We analyse by detailed modelling the spectra observed from the sample galaxies at z \sim 0.8 presented by Ly et al ( 2015 ) , constraining the models by the [ OIII ] 5007+4959/ [ OIII ] 4363 line ratios .
Composite models ( shock + photoionization ) are adopted .
Shock velocities \geq 100 km s ^ { -1 } and preshock densities n _ { 0 } \sim 200 cm ^ { -3 } characterize the gas surrounding the starburst ( SB ) , while n _ { 0 } are higher by a factor of 1.5-10 in the AGN emitting gas .
SB effective temperatures are similar to those of quiescent galaxies ( T _ { * } \sim 4-7 10 ^ { 4 } K ) .
Cloud geometrical thickness in the SB are \leq 10 ^ { 16 } cm indicating major fragmentation , while in AGN they reach > 10 pc .
O/H are about solar for all the objects , except for a few AGN clouds with O/H= 0.3 -0.5 solar .
Starburst models reproduce most of the data within the observational errors .
About half of the object spectra are well fitted by an accreting AGN .
Some galaxies show multiple radiation sources , such as SB+AGN , or a double AGN .