Physics of the interstellar medium

Star formation is a multi-scale process, resulting from a complex interplay between gravity, turbulence, magnetic fields, and feedback mechanisms. Therefore, the key to understand the star formation process lies in obtaining an observational description of the dynamical evolution of the magnetized turbulent interstellar medium and to compare the observational results with theoretical models and numerical simulations of molecular cloud formation and evolution.

Astrophysical observations

To study the lifecycle of the interstellar medium and the physical processes leading to star formation, I use observed data sets derived from multiple telescopes such as single-dish submillimeter/radio telescopes (IRAM-30m, Nobeyama-45m, JCMT, and APEX), interferometer (ALMA), and space submillimeter/infrared telescopes (Herschel and Planck). These data trace the (column) density, the magnetic field, and the velocity structures from the large scales of clouds, to the smaller scales inside filaments and star forming cores, spanning a wide range of gas densities and evolutionary stages.

Observations and theory

To understand the physics at play in the interstellar medium, it is essential to confront the observational results with theoretical models and numerical simulations of molecular cloud formation and evolution. These simulations provide the three-dimensional structures of density, velocity and magnetic field, and allow us to trace the evolution of matter from the large diffuse clouds to the filaments and to the star-forming cores.