MOTTE, F.; NONY, T.; LOUVET, F.; MARSH, K. A.; BONTEMPS, Sylvain; WHITWORTH, A. P.; MEN'SHCHIKOV, A.; LUONG, Q. Nguyen; CSENGERI, T.; MAURY, A. J.; GUSDORF, A.; CHAPILLON, E.; KÖNYVES, V.; SCHILKE, P.; DUARTE-CABRAL, A.; DIDELON, P.; GAUDEL, M.

doi:10.1038/s41550-018-0452-x

Métadonnées

Afficher la notice complète

Licence d’utilisation du document

MOTTE, F.
Institut de Planétologie et d'Astrophysique de Grenoble [IPAG]

NONY, T.
Institut de Planétologie et d'Astrophysique de Grenoble [IPAG]

LOUVET, F.
Universidad de Santiago de Chile [Santiago] [USACH]

Langue

Article de revue

Ce document a été publié dans

Nature Astronomy. 2018, vol. 2, p. 478-482

Nature Publishing Group

Résumé en anglais

Understanding the processes that determine the stellar Initial Mass Function (IMF) is a critical unsolved problem, with profound implications for many areas of astrophysics. In molecular clouds, stars are formed in cores, gas condensations which are sufficiently dense that gravitational collapse converts a large fraction of their mass into a star or small clutch of stars. In nearby star-formation regions, the core mass function (CMF) is strikingly similar to the IMF, suggesting that the shape of the IMF may simply be inherited from the CMF. Here we present 1.3 mm observations, obtained with ALMA, the world's largest interferometer, of the active star-formation region W43-MM1, which may be more representative of the Galactic-disk regions where most stars form. The unprecedented resolution of these observations reveals, for the first time, a statistically robust CMF at high masses, with a slope that is markedly shallower than the IMF. This seriously challenges our understanding of the origin of the IMF.< Réduire

DOI

http://dx.doi.org/10.1038/s41550-018-0452-x

Projet Européen

A Gaia and Herschel Study of the Density Distribution and Evolution of Young Massive Star Clusters
Interpreting Dust Polarization Maps to Characterize the Role of the Magnetic Field in Star Formation Processes

Origine

Importé de hal

Unités de recherche

Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804