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The aim of this paper is to test the basic model of negative AGN feedback.According to this model, once the central black hole accretes at the Eddingtonlimit and reaches a certain critical mass, AGN driven outflows blow out gas,suppressing star formation in the host galaxy and self-regulating black holegrowth. We consider a sample of 224 quasars selected from the SDSS at z<1observed in the infrared band by Herschel. We evaluate the star formation ratein relation to several outflow signatures traced by the [OIII]4959,5007 and[OII]3726,3729 emission lines in about half of the sample with high qualityspectra. Most of the quasars show asymmetric and broad wings in [OIII], whichwe interpret as outflow signatures. We separate the quasars in two groups,``weakly'' and ``strongly'' outflowing, using three different criteria. When wecompare the mean star formation rate in five redshift bins in the two groups,we find that the SFRs are comparable or slightly larger in the stronglyoutflowing quasars. We estimate the stellar mass from SED fitting and thequasars are distributed along the star formation main sequence, although with alarge scatter. The scatter from this relation is uncorrelated with respect tothe kinematic properties of the outflow. Moreover, for quasars dominated in theinfrared by starburst or by AGN emission, we do not find any correlationbetween the star formation rate and the velocity of the outflow, a trendpreviously reported in the literature for pure starburst galaxies. We concludethat the basic AGN negative feedback scenario seems not to agree with ourresults. Although we use a large sample of quasars, we did not find anyevidence that the star formation rate is suppressed in the presence of AGNdriven outflows on large scale. A possibility is that feedback is effectiveover much longer timescales than those of single episodes of quasar activity.

Is there any evidence that ionised outflows quench star formation in type 1 quasars at z<1?