ALMAGAL II. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy. ALMA data processing and pipeline

Á. Sánchez-Monge; C. L. Brogan; T. R. Hunter; A. Ahmadi; A. Avison; M. T. Beltrán; H. Beuther; A. Coletta; G. A. Fuller; K. G. Johnston; B. Jones; S. -Y. Liu; C. Mininni; S. Molinari; P. Schilke; E. Schisano; Y. -N. Su; A. Traficante; Q. Zhang; C. Battersby; M. Benedettini; D. Elia; P. T. P. Ho; P. D. Klaassen; R. S. Klessen; C. Y. Law; D. C. Lis; T. Liu; L. Maud; T. Möller; L. Moscadelli; S. Pezzuto; K. L. J. Rygl; P. Sanhueza; J. D. Soler; G. Stroud; Y. Tang; F. F. S. van der Tak; D. L. Walker; J. Wallace; S. Walch; M. R. A. Wells; F. Wyrowski; T. Zhang; J. Allande; L. Bronfman; E. Dann; F. De Angelis; F. Fontani; Th. Henning; W. -J. Kim; R. Kuiper; M. Merello; F. Nakamura; A. Nucara; A. J. Rigby

arXiv · 2503.05559

ALMAGAL II. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy. ALMA data processing and pipeline

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Abstract

The ALMAGAL Large Program has observed 1017 high-mass star-forming regions distributed throughout the Galaxy, sampling different evolutionary stages and environmental conditions. In this work, we present the acquisition and processing of the ALMAGAL data. The main goal is to set up a robust pipeline that generates science-ready products, with a good and uniform quality across the whole sample. ALMAGAL observations were performed with the Atacama Large Millimeter/submillimeter Array (ALMA). Each field was observed in three different telescope arrays, being sensitive to spatial scales ranging from 1000 au up to 0.1 pc. The spectral setup allows sensitive imaging of the continuum emission at 219 GHz, and it covers multiple molecular spectral lines observed in four different spectral windows that span about 4 GHz in frequency coverage. We have designed a Python-based processing workflow to calibrate and image these observational data. This ALMAGAL pipeline includes an improved continuum determination, suited for line-rich sources; an automatic self-calibration process that improves the dynamical range of the final images; and the combination of data from different telescope arrays to produce science-ready, fully combined images. The fully combined products have spatial resolutions in the range 800-2000 au, and mass sensitivities in the range 0.02-0.07 Mo. We also present a first analysis of the spectral line information included in the ALMAGAL setup, and its potential for future scientific studies. As an example, specific spectral lines at 1000 au scales resolve the presence of multiple outflows in clusters and will help us to search for disk candidates around massive protostars. Moreover, the broad frequency bands provide information on the chemical richness of the different cluster members, which can be used to study the chemical evolution during the formation process of star clusters.

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Á. Sánchez-Monge, C. L. Brogan, T. R. Hunter, A. Ahmadi, A. Avison, M. T. Beltrán, H. Beuther, A. Coletta, G. A. Fuller, K. G. Johnston, B. Jones, S. -Y. Liu, C. Mininni, S. Molinari, P. Schilke, E. Schisano, Y. -N. Su, A. Traficante, Q. Zhang, C. Battersby, M. Benedettini, D. Elia, P. T. P. Ho, P. D. Klaassen, R. S. Klessen, C. Y. Law, D. C. Lis, T. Liu, L. Maud, T. Möller, L. Moscadelli, S. Pezzuto, K. L. J. Rygl, P. Sanhueza, J. D. Soler, G. Stroud, Y. Tang, F. F. S. van der Tak, D. L. Walker, J. Wallace, S. Walch, M. R. A. Wells, F. Wyrowski, T. Zhang, J. Allande, L. Bronfman, E. Dann, F. De Angelis, F. Fontani, Th. Henning, W. -J. Kim, R. Kuiper, M. Merello, F. Nakamura, A. Nucara, A. J. Rigby. 2025-03-07. ALMAGAL II. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy. ALMA data processing and pipeline. https://arxiv.org/abs/2503.05559

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