  In this work, we analyze the observational properties of static, spherically
symmetric boson stars with fourth and sixth-order self-interactions, using the
Julia-based general-relativistic radiative transfer code Skylight. We assume
the boson stars are surrounded by an optically thick, geometrically thin
accretion disk. We use the Novikov-Thorne model to compute the energy flux,
introducing a physically based accretion model around these boson star
configurations. Additionally, we calculate the relativistic broadening of
emission lines, incorporating a lamppost corona model with full relativistic
effects for the first time around a boson star. Our results show distinct
observational features between quartic-potential boson stars and Schwarzschild
black holes, owing to the presence of stable circular orbits at all radii
around the former. On the other hand, compact solitonic boson stars, which
possess an innermost stable circular orbit, have observational features closely
similar to black holes. This similarity emphasizes their potential as
black-hole mimickers. However, the compact boson stars, lacking an event
horizon, have complex light-ring structures that produce potentially observable
differences from black holes with future generations of experiments.
