## Li & Klein (2019) – Magnetized interstellar molecular clouds: II. The Large-Scale Structure and Dynamics of Filamentary Molecular Clouds

Ideal MHD high resolution AMR simulations with driven turbulence and self-gravity have been performed that demonstrate the formation of long filamentary molecular clouds at the converging location of large-scale turbulence

## Punanova et al. (2018) – Kinematics of dense gas in the L1495 filament

We study the kinematics of the dense gas of starless and protostellar cores traced by the N2D+(2-1), N2H+(1-0), DCO+(2-1), and H13CO+(1-0) transitions along the L1495 filament and the kinematic links

## Grossschedl et al. (2018) – 3D shape of Orion A from Gaia DR2

We use the $\mathit{Gaia}$ DR2 distances of about 700 mid-infrared selected young stellar objects in the benchmark giant molecular cloud Orion A to infer its 3D shape and orientation. We

## Mattern et al. (2018) – SEDIGISM: The kinematics of ATLASGAL filaments

Analysing the kinematics of filamentary molecular clouds is a crucial step towards understanding their role in the star formation process. Therefore, we study the kinematics of 283 filament candidates in

## Körtgen et al. (2018) – The Origin of Filamentary Star Forming Clouds in Magnetised Galaxies

Observations show that galaxies and their interstellar media are pervaded by strong magnetic fields with energies in the diffuse component being at least comparable to the thermal and even as

## Zucker, Battersby & Goodman (2018) – The Physical Properties of Large-Scale Galactic Filaments

The characterization of our Galaxy’s longest filamentary gas features has been the subject of several studies in recent years, producing not only a sizeable sample of large-scale filaments, but also

## Wareing et al. (2016) – Magnetohydrodynamical simulation of the formation of clumps and filaments in quiescent diffuse medium by thermal instability

We have used the adaptive mesh refinement hydrodynamic code, MG, to perform idealized 3D magnetohydrodynamical simulations of the formation of clumpy and filamentary structure in a thermally unstable medium without