This project aims at modelling self-consistently a piece of galaxy as described in Hennebelle & Iffrig 2014, A&A, 570, 80 and Iffrig & Hennebelle 2017, A&A, 604, 70 and to zoom onto dense cores. It is described in Hennebelle 2018, A&A, 611, 24. Computational boxes of about 1 kpc are considered. An external gravitational potential, due to the dark matter and stellar component of the galaxies is added and induce the disk stratification. Self-gravity, atomic cooling, magnetic field are all included. Stellar feedback is included through supernovae remnants, which explode immediatly after a massive star formed. Momentum is injected. These models provide a reasonable description of the interstellar medium in Milky way type galaxies from a few 100 pc down to a few hundreds of AU (as intensive adaptive mesh is being used here). Note however that the hot ionised coronal phase is not well described and consequently the galactic outflows are also not well described. These models typically lead to a reasonable population of dense cores.
This project provides images of column density, density, temperature and magnetic field. Distribution of mass, density, temperature and magnetic field are given. Cores have been extracted using the HOP algorithm and their statistical properties (such as mass, internal velocity dispersion, size...) can be obtained. The cooresponding statistics are also available. It is possible to query the clumps by specifying some requested properties. Finally the full clump data can be extracted and downloaded on demand.
