  In circumstellar disks around young stars, the gravitational influence of
nascent planets produces telltale patterns in density, temperature, and
kinematics. To better understand these signatures, we first performed 3D
hydrodynamical simulations of a 0.012 $M_{\odot}$ disk, with a Saturn-mass
planet orbiting circularly in-plane at 40 au. We tested four different disk
thermodynamic prescriptions (in increasing order of complexity, local
isothermality, $\beta$-cooling, two-temperature radiation hydrodynamics, and
three-temperature radiation hydrodynamics), finding that $\beta$-cooling offers
a reasonable approximation for the three-temperature approach when the planet
is not massive or luminous enough to substantially alter the background
temperature and density structure. Thereafter, using the three-temperature
scheme, we relaxed this assumption, simulating a range of different planet
masses (Neptune-mass, Saturn-mass, Jupiter-mass) and accretion luminosities (0,
$10^{-3} L_{\odot}$) in the same disk. Our investigation revealed that
signatures of disk-planet interaction strengthen with increasing planet mass,
with circumplanetary flows becoming prominent in the high-planet-mass regime.
Accretion luminosity, which adds pressure support around the planet, was found
to weaken the midplane Doppler-flip, potentially visible in optically thin
tracers like C$^{18}$O, while strengthening the spiral signature, particularly
in upper disk layers sensitive to thicker lines, like those of $^{12}$CO.
