Galaxy groups are not scaled down versions of massive galaxy clusters - the hot gas in groups [known as the intragroup medium (IGrM)] is, on average, less dense than the intracluster medium, implying that one or more non-gravitational processes (e.g. radiative cooling, star formation and/or feedback) has had a relatively larger effect on groups. In

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We undertake the first high-resolution spectroscopic study of the Triangulum-Andromeda (TriAnd) star cloud—an extended, mid-latitude Milky Way (MW) halo substructure about 20 kpc away in the second Galactic quadrant— through six M giant star candidates selected to be both spatially and dynamically associated with this system. The abundance patterns

By tracing the distribution of cool dust in the extended envelopes of post-asymptotic giant branch stars and (proto)-planetary nebulae ((P)PNe), we aim to recover, or constrain, the mass-loss history experienced by these stars in their recent past. The Far-Infrared Surveyor (FIS) instrument on board the AKARI satellite was used to obtain far

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Over the last few years a large set of spectropolarimetric observations of prominences and spicules in the He I D3 multiplet have been collected at the observatory of the Istituto Ricerche Solari Locarno (IRSOL), using increasingly improved versions of the ZIMPOL polarimeter. The novel HAZEL inversion code of Stokes profiles generated by the joint