We present a detailed analysis of a large sample of 31 low-redshift , mostly radio-quiet type 1 quasi-stellar objects ( QSOs ) observed with integral field spectroscopy to study their extended emission-line regions ( EELRs ) .
We focus on the ionisation state of the gas , size and luminosity of extended narrow line regions ( ENLRs ) , which corresponds to those parts of the EELR dominated by ionisation from the QSO , as well as the kinematics of the ionised gas .
We detect EELRs around 19 of our 31 QSOs ( 61 % ) after deblending the unresolved QSO emission and the extended host galaxy light in the integral field data with a new dedicated algorithm .
Based on standard emission-line diagnostics we identify 13 EELRs to be entirely ionised by the QSO radiation , 3 EELRs are composed of H ii regions and 3 EELRs display signatures of both ionisation mechanisms at different locations .
The typical size of the ENLR is \sim 10 kpc at a median nuclear [ O iii ] luminosity of \log ( L ( [ { O \textsc { iii } } ] ) / [ \mathrm { erg } \mathrm { s } ^ { -1 } ] ) = 42.7 \pm 0.15 .
We show that the ENLR sizes are least a factor of \sim 2 larger than determined with the Hubble Space Telescope , but are consistent with those of recently reported type 2 QSOs at matching [ O iii ] luminosities .
The ENLR of type 1 and type 2 QSOs therefore appear to follow the same size-luminosity relation .
Furthermore , we show for the first time that the ENLR size is much better correlated with the QSO continuum luminosity than with the total/nuclear [ O iii ] luminosity .
We show that ENLR luminosity and radio luminosity are correlated , and argue that radio jets even in radio-quiet QSOs are important for shaping the properties of the ENLR .
Strikingly , the kinematics of the ionised gas is quiescent and likely gravitationally driven in the majority of cases and we find only 3 objects with radial gas velocities exceeding > 400 \mathrm { km } \mathrm { s } ^ { -1 } in specific regions of the EELR that can be associate with radio jets .
In general , these are significantly lower outflow velocities and detection rates compared to starburst galaxies or radio-loud QSOs .
This represent a challenge for some theoretical feedback models in which luminous QSOs are expected to radiatively drive an outflow out to scales of the entire host galaxy .