[MCFCs = massive cluster-forming clumps]

Stars are born from the hierarchical fragmentation of molecular clouds. Most of them, and almost all high-mass stars (M > 8 Msun), which play a fundamental role in the galactic ecology, form in clustered systems. However, how these systems form is still under debate, as there is no agreement on how the process of fragmentation starts and proceeds, primarily in massive star-forming regions. Although recent years have witnessed considerable progress in the characterization of young embedded protostellar clusters thanks to infrared surveys, The same steps forward were not achieved for the earliest phases where protoclusters are composed of dense cores, the stellar precursors, due to the limited angular resolution and sensitivity of millimeter surveys. The ALMAGAL Large Program filled this gap by observing with ALMA at 1.4 mm and high angular resolution (~1000 au) more than 1000 massive clumps, potential sites of high-mass and cluster formation, in a wide variety of Galactic environments. In this talk, I will present the characterization of the spatial distribution of the population of dense cores identified in the ALMAGAL clumps. The large sample of clumps observed by ALMAGAL allows us for a quantitative and statistically robust analysis of the cluster of cores. Specifically, I will discuss where dense cores are located, what are their reciprocal separation, and how they are spatially distributed in the clump, which are all clues about the physical conditions of the fragmentation process. Finally, I will discuss how these properties vary over the early evolution of these systems, before the dispersal of the gas due to the stellar feedback. Our results indicate that, despite the wide diversity of observed fragmentation aspects, the distributions of dense cores are compatible with pure gravitational fragmentation without a contribution due to the turbulent support. Nonetheless, the wide observed variety requires future dedicated modeling with numerical simulations to reproduce the statistical properties of the observed distributions.

Breve CV del Dr. Eugenio Schisano:

è un ricercatore presso lo INAF-IAPS di Roma dove studia le fasi iniziali del processo di formazione stellare lavorando per nell’ambito delle grandi surveys infrarosse e millimetriche del piano Galattico. Ha conseguito il suo PhD presso l’Università “Federico II” studiando i dischi circumstellari attorno a stelle di tipo solare. Ha lavorato come post-doc allo IAPS-INAF e ad IPAC-CalTech nell’ambito delle analisi delle principali surveys del piano Galattico acquisite coi telescopi spaziali (Spitzer, Herschel, WISE), focalizzando la sua ricerca sulla struttura filamentare del materiale denso connesso alle regioni di formazione stellare. Lavora anche con dati di radiotelescopi  da terra a single-dish che interferometri alle lunghezze d’onda millimetriche, per l’analisi multifrequenza delle regioni di formaizone stellare. E’ un esperto di analisi delle immagini astronomiche, sia di continuo che in riga spettrale, e di tecniche di analisi statistica su grandi quantità di dati.