Schematic of the IPS interface with the telescope. The array of seven lenslets couples the light from the telescope’s Cassegrain focal plane into MMFs. For these on-sky results, only one lenslet, and hence one MMF, was used. The light was transported to a photonic lantern, which converts the multimoded light to a series of single modes in multiple SMFs, which were then simultaneously interfaced to the AWG chip. The AWG chip outputs the spectrally dispersed signal from all 12 input SMFs on its output face, which was re-imaged onto the slit. The IRIS 2 imaging spectrograph was used as a cross-disperser, separating the spectra from the multiple input fibres along with the different grating orders.