Revisiting the evolved hypergiants in the Magellanic Clouds
  The massive stars that survive the phase of red supergiants (RSGs) spend the
rest of their life in extremity. Their unstable atmospheres facilitate the
formation and episodic ejection of shells that alter the stellar appearance and
surroundings. In the present study, we revise the evolutionary state of eight
hypergiants in the Magellanic Clouds, four of early-A type and four of FG type,
and complement the short list of the eruptive post-RSGs termed as yellow
hypergiants (YHGs). We refine the outdated temperatures and luminosities of the
stars by means of high-resolution spectroscopy with FEROS. The A-type stars are
suggested to be in their early, post-main sequence phase, showing
spectrophotometric characteristics of redward evolving supergiants. On the
other hand, the FG-type stars manifest themselves through the enhanced
atmospheric activity that is traced by emission filling in H$\alpha$ and the
dynamical modulation of the low-excitation BaII line. Of these stars, the dusty
HD269723 is suggested to have recently departed from a cool phase. We identify
double-peaked emission in the FEROS data of HD269953 that emerges from an
orbiting disk-hosting companion. The highlight of the study is an episode of
enhanced mass loss of HD271182 that manifests as a dimming event in the
lightcurve and renders the star "modest" analogue to $\rho$ Cas. The luminosity
$\log(L/L_{\odot})= 5.6$ of HD271182 can serve as an updated threshold for the
luminosity of stars exhibiting a post-RSG evolution in the Large Magellanic
Cloud.
