The Rosetta Stone project. III. ALMA synthetic observations of fragmentation in high-mass star-forming clumps
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2025
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| author | Nucara, Alice Traficante, Alessio Lebreuilly, Ugo Tung, Ngo-Duy Molinari, Sergio Hennebelle, Patrick Testi, Leonardo Klessen, Ralf S. Pelkonen, Veli-Matti Avison, Adam Benedettini, Milena Coletta, Alessandro De Angelis, Fabrizio Elia, Davide Fuller, Gary A. Jones, Bethany M. Mercimek, Seyma Mininni, Chiara Pezzuto, Stefania Pillai, Thushara Roccatagliata, Veronica Schisano, Eugenio Soler, Juan D. Suin, Paolo Toci, Claudia Walker, Daniel |
| author_facet | Nucara, Alice Traficante, Alessio Lebreuilly, Ugo Tung, Ngo-Duy Molinari, Sergio Hennebelle, Patrick Testi, Leonardo Klessen, Ralf S. Pelkonen, Veli-Matti Avison, Adam Benedettini, Milena Coletta, Alessandro De Angelis, Fabrizio Elia, Davide Fuller, Gary A. Jones, Bethany M. Mercimek, Seyma Mininni, Chiara Pezzuto, Stefania Pillai, Thushara Roccatagliata, Veronica Schisano, Eugenio Soler, Juan D. Suin, Paolo Toci, Claudia Walker, Daniel |
| contents | The physical mechanisms that regulate the collapse of high-mass parsec-scale clumps and allow them to form clusters of new stars represent a crucial aspect of star formation. To investigate these mechanisms, we developed the Rosetta Stone project: an end-to-end (simulations-observations) framework that is based on the systematic production of realistic synthetic observations of clump fragmentation and their comparison with real data. In this work, we compare ALMA 1.3mm continuum dust emission observations from the SQUALO survey with a new set of 24 radiative magnetohydrodynamical simulations of high-mass clump fragmentation, post-processed using the CASA software to mimic the observing strategy of SQUALO. The simulations were initialized combining typical values of clump mass (500,1000 solar masses) and radius (~0.4pc) with two levels of turbulence (Mach number of 7,10) and three levels of magnetization (mass-to-flux ratio of ~3,10,100). Following the clump evolution over time with two random seeds projected along three orthogonal directions, we produced a collection of 732 synthetic fields. The synthetic observations of clump fragmentation at ~7000AU revealed between 2 and 14 fragments per field. Among the initial conditions of the simulations, magnetic fields have the largest impact on the fragment multiplicity at these scales. In advanced stages of clump evolution, a lower number of fragments is preferentially associated with magnetized clumps. Fragments identified at ~7000AU correspond to individual or multiple sink particles in ~75% of the cases, suggesting that not all fragments are actively forming stars. Both sinks and fragments accrete mass throughout the whole clump evolution, favoring a scenario in which fragments are not isolated from the environment. Our study demonstrates the importance of synthetic observations in interpreting results from interferometric observations. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_11032 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Rosetta Stone project. III. ALMA synthetic observations of fragmentation in high-mass star-forming clumps Nucara, Alice Traficante, Alessio Lebreuilly, Ugo Tung, Ngo-Duy Molinari, Sergio Hennebelle, Patrick Testi, Leonardo Klessen, Ralf S. Pelkonen, Veli-Matti Avison, Adam Benedettini, Milena Coletta, Alessandro De Angelis, Fabrizio Elia, Davide Fuller, Gary A. Jones, Bethany M. Mercimek, Seyma Mininni, Chiara Pezzuto, Stefania Pillai, Thushara Roccatagliata, Veronica Schisano, Eugenio Soler, Juan D. Suin, Paolo Toci, Claudia Walker, Daniel Solar and Stellar Astrophysics Astrophysics of Galaxies Instrumentation and Methods for Astrophysics The physical mechanisms that regulate the collapse of high-mass parsec-scale clumps and allow them to form clusters of new stars represent a crucial aspect of star formation. To investigate these mechanisms, we developed the Rosetta Stone project: an end-to-end (simulations-observations) framework that is based on the systematic production of realistic synthetic observations of clump fragmentation and their comparison with real data. In this work, we compare ALMA 1.3mm continuum dust emission observations from the SQUALO survey with a new set of 24 radiative magnetohydrodynamical simulations of high-mass clump fragmentation, post-processed using the CASA software to mimic the observing strategy of SQUALO. The simulations were initialized combining typical values of clump mass (500,1000 solar masses) and radius (~0.4pc) with two levels of turbulence (Mach number of 7,10) and three levels of magnetization (mass-to-flux ratio of ~3,10,100). Following the clump evolution over time with two random seeds projected along three orthogonal directions, we produced a collection of 732 synthetic fields. The synthetic observations of clump fragmentation at ~7000AU revealed between 2 and 14 fragments per field. Among the initial conditions of the simulations, magnetic fields have the largest impact on the fragment multiplicity at these scales. In advanced stages of clump evolution, a lower number of fragments is preferentially associated with magnetized clumps. Fragments identified at ~7000AU correspond to individual or multiple sink particles in ~75% of the cases, suggesting that not all fragments are actively forming stars. Both sinks and fragments accrete mass throughout the whole clump evolution, favoring a scenario in which fragments are not isolated from the environment. Our study demonstrates the importance of synthetic observations in interpreting results from interferometric observations. |
| title | The Rosetta Stone project. III. ALMA synthetic observations of fragmentation in high-mass star-forming clumps |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies Instrumentation and Methods for Astrophysics |
| url | https://arxiv.org/abs/2507.11032 |