  Using the OH-airglow suppressor spectrograph at the University of Hawaii 2.2m
telescope and the CGS4 spectrometer at the United Kingdom Infrared Telescope,
we have found exceptionally large Balmer decrements in two unusual high-z QSOs,
Hawaii 167 (z=2.36, Ha/Hb = 13) and Q0059-2735 (z=1.59, Ha/Hb = 7.6), the
latter being a so-called low-ionization broad absorption line QSO (BALQSO). We
argue that these objects are young QSOs heavily enshrouded by dust. In fact,
the internal reddening might be so large as to completely extinguish the QSO
light in the restframe UV, allowing us to see the underlying stellar
population. Our possible detection of the 4000 A break in Hawaii 167 supports
this idea. Its small amplitude indicates a very young age for the population,
~15 Myrs. To explain the properties of these QSOs, we propose a model in which
a young QSO is surrounded by a shell of young massive stars mixed with
significant amounts of dust. We predict that as the QSO emerges from this dust
cocoon, it will eventually take on the appearance of a normal BALQSO.
