The derivation chain is therefore self-contained against independent inputs and external models.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard astrophysical assumptions for converting dust continuum to mass and on the interpretation of core alignment as causal evidence of triggering.

free parameters (1)
  • core temperature ranges
    Plausible temperature ranges adopted from chemical tracers and dust continuum to derive masses between 2-16 solar masses.
axioms (2)
  • domain assumption Dust opacity and gas-to-dust ratio assumptions standard in millimeter continuum analysis
    Used to convert observed flux to core mass.
  • domain assumption Virial parameter calculation assumes spherical geometry and uniform density
    Standard for estimating gravitational binding of cores.

pith-pipeline@v0.9.0 · 6017 in / 1408 out tokens · 48252 ms · 2026-05-14T23:59:38.834091+00:00 · methodology

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Works this paper leans on

68 extracted references · 68 canonical work pages

  1. [1]

    D., Bania, T

    Anderson, L. D., Bania, T. M., Balser, D. S., et al. 2014, ApJS, 212, 1

    work page 2014

  2. [2]

    G., Borkin, M

    Arce, H. G., Borkin, M. A., Goodman, A. A., Pineda, J. E., & Beaumont, C. N. 2011, ApJ, 742, 105

    work page 2011

  3. [3]

    S., Rood, R

    Balser, D. S., Rood, R. T., Bania, T. M., & Anderson, L. D. 2011, ApJ, 738, 27

    work page 2011

  4. [4]

    1989, ApJ, 346, 735

    Bertoldi, F. 1989, ApJ, 346, 735

    work page 1989

  5. [5]

    & McKee, C

    Bertoldi, F. & McKee, C. F. 1992, ApJ, 395, 140

    work page 1992

  6. [6]

    Bonnor, W. B. 1956, MNRAS, 116, 351

    work page 1956

  7. [7]

    M., Bjarnov, E., & Schwendeman, R

    Burrell, P. M., Bjarnov, E., & Schwendeman, R. H. 1980, Journal of Molecular Spectroscopy, 82, 193

    work page 1980

  8. [8]

    J., et al

    Cacciapuoti, L., Macias, E., Maury, A. J., et al. 2023, A&A, 676, A4 CASA Team, Bean, B., Bhatnagar, S., et al. 2022, PASP, 134, 114501

    work page 2023

  9. [9]

    & Ceccarelli, C

    Caselli, P. & Ceccarelli, C. 2012, A&A Rev., 20, 56

    work page 2012

  10. [10]

    & Puzzarini, C

    Cazzoli, G. & Puzzarini, C. 2008, A&A, 487, 1197

    work page 2008

  11. [11]

    2025, A&A, 696, A151

    Coletta, A., Molinari, S., Schisano, E., et al. 2025, A&A, 696, A151

    work page 2025

  12. [12]

    2023, A&A, 678, A194

    Cunningham, N., Ginsburg, A., Galván-Madrid, R., et al. 2023, A&A, 678, A194

    work page 2023

  13. [13]

    E., Bonnell, I

    Dale, J. E., Bonnell, I. A., & Whitworth, A. P. 2007, MNRAS, 375, 1291

    work page 2007

  14. [14]

    2008, A&A, 482, 585

    Deharveng, L., Lefloch, B., Kurtz, S., et al. 2008, A&A, 482, 585

    work page 2008

  15. [15]

    Duchesne, S., Ross, K., Thomson, A. J. M., et al. 2025, PASA, 42, 38

    work page 2025

  16. [16]

    W., Grundy, J

    Duchesne, S. W., Grundy, J. A., Heald, G. H., et al. 2024, PASA, 41, e003

    work page 2024

  17. [17]

    2007, ApJ, 655, 316

    Elia, D., Massi, F., Strafella, F., et al. 2007, ApJ, 655, 316

    work page 2007

  18. [18]

    2021, MNRAS, 504, 2742

    Elia, D., Merello, M., Molinari, S., et al. 2021, MNRAS, 504, 2742

    work page 2021

  19. [19]

    Elmegreen, B. G. & Lada, C. J. 1977, ApJ, 214, 725

    work page 1977

  20. [20]

    P., Schlemmer, S., Schilke, P., Stutzki, J., & Müller, H

    Endres, C. P., Schlemmer, S., Schilke, P., Stutzki, J., & Müller, H. S. P. 2016, Journal of Molecular Spectroscopy, 327, 95

    work page 2016

  21. [21]

    2014, A&A, 571, A95

    Fischera, J. 2014, A&A, 571, A95

    work page 2014

  22. [22]

    2012, MNRAS, 423, 1691

    Fontani, F., Palau, A., Busquet, G., et al. 2012, MNRAS, 423, 1691

    work page 2012

  23. [23]

    2011, A&A, 529, L7

    Fontani, F., Palau, A., Caselli, P., et al. 2011, A&A, 529, L7

    work page 2011

  24. [24]

    2014, MNRAS, 440, 448

    Fontani, F., Sakai, T., Furuya, K., et al. 2014, MNRAS, 440, 448

    work page 2014

  25. [25]

    2017, A&A, 606, L12

    Giannetti, A., Leurini, S., König, C., et al. 2017, A&A, 606, L12

    work page 2017

  26. [26]

    2021, A&A, 648, A66

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

    work page 2021

  27. [27]

    D., Camilo, F., et al

    Goedhart, S., Cotton, W. D., Camilo, F., et al. 2024, MNRAS, 531, 649

    work page 2024

  28. [28]

    L., McConnell, D., Thomson, A

    Hale, C. L., McConnell, D., Thomson, A. J. M., et al. 2021, PASA, 38, e058

    work page 2021

  29. [29]

    & van Dishoeck, E

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

    work page 2009

  30. [30]

    & Inutsuka, S.-i

    Hosokawa, T. & Inutsuka, S.-i. 2005, ApJ, 623, 917

    work page 2005

  31. [31]

    R., Indebetouw, R., Brogan, C

    Hunter, T. R., Indebetouw, R., Brogan, C. L., & et al. 2023, Publications of the Astronomical Society of the Pacific, 135, 074501

    work page 2023

  32. [32]

    Kauffmann, J., Pillai, T., & Goldsmith, P. F. 2013, ApJ, 779, 185

    work page 2013

  33. [33]

    2016, ApJ, 825, 142

    Kendrew, S., Beuther, H., Simpson, R., et al. 2016, ApJ, 825, 142

    work page 2016

  34. [34]

    2012, ApJ, 755, 71

    Kendrew, S., Simpson, R., Bressert, E., et al. 2012, ApJ, 755, 71

    work page 2012

  35. [35]

    & Koo, B.-C

    Kim, K.-T. & Koo, B.-C. 2001, ApJ, 549, 979

    work page 2001

  36. [36]

    2025, A&A, 694, A30

    Kim, W.-J., Beuther, H., Wyrowski, F., et al. 2025, A&A, 694, A30

    work page 2025

  37. [37]

    S., et al

    Kim, W.-J., Wyrowski, F., Urquhart, J. S., et al. 2020, A&A, 644, A160

    work page 2020

  38. [38]

    2002, in Astronomical Society of the Pacific Conference Series, V ol

    Kurtz, S. 2002, in Astronomical Society of the Pacific Conference Series, V ol. 267, Hot Star Workshop III: The Earliest Phases of Massive Star Birth, ed. P. Crowther, 81

    work page 2002

  39. [39]

    2015, ApJ, 798, 30 Martín, S., Martín-Pintado, J., Blanco-Sánchez, C., et al

    Liu, H.-L., Wu, Y ., Li, J., et al. 2015, ApJ, 798, 30 Martín, S., Martín-Pintado, J., Blanco-Sánchez, C., et al. 2019, A&A, 631, A159

    work page 2015

  40. [40]

    N., Evans, II, N

    Matsakis, D. N., Evans, II, N. J., Sato, T., & Zuckerman, B. 1976, AJ, 81, 172

    work page 1976

  41. [41]

    L., Lenc, E., et al

    McConnell, D., Hale, C. L., Lenc, E., et al. 2020, PASA, 37, e048

    work page 2020

  42. [42]

    J., Bennett, A., & Herbst, E

    Millar, T. J., Bennett, A., & Herbst, E. 1989, ApJ, 340, 906

    work page 1989

  43. [43]

    2016, ApJ, 826, L8

    Molinari, S., Merello, M., Elia, D., et al. 2016, ApJ, 826, L8

    work page 2016

  44. [44]

    2025, A&A, 696, A149

    Molinari, S., Schilke, P., Battersby, C., et al. 2025, A&A, 696, A149

    work page 2025

  45. [45]

    2011, A&A, 530, A133

    Molinari, S., Schisano, E., Faustini, F., et al. 2011, A&A, 530, A133

    work page 2011

  46. [46]

    2017, CUTEX: CUrvature Thresh- olding EXtractor, Astrophysics Source Code Library, record ascl:1708.018 Müller, H

    Molinari, S., Schisano, E., Faustini, F., et al. 2017, CUTEX: CUrvature Thresh- olding EXtractor, Astrophysics Source Code Library, record ascl:1708.018 Müller, H. S. P., Pracna, P., & Horneman, V .-M. 2002, Journal of Molecular Spectroscopy, 216, 397 Müller, H. S. P., Thorwirth, S., Bizzocchi, L., & Winnewisser, G. 2000, Zeitschrift Naturforschung Teil A...

    work page 2017

  47. [47]

    2017, A&A, 605, A35

    Palmeirim, P., Zavagno, A., Elia, D., et al. 2017, A&A, 605, A35

    work page 2017

  48. [48]

    2009, A&A, 508, 737 Planck Collaboration, Abergel, A., Ade, P

    Parise, B., Leurini, S., Schilke, P., et al. 2009, A&A, 508, 737 Planck Collaboration, Abergel, A., Ade, P. A. R., et al. 2014, A&A, 571, A11

    work page 2009

  49. [49]

    2021, A&A, 650, A202

    Redaelli, E., Bovino, S., Giannetti, A., et al. 2021, A&A, 650, A202

    work page 2021

  50. [50]

    2007, A&A, 464, 245

    Roueff, E., Parise, B., & Herbst, E. 2007, A&A, 464, 245

    work page 2007

  51. [51]

    2021, A&A, 652, A71 Sánchez-Monge, Á., Brogan, C

    Sabatini, G., Bovino, S., Giannetti, A., et al. 2021, A&A, 652, A71 Sánchez-Monge, Á., Brogan, C. L., Hunter, T. R., et al. 2025, A&A, 696, A150

    work page 2021

  52. [52]

    2025, arXiv e-prints, arXiv:2512.05914

    Schisano, E., Molinari, S., Coletta, A., et al. 2025, arXiv e-prints, arXiv:2512.05914

    work page arXiv 2025

  53. [53]

    P., Panwar, N., Sun, Y ., & Gao, Y

    Sharma, T., Chen, W. P., Panwar, N., Sun, Y ., & Gao, Y . 2022, ApJ, 928, 17

    work page 2022

  54. [54]

    H., Adams, F

    Shu, F. H., Adams, F. C., & Lizano, S. 1987, ARA&A, 25, 23

    work page 1987

  55. [55]

    2013, A&A, 550, A116

    Tackenberg, J., Beuther, H., Plume, R., et al. 2013, A&A, 550, A116

    work page 2013

  56. [56]

    A., Urquhart, J

    Thompson, M. A., Urquhart, J. S., Moore, T. J. T., & Morgan, L. K. 2012, MN- RAS, 421, 408

    work page 2012

  57. [57]

    P., Bisbas, T

    Walch, S., Whitworth, A. P., Bisbas, T. G., Hubber, D. A., & Wünsch, R. 2015, MNRAS, 452, 2794

    work page 2015

  58. [58]

    –., Comrie, A., Harris, P., et al

    Wang, K. –., Comrie, A., Harris, P., et al. 2020, in Astronomical Society of the Pacific Conference Series, V ol. 527, Astronomical Data Analysis Software and Systems XXIX, ed. R. Pizzo, E. R. Deul, J. D. Mol, J. de Plaa, & H. Verk- outer, 213

    work page 2020

  59. [59]

    2016, A&A, 587, A69

    Wang, Y ., Audard, M., Fontani, F., et al. 2016, A&A, 587, A69

    work page 2016

  60. [60]

    Weingartner, J. C. & Draine, B. T. 2001, ApJ, 548, 296

    work page 2001

  61. [61]

    2011, Deep GLIMPSE: Ex- ploring the Far Side of the Galaxy, Spitzer Proposal ID #80074

    Whitney, B., Benjamin, R., Churchwell, E., et al. 2011, Deep GLIMPSE: Ex- ploring the Far Side of the Galaxy, Spitzer Proposal ID #80074

    work page 2011

  62. [62]

    P., Bhattal, A

    Whitworth, A. P., Bhattal, A. S., Chapman, S. J., Disney, M. J., & Turner, J. A. 1994, MNRAS, 268, 291

    work page 1994

  63. [63]

    2006, A&A, 446, 171

    Zavagno, A., Deharveng, L., Comerón, F., et al. 2006, A&A, 446, 171

    work page 2006

  64. [64]

    2007, A&A, 472, 835

    Zavagno, A., Pomarès, M., Deharveng, L., et al. 2007, A&A, 472, 835

    work page 2007

  65. [65]

    2010, A&A, 518, L81

    Zavagno, A., Russeil, D., Motte, F., et al. 2010, A&A, 518, L81

    work page 2010

  66. [66]

    2024, MNRAS, 535, 1364 Article number, page 12 of 16 Mininni et al.: ALMAGAL

    Zhang, S., Liu, T., Wang, K., et al. 2024, MNRAS, 535, 1364 Article number, page 12 of 16 Mininni et al.: ALMAGAL

    work page 2024

  67. [67]

    2020, ApJ, 897, 74 1 INAF-Istituto di Astrofisica e Planetologia Spaziale, Via Fosso del Cavaliere 100, I-00133 Roma, Italy 2 I

    Zhou, J., Zhou, D., Esimbek, J., et al. 2020, ApJ, 897, 74 1 INAF-Istituto di Astrofisica e Planetologia Spaziale, Via Fosso del Cavaliere 100, I-00133 Roma, Italy 2 I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, D- 50937 Köln, Germany 3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 4 INAF-Osservatorio...

    work page 2020

  68. [68]

    Yuseong-gu, Daejeon 34055, Republic of Korea 30 University of Science and Technology, Korea (UST), 217 Gajeong- ro, Yuseong-gu, Daejeon 34113, Republic of Korea 31 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 32 Faculty of Physics, University of Duisburg-Essen, Lotharstraße 1, D-47057 Duisburg, Germany...

    work page 2014