  Ellerman Bombs are signatures of magnetic reconnection, which is an important
physical process in the solar atmosphere. How and where they occur is a subject
of debate. In this paper we analyse Sunrise/IMaX data together with 3D MHD
simulations that aim to reproduce the exact scenario proposed for the formation
of these features. Although the observed event seems to be more dynamic and
violent than the simulated one, simulations clearly confirm the basic scenario
for the production of EBs. The simulations also reveal the full complexity of
the underlying process. The simulated observations show that the Fe I 525.02 nm
line gives no information on the height where reconnection takes place. It can
only give clues about the heating in the aftermath of the reconnection. The
information on the magnetic field vector and velocity at this spatial
resolution is, however, extremely valuable because it shows what numerical
models miss and how they can be improved.
