Observing and Simulating Galaxy Evolution - from X-ray to Millimeter
  Wavelengths
  What main mechanisms set the star formation rate (SFR) of galaxies? This PhD
thesis is a quest into the influences of gas and active galactic nuclei (AGNs)
on the SFR, with particular focus on massive galaxies at z~2. First, a new code
if presented; SImulator of GAlaxy Millimeter/submillimeter Emission (S\'IGAME)
which can predict the atomic/molecular line emission in the far-infrared regime
from galaxies. By post-processing the outputs of cosmological simulations of
galaxy formation with sub-grid physics recipes, S\'IGAME divides the
interstellar medium (ISM) into different gas phases and derives density and
temperature structure, employing locally resolved radiation and pressure
fields. This method is used to predict the strengths of CO rotational
transitions as well as the [CII] emission line in normal star-forming galaxies
at z~2. A CO ladder close to that of our own Galaxy is found, but with CO-H2
conversion factors about 3 times smaller. For a set of 7 simulated galaxies at
z~2, the relation between [CII] luminosity and SFR displays a slope
significantly steeper than that found for observed galaxies at z<0.5. A
corresponding relation on kpc-scales is established for the first time
theoretically. Finally, a separate study uncovers the number fraction of AGNs
among massive galaxies at z~2, by analyzing CHANDRA CDF-S X-ray data. It is
found that about every fifth massive galaxy, quenched or not, contains an X-ray
luminous AGN. Interestingly, an even higher fraction of low-luminosity AGNs
emerges in the X-ray undetected galaxies when performing a stacking analysis,
and preferentially in the quenched ones, lending support to the importance of
AGNs in impeding star formation during galaxy evolution.
