  We investigate the solar phenomena associated with the origin of the solar
energetic particle (SEP) event observed on 2013 April 11 by a number of
spacecraft distributed in the inner heliosphere over a broad range of
heliolongitudes. We use Extreme UltraViolet (EUV) and white-light coronagraph
observations from the Solar Dynamics Observatory (SDO), the SOlar and
Heliospheric Observatory (SOHO) and the twin Solar TErrestrial RElations
Observatory spacecraft (STEREO-A and STEREO-B) to determine the angular extent
of the EUV wave and coronal mass ejection (CME) associated with the origin of
the SEP event. We compare the estimated release time of SEPs observed at each
spacecraft with the arrival time of the structures associated with the CME at
the footpoints of the field lines connecting each spacecraft with the Sun.
Whereas the arrival of the EUV wave and CME-driven shock at the footpoint of
STEREO-B is consistent, within uncertainties, with the release time of the
particles observed by this spacecraft, the EUV wave never reached the footpoint
of the field lines connecting near-Earth observers with the Sun, even though an
intense SEP event was observed there. We show that the west flank of the
CME-driven shock propagating at high altitudes above the solar surface was most
likely the source of the particles observed near Earth, but it did not leave
any EUV trace on the solar disk. We conclude that the angular extent of the EUV
wave on the solar surface did not agree with the longitudinal extent of the SEP
event in the heliosphere. Hence EUV waves cannot be used reliably as a proxy
for the solar phenomena that accelerates and injects energetic particles over
broad ranges of longitudes.
