  Flux calibrated images of the known supernova remnant G 34.7-0.4 in basic
optical emission lines are presented. The low ionization images show a
relatively flat flux distribution. The diffuse and patchy morphology of the
detected optical emission may indicate the presence of turbulent magnetic
fields. Typical observed Halpha+[N II] fluxes are ~8 x 10^{-17} erg s^{-1}
cm^{-2} arcsec^{-2}, while the [S II] fluxes are lower around 4 x 10^{-17} erg
s^{-1} cm^{-2} arcsec^{-2}. Emission in the medium ionization line of [O III]
5007 A is not detected within our sensitivity limits, probably due to the heavy
extinction towards the remnant. The long-slit spectra reveal strong [S II] and
[N II] emission relative to Halpha and moderate [O I] 6300 A emission. Shock
velocities in the range of 110-150 km/s and low electron densities are
estimated. Archival MSX infrared data show emission in the south and west areas
of the remnant matching rather well the optical and radio emission.
