The Emergence of Bulges and Disks in the Universe
  This thesis makes use of the imaging data from the Advanced Camera for
Surveys (ACS) of the Hubble Space Telescope (HST) in the Cosmic Evolution
Survey (COSMOS) and the Deep Extragalactic VIsible Legacy Survey (DEVILS)
field. We provide visual morphological classifications of 44,000 galaxies out
to redshift $z = 1$ and above a stellar mass of $10^{9.5} M_\odot$ (D10/ACS
sample). We perform a robust Bayesian bulge-disk decomposition analysis of the
D10/ACS sample. This study forms one of the largest morphological
classification and structural analyses catalogues in this field to date. Using
these catalogues, we explore the evolution of the stellar mass function (SMF)
and the stellar mass density (SMD) together with the stellar mass-size
relations ($M_*-R_e$) of galaxies as a function of morphological type as well
as for disks and bulges, separately. We quantify that one-third of the current
stellar mass of the Universe was formed during the last 8 Gyr. We find that the
moderate growth of the high-mass end of the SMF is dominated by the growth of
elliptical systems and that the vast majority of the stellar mass of the
Universe is locked up in disk+bulge systems at all epochs and that they
increase their contribution to the total SMD with time. The contribution of the
pure-disk morphology gradually decreases with time ($\sim40\%$), while
ellipticals increase their contribution by a factor of $1.7$ since $z = 1$. By
decomposing galaxies into disks and bulges we quantify that on average
$\sim50\%$ of the total stellar mass of the Universe at all epochs is in disk
structures with this contribution relatively unchanged since $z \sim 0.6$. With
this comes more rapid growth of pseudo-bulges and spheroids (bulges and
ellipticals) in mass. Furthermore, while the cosmic star-formation history is
declining the Universe is transitioning from a disk dominated era to ...
