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ALMAGAL I. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy. Presentation of the survey and early results

Fuente: arXiv

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Détails bibliographiques
Auteurs principaux:	Molinari, S., Schilke, P., Battersby, C., Ho, P. T. P., Sanchez-Monge, A., Traficante, A., Jones, B., Beltran, M. T., Beuther, H., Fuller, G. A., Zhang, Q., Klessen, R. S., Walch, S., Tang, Y. -W., Benedettini, M., Elia, D., Coletta, A., Mininni, C., Schisano, E., Avison, A., Law, C. Y., Nucara, A., Soler, J. D., Stroud, G., Wallace, J., Wells, M. R. A., Ahmadi, A., Brogan, C. L., Hunter, T. R., Liu, S. -Y., Pezzuto, S., Su, Y. -N., Zimmermann, B., Zhang, T., Wyrowski, F., De Angelis, F., Liu, S., Clarke, S. D., Fontani, F., Klaassen, P. D., Koch, P., Johnston, K. G., Lebreuilly, U., Liu, T., Lumsden, S. L., Moeller, T., Moscadelli, L., Kuiper, R., Lis, D., Peretto, N., Pfalzner, S., Rigby, A. J., Sanhueza, P., Rygl, K. L. J., van der Tak, F., Zinnecker, H., Amaral, F., Bally, J., Bronfman, L., Cesaroni, R., Goh, K., Hoare, M. G., Hatchfield, P., Hennebelle, P., Henning, T., Kim, K. T., Kim, W. -J., Maud, L., Merello, M., Nakamura, F., Plume, R., Qin, S. -L., Svoboda, B., Testi, L., Veena, V. S., Walker, D.
Format:	Preprint
Publié:	2025
Sujets:	Astrophysics of Galaxies Solar and Stellar Astrophysics
Accès en ligne:	Acceder al recurso
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_version_	1866929747471106048
author	Molinari, S. Schilke, P. Battersby, C. Ho, P. T. P. Sanchez-Monge, A. Traficante, A. Jones, B. Beltran, M. T. Beuther, H. Fuller, G. A. Zhang, Q. Klessen, R. S. Walch, S. Tang, Y. -W. Benedettini, M. Elia, D. Coletta, A. Mininni, C. Schisano, E. Avison, A. Law, C. Y. Nucara, A. Soler, J. D. Stroud, G. Wallace, J. Wells, M. R. A. Ahmadi, A. Brogan, C. L. Hunter, T. R. Liu, S. -Y. Pezzuto, S. Su, Y. -N. Zimmermann, B. Zhang, T. Wyrowski, F. De Angelis, F. Liu, S. Clarke, S. D. Fontani, F. Klaassen, P. D. Koch, P. Johnston, K. G. Lebreuilly, U. Liu, T. Lumsden, S. L. Moeller, T. Moscadelli, L. Kuiper, R. Lis, D. Peretto, N. Pfalzner, S. Rigby, A. J. Sanhueza, P. Rygl, K. L. J. van der Tak, F. Zinnecker, H. Amaral, F. Bally, J. Bronfman, L. Cesaroni, R. Goh, K. Hoare, M. G. Hatchfield, P. Hennebelle, P. Henning, T. Kim, K. T. Kim, W. -J. Maud, L. Merello, M. Nakamura, F. Plume, R. Qin, S. -L. Svoboda, B. Testi, L. Veena, V. S. Walker, D.
author_facet	Molinari, S. Schilke, P. Battersby, C. Ho, P. T. P. Sanchez-Monge, A. Traficante, A. Jones, B. Beltran, M. T. Beuther, H. Fuller, G. A. Zhang, Q. Klessen, R. S. Walch, S. Tang, Y. -W. Benedettini, M. Elia, D. Coletta, A. Mininni, C. Schisano, E. Avison, A. Law, C. Y. Nucara, A. Soler, J. D. Stroud, G. Wallace, J. Wells, M. R. A. Ahmadi, A. Brogan, C. L. Hunter, T. R. Liu, S. -Y. Pezzuto, S. Su, Y. -N. Zimmermann, B. Zhang, T. Wyrowski, F. De Angelis, F. Liu, S. Clarke, S. D. Fontani, F. Klaassen, P. D. Koch, P. Johnston, K. G. Lebreuilly, U. Liu, T. Lumsden, S. L. Moeller, T. Moscadelli, L. Kuiper, R. Lis, D. Peretto, N. Pfalzner, S. Rigby, A. J. Sanhueza, P. Rygl, K. L. J. van der Tak, F. Zinnecker, H. Amaral, F. Bally, J. Bronfman, L. Cesaroni, R. Goh, K. Hoare, M. G. Hatchfield, P. Hennebelle, P. Henning, T. Kim, K. T. Kim, W. -J. Maud, L. Merello, M. Nakamura, F. Plume, R. Qin, S. -L. Svoboda, B. Testi, L. Veena, V. S. Walker, D.
contents	Fundamental questions about the physics responsible for fragmenting molecular parsec-scale clumps into cores of ~1000 au are still open, that only a statistically significant investigation with ALMA is able to address: what are the dominant agents that determine the core demographics, mass, and spatial distribution as a function of the physical properties of the hosting clumps, their evolutionary stage and the different Galactic environments in which they reside? To what extent extent is fragmentation driven by clumps dynamics or mass transport in filaments? With ALMAGAL we observed the 1.38 mm continuum and lines toward more than 1000 dense clumps in our Galaxy, with M>500M_sun, surface density > 0.1 g/cm2 and d<7.5 kpc. The ACA and two 12-m array setups were used to deliver a minimum resolution of ~1000 au over the entire sample distance range. The sample covers all evolutionary stages from infrared dark clouds (IRDCs) to HII regions from the tip of the Galactic bar to the outskirts of the Galaxy. The spectral setup includes several molecular lines to trace the multiscale physics and dynamics of gas, notably CH3CN, H2CO, SiO, CH3OH, DCN, HC3N, SO etc. We present an initial overview of the observations and the early science product and results, with a first characterization of the morphological properties of the continuum emission. We use "perimeter-versus-area" and convex hull-versus-area metrics to classify the different morphologies. More extended and morphologically complex shapes are found toward clumps that are relatively more evolved and have higher surface densities.
format	Preprint
id	arxiv_https___arxiv_org_abs_2503_05555
institution	arXiv
publishDate	2025
record_format	arxiv
spellingShingle	ALMAGAL I. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy. Presentation of the survey and early results Molinari, S. Schilke, P. Battersby, C. Ho, P. T. P. Sanchez-Monge, A. Traficante, A. Jones, B. Beltran, M. T. Beuther, H. Fuller, G. A. Zhang, Q. Klessen, R. S. Walch, S. Tang, Y. -W. Benedettini, M. Elia, D. Coletta, A. Mininni, C. Schisano, E. Avison, A. Law, C. Y. Nucara, A. Soler, J. D. Stroud, G. Wallace, J. Wells, M. R. A. Ahmadi, A. Brogan, C. L. Hunter, T. R. Liu, S. -Y. Pezzuto, S. Su, Y. -N. Zimmermann, B. Zhang, T. Wyrowski, F. De Angelis, F. Liu, S. Clarke, S. D. Fontani, F. Klaassen, P. D. Koch, P. Johnston, K. G. Lebreuilly, U. Liu, T. Lumsden, S. L. Moeller, T. Moscadelli, L. Kuiper, R. Lis, D. Peretto, N. Pfalzner, S. Rigby, A. J. Sanhueza, P. Rygl, K. L. J. van der Tak, F. Zinnecker, H. Amaral, F. Bally, J. Bronfman, L. Cesaroni, R. Goh, K. Hoare, M. G. Hatchfield, P. Hennebelle, P. Henning, T. Kim, K. T. Kim, W. -J. Maud, L. Merello, M. Nakamura, F. Plume, R. Qin, S. -L. Svoboda, B. Testi, L. Veena, V. S. Walker, D. Astrophysics of Galaxies Solar and Stellar Astrophysics Fundamental questions about the physics responsible for fragmenting molecular parsec-scale clumps into cores of ~1000 au are still open, that only a statistically significant investigation with ALMA is able to address: what are the dominant agents that determine the core demographics, mass, and spatial distribution as a function of the physical properties of the hosting clumps, their evolutionary stage and the different Galactic environments in which they reside? To what extent extent is fragmentation driven by clumps dynamics or mass transport in filaments? With ALMAGAL we observed the 1.38 mm continuum and lines toward more than 1000 dense clumps in our Galaxy, with M>500M_sun, surface density > 0.1 g/cm2 and d<7.5 kpc. The ACA and two 12-m array setups were used to deliver a minimum resolution of ~1000 au over the entire sample distance range. The sample covers all evolutionary stages from infrared dark clouds (IRDCs) to HII regions from the tip of the Galactic bar to the outskirts of the Galaxy. The spectral setup includes several molecular lines to trace the multiscale physics and dynamics of gas, notably CH3CN, H2CO, SiO, CH3OH, DCN, HC3N, SO etc. We present an initial overview of the observations and the early science product and results, with a first characterization of the morphological properties of the continuum emission. We use "perimeter-versus-area" and convex hull-versus-area metrics to classify the different morphologies. More extended and morphologically complex shapes are found toward clumps that are relatively more evolved and have higher surface densities.
title	ALMAGAL I. The ALMA evolutionary study of high-mass protocluster formation in the Galaxy. Presentation of the survey and early results
topic	Astrophysics of Galaxies Solar and Stellar Astrophysics
url	https://arxiv.org/abs/2503.05555