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I report on the development of new code to support the Nasmyth and E-Wantenna mount types in AIPS which will allow polarisation analysis ofobservations made using these uncommon antenna configurations. These mounttypes may become more widely spread as they have several advantages,particularly for geodetic observatories. Multi-band observations, with multiplereceivers, can only be fitted into telescopes with Nasmyth feeds. These are therequirements for the new generation of geodetic arrays as discussed in IVS2010.Further more the next generation of antennae will also be required to have veryhigh slew rates, and these can be achieved with the E-W mount.  The mount type affects the differential phase between the left and the righthand circular polarisations (LHC and RHC) for different points on the sky. Thetarget antennae for the project was the Yebes 40m telescope, but as that wasstill under construction the data used as a demonstration was from the PicoVeleta antenna as part of the Global Millimeter VLBI Array (GMVA). For the E-Wmount type there are suitable data from the Australian LBA array. I demonstratethe effectiveness of the changes made and that the Nasmyth and E-W correctionscan be applied.

On the solution of the polarisation gain terms for VLBI data collected with antennas having Nasmyth or E-W mounts