  We investigate the possibility to distinguish the small-coupling,
slow-rotation black hole solution of Chern-Simons (CS) gravity from the Kerr
solution. We develop simulations of electromagnetic observables in the vicinity
of CS and Kerr black holes. We show that the typical relative observable
difference between CS and Kerr spacetimes is of the order of 0.1% thus beyond
reach of current or near-future instruments.
