Olivares Romero, JavierBouy, HervéMiret Roig, NuriaGalli, P. A. B.Sarro Baro, Luis ManuelMoraux, EstelleBerihuete, Ángel2024-06-042024-06-042023-02-27The cosmic DANCe of Perseus - I. Membership, phase-space structure, mass, and energy distributions J. Olivares, H. Bouy, N. Miret-Roig, P. A. B. Galli, L. M. Sarro, E. Moraux and A. Berihuete A&A, 671 (2023) A1 DOI: https://doi.org/10.1051/0004-6361/2022450980004-6361 - eISSN 1432-0746https://doi.org/10.1051/0004-6361/202245098https://hdl.handle.net/20.500.14468/22265The registered version of this article, first published in Astronomy & Astrophysics (A&A), is available online at the publisher's website: EDP Sciences, https://doi.org/10.1051/0004-6361/202245098La versión registrada de este artículo, publicado por primera vez en Astronomy & Astrophysics (A&A), está disponible en línea en el sitio web del editor: EDP Sciences, https://doi.org/10.1051/0004-6361/202245098Context. Star-forming regions are excellent benchmarks for testing and validating theories of star formation and stellar evolution. The Perseus star-forming region, being one of the youngest (< 10 Myr), closest (280−320 pc), and most studied in the literature, is a fundamental benchmark. Aims. We aim to study the membership, phase-space structure, mass, and energy (kinetic plus potential) distribution of the Perseus star-forming region using public catalogues (Gaia, APOGEE, 2MASS, and Pan-STARRS). Methods. We used Bayesian methodologies that account for extinction to identify the Perseus physical groups in the phase-space, retrieve their candidate members, derive their properties (age, mass, 3D positions, 3D velocities, and energy), and attempt to reconstruct their origin. Results. We identify 1052 candidate members in seven physical groups (one of them new) with ages between 3 and 10 Myr, dynamical super-virial states, and large fractions of energetically unbounded stars. Their mass distributions are broadly compatible with that of Chabrier for masses ≳0.1 M⊙ and do not show hints of over-abundance of low-mass stars in NGC 1333 with respect to IC 348. These groups’ ages, spatial structure, and kinematics are compatible with at least three generations of stars. Future work is still needed to clarify if the formation of the youngest was triggered by the oldest. Conclusions. The exquisite Gaia data complemented with public archives and mined with comprehensive Bayesian methodologies allow us to identify 31% more members than previous studies, discover a new physical group (Gorgophone: 7 Myr, 191 members, and 145 M⊙), and confirm that the spatial, kinematic, and energy distributions of these groups support the hierarchical star formation scenario.en33 Ciencias Tecnológicasjournal articleopen clusters and associations: individual: Perseusstars: luminosity functionmass functionproper motionsstars: kinematics and dynamicsmethods: statisticalastrometry