  In a Lambda CDM Universe, galaxies grow in mass both through star formation
and through addition of already-formed stars in galaxy mergers. Because of this
partial decoupling of these two modes of galaxy growth, I discuss each
separately in this biased and incomplete review of galaxy assembly; first
giving an overview of the cosmic-averaged star formation history, and then
moving on to discuss the importance of major mergers in shaping the properties
of present-day massive galaxies. The cosmic-averaged star formation rate, when
integrated, is in reasonable agreement with the build-up of stellar mass
density. Roughly 2/3 of all stellar mass is formed during an epoch of rapid
star formation prior to z=1, with the remaining 1/3 formed in the subsequent 9
Gyr during a period of rapidly-declining star formation rate. The epoch of
important star formation in massive galaxies is essentially over. In contrast,
a significant fraction of massive galaxies undergo a major merger at z<1, as
evidenced by close pair statistics, morphologically-disturbed galaxy counts,
and the build-up of stellar mass in morphologically early-type galaxies. Each
of these methods is highly uncertain; yet, taken together, it is not
implausible that the massive galaxy population is strongly affected by late
galaxy mergers, in excellent qualitative agreement with our understanding of
galaxy evolution in a Lambda CDM Universe.
