  As part of our KMOS AGN Survey at High-redshift (KASHz), we present
spatially-resolved VLT/KMOS and VLT/SINFONI spectroscopic data and ALMA
870$\mu$m continuum imaging of eight $z$=1.4--2.6 moderate AGN ($L_{\rm 2-10
\rm kev}$ = $10^{42} - 10^{45}$ ergs s$^{-1}$). We map [OIII], H$\alpha$ and
rest-frame FIR emission to search for any spatial anti-correlation between
ionised outflows (traced by the [OIII] line) and star formation (SF; traced by
H$\alpha$ and FIR), that has previously been claimed for some high-z AGN and
used as evidence for negative and/or positive AGN feedback. Firstly, we
conclude that H$\alpha$ is unreliable to map SF inside our AGN host galaxies
based on: (i) SF rates inferred from attenuation-corrected H$\alpha$ can lie
below those inferred from FIR; (ii) the FIR continuum is more compact than the
H$\alpha$ emission by a factor of $\sim 2$ on average; (iii) in half of our
sample, we observe significant spatial offsets between the FIR and H$\alpha$
emission, with an average offset of $1.4\pm0.6$ kpc. Secondly, for the five
targets with outflows we find no evidence for a spatial anti-correlation
between outflows and SF using either H$\alpha$ or FIR as a tracer. This holds
for our re-analysis of a famous $z$=1.6 X-ray AGN (`XID 2028') where positive
and negative feedback has been previously claimed. Based on our results, any
impact on SF by ionised outflows must be subtle, either occurring on scales
below our resolution, or on long timescales.
