  The Vela supernova remnant complex is a region containing at least three
supernova remnants: Vela, Puppis A, and Vela Jr. With the launch of the
spectro-imaging X-ray telescope eROSITA on board the Spectrum Roentgen Gamma
(SRG) mission, it became possible to observe the one degree wide Vela Jr in its
entirety. Although several previous pointed Chandra and XMM-Newton observations
are available, it is only the second time after the ROSAT all-sky survey that
the whole remnant was observed in X-rays with homogeneous sensitivity. Vela Jr
is one of the few remnants emitting in the TeV band, making it an important
object in shock acceleration studies. However, the age and distance
determination using X-ray emission is largely hampered by the presence of the
Vela SNR along the same line. With the eROSITA data set our aim is to
characterize the emission of Vela Jr and distinguish it from Vela emission, and
also to characterize the spectral emission of the inner remnant. We processed
the eROSITA data dividing the whole remnant into seven different regions. In
addition, images of the whole remnant were employed to pinpoint the position of
the geometric center and constrain the proper motion of the CCO. We also
employed archival XMM-Newton pointed observations of the NW rim to determine
the cutoff energy of the electrons and the expansion velocity. We find the
magnetic field can vary between 2 $\mu$G and 16 $\mu$G in the NW rim. We also
find that the remnant spectrum is uniformly featureless in most regions, except
for two inner regions where an extra thermal model component improves the fit.
We obtain new coordinates for the geometric remnant center, resulting in a
separation of only 35.2 $\pm$ 15.8" from the position of the CCO. As a result,
we reinforce the association between the CCO and a proposed faint optical/IR
counterpart.
