  Observations of the nearby universe reveal an increasing fraction of active
galactic nuclei (AGN) with decreasing projected separation for close galaxy
pairs, relative to control galaxies. This implies galaxy interactions play a
role in enhancing AGN activity. However, the picture at higher redshift is less
established, partly due to limited spectroscopic redshifts. We combine
spectroscopic surveys with photometric redshift probability distribution
functions for galaxies in the CANDELS and COSMOS surveys, to produce the
largest ever sample of galaxy pairs used in an AGN fraction calculation for
cosmic noon ($0.5<z<3$). We present a new technique for assessing galaxy pair
probability (based on line-of-sight velocities +/-1000 km/s) from photometric
redshift posterior convolutions and use these to produce weighted AGN
fractions. Over projected separations 5-100kpc we find no evidence for
enhancement, relative to isolated control galaxies, of X-ray (L_X > 10^42
erg/s) or infrared-selected AGN in major (mass ratios up to 4:1) or minor (4:1
to 10:1) galaxy pairs. However, defining the most obscured AGN as those
detected in the infrared but not in X-rays, we observe a trend of increasing
obscured AGN enhancement at decreasing separations. The peak enhancement,
relative to isolated controls, is a factor of 2.08+/-0.61 for separations
<25kpc. Our simulations with mock data, indicates this could be a lower limit
of the true enhancement. If confirmed with improved infrared imaging (e.g.,
with JWST) and redshifts (e.g., with forthcoming multi-object spectrograph
surveys), this would suggest that galaxy interactions play a role in enhancing
the most obscured black hole growth at cosmic noon.
