To investigate the role of magnetic fields in the evolution of the interstellar medium,
formation and evolution of molecular clouds, and ultimately the formation of stars, their three …

We present the first Bayesian method for tomographic decomposition of the plane-of-sky
orientation of the magnetic field with the use of stellar polarimetry and distance. This …

Abstract The North Celestial Pole Loop (NCPL) provides a unique laboratory for studying the
early-stage precursors of star formation. Uncovering its origin is key to understanding the …

The heart of the Large Magellanic Cloud, 30 Doradus, is a complex region with a clear core-
halo structure. Feedback from the stellar cluster R136 has been shown to be the main …

Context. Carbon monoxide (CO) is a poor tracer of H 2 in the diffuse interstellar medium
(ISM), where most of the carbon is not incorporated into CO molecules, unlike the situation at …

High-spatial-resolution H i observations have led to the realization that the nearby (within
few hundreds of parsecs) Galactic atomic filamentary structures are aligned with the ambient …

Context. The formation of molecular gas in interstellar clouds is a slow process, but can be
enhanced by gas compression. Magneto-hydrodynamic (MHD) waves can create …

We have mapped the magnetic field (B-field) for a region of about 30 pc around the centre of
our Galaxy, which encompasses the circumnuclear disk (CND), the minispiral, and the 20 …

Magnetic fields may play a crucial role in setting the initial conditions of massive star and
star cluster formation. To investigate this, we report SOFIA-HAWC+ 214 μm observations of …

The most abundant interstellar molecule, molecular hydrogen (H 2), is practically invisible in
cold molecular clouds. Astronomers typically use carbon monoxide (CO) to trace the bulk …