Abstract: Cosmological simulations predict that AGN feedback is responsible for suppressing the growth of massive galaxies and is believed to be a key process in reproducing basic properties of galaxies (such as luminosity function, the black hole–spheroid relationships, galaxy sizes, galaxy colour bi-modality). There have been a number studies (Cano Diaz et al 2012, Cresci et al 2015, Carniani et al 2016 ) that have suggested an anti-correlation between ionised outflows (traced with [O III] in IFU data) and star formation (traced using H-alpha in IFU data) in the host galaxies of high-luminosity AGN. However, the H-alpha line as a tracer of star formation is susceptible to obscuration by dust, therefore this anti-correlation between star formation and outflows might be caused by dust obscuration, rather than star-formation suppression. We have utilised the largest sample of AGN observed with IFU at high redshift (the KASHz survey) to select AGN with high-quality IFU data, to map both the H-alpha and [OIII] kinematics, and that also have ancillary ALMA (870 micron) data, to map the dust. Using this unique sample of AGN, with a range of luminosities, as well as a new ALMA data for the quasars mentioned above, I will re-investigate the evidence for rapid suppression of star formation by AGN outflows and answer the question: Do powerful AGN really rapidly suppress star formation?

Bio: have finished my PhD at Durham in 2019 and I started a postdoc in Sweden at Chalmers University with prof. Kirsten Knudsen. In September 2021 I have moved to KICC at Cambridge to join prof. Roberto Maiolino’s group.