  Aim: We observed the center of the supernova remnant Vela Jr in radio
continuum in order to search for a counterpart to the compact central X-ray
source CXOU J085201.4-461753, possibly a neutron star candidate which could be
the remnant of the supernova explosion. Method: Observations were made with the
Australia Telescope Compact Array at 13 and 20 cm. Spectral indices were
obtained using flux density correlations of the data which were spatially
filtered to have the same u-v coverage. A multiwavelength search for
counterparts to the compact central X-ray source was made. Results: We compiled
a new catalogue of 31 small diameter radio sources, including the previously
known source PMN J0853-4620, listing the integrated flux densities at 20 cm
and, for half of the sources, the flux densities at 13 cm with the
corresponding spectral indices. All sources are unresolved at the present
angular resolution except for Source 18, which is clearly elongated and lies
strikingly close to CXOU J085201.4-461753. Our observations show no evidence
for the existence of a pulsar wind driven nebula associated with the point
X-ray source. Furthermore, Source 18 has a thermal spectrum with index +0.8 +/-
0.4, and appears to be the counterpart of the optical source Wray 16-30. In
spite of the absence of OIII emission lines as reported in the literature, we
find that this object could be explained as a low emission planetary nebula
belonging to the ``butterfly'' morphological class. Conclusions: We conclude
that if the radio source 18 is actually a planetary nebula, then CXOU
J085201.4-461753 is more likely to be related to it rather than to Vela Jr.
