Pictures & Movies

Gas distribution of a 10⁸ M_☉ dwarf galaxy (stellar and dark matter distributions are not shown) simulated with 4 M_☉ gas phase elements and 0.1 pc resolution with the MFM code version (Steinwandel et al. 2019) including non-equilibrium chemistry, Strömgren photoionization and SNe from individual massive stars (see e.g. Hu et al. 2019). Red, green, and blue regions highlight molecular, neutral and ionized hydrogen, respectively. One can clearly see single and overlapping SN bubbles molecular filaments and cloud complexes as well as vertical filamentary outflow.

Large scale stellar and gas surface density, temperature and pressure maps of a gas rich dwarf galaxy merger in a starburst phase, highlighting the dynamic fidelity of the simulation code. Massive star clusters made of individual stars sampled above 4 M_☉ drive a super-bubble (Lahén et al. 2019).

Movie of the dwarf merger simulation highlighting the dynamic fidelity of the simulation code. Massive star clusters made of individual stars sampled above 4 M_☉ drive strong outflows (Lahén et al. 2019, 2020).

Hierarchical formation of a proto globular cluster (upper left) from high density gas (upper right) with low temperatures (bottom left) and high pressures (bottom right). The massive star clusters is made of individual stars sampled above 4 M_☉ and has globular cluster properties (Lahén et al. 2019).