We conduct a detailed comparison between the kinematics, morpology and excitation conditions of the RW Aur microjet on scales < 200 AU with predictions from stationary, self-similar, cold disk wind solutions. Implications for launching and ionization mechanisms of jets in young stars are discussed.

Using archival HST/WFPC2 imaging of 7 LMC globular clusters, and following the methods outlined in our previous study, we have reached the tightest constrain so far on their age dispersion, which cannot be greater than ~ 0.5 Gyr. We also confirm earlier results that their average age is comparable to that of the metal-poor Galactic globulars

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Extensive characterisation of subsystems such as detectors and their curing, preamplifiers, filters, on-board secondary standard sources and cryomechanisms were the basis for the understanding of the assembled instrument and the development of a dedicated CALibration FACility for ISOPHOT. In the CALFAC the instrument was fully calibrated and the

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Hot subdwarf stars (hot sds) are blue subluminous objects at high galactic latitudes. They split into two well-separated spectroscopic sequences: the O (sdOs) and B-type (sdBs), according to composition and effective temperature. As they are immediate progenitors of white dwarfs (WDs), this resembles the spectroscopic H (DA)/He (DB) distinction