Except PKS 1830-211, all sources detected in our observations are
extended. Both their morphologies and spectral indices suggest that sources
, 
, and 
are previously
unnoticed SNRs. Sources 
and could be remnants
with particularly flat spectra as well. The most intense of these galactic
sources is , with an integrated flux density of 17.7 Jy at
1.42 GHz. None known radio pulsar is associated with this object. The
surface brightness is 
W
m-2 Hz-1 sr-1, and its distance, according to a 
relationship (Milne 1979), would be roughly of 
2.5 kpc.
This implies a radius of 32.5 pc. In a standard ISM (
cm-3) and assuming a Sedov phase for the expanding shell, the age of
the SNR would be 
yr.
In Fig. 2 (click here) we have superimposed to the filtered radio map the
confidence contours of the likelihood test statistics of 2EG 
provided by Thompson et al. (1996). It is clear
that the only source within the 95% confidence contour (which is ussually
considered as representative of the EGRET statistical point source
uncertainties) is PKS 1830-211. The angular separation between the
location of the highest likelihood test statistic for 2EG
and the position of the AGN is just 
arcminutes. The remaining
radio sources are too far from the EGRET source position to significantly
contribute to the 
-ray emission. The nearest source is , and one might speculate that the pulsar produced in the
supernova event that originated the remnant could be a Geminga-like object
with a high proper velocity that would have driven it to the position of
the EGRET detections. This seems unlikely. In fact, the angular distance
from the flux peak of to the EGRET highest confidence
contour is 
, which corresponds to a distance of 
pc. The proper motion of the pulsar then should exceed 1300 km s-1,
which seems unrealistic. Moreover, the pulsar hypothesis is not supported
by the observed -spectrum of 2EG (Merck
et al. 1996). This spectrum can be properly fitted by a power-law
given by 
cm-2 s-1 MeV-1, which is considerably steeper than observed
in -ray pulsars (indices typically 
, see Fierro
et al. 1993). The possible presence of -ray variability in
the time history of 2EG (see below) also suggest to rule
out a pulsar origin of the emission.
It is also worhty to remark that the Bayes's theorem has been used by
Mattox et al. (1997) to computed a posteriori probability that
PKS 1830-211 is the correct identification of 2EG . The
resulting probability is 0.98, with an a priori probability of 
.
In this computation radio sources from the Parkes-MIT-NRAO survey
(Griffith & Wright 1993) were used. If we take into account
that there are just 183 strong flat-spectrum radio sources at
the possibility of a chance association results negligible.