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Extremely high velocity emission likely related to jets is known to occur insome proto-Planetary Nebulae. However, the molecular complexity of thiskinematic component is largely unknown. We observed the known extreme outflowfrom the proto-Planetary Nebula IRAS 16342-3814, a prototype water fountain, inthe full frequency range from 73 to 111 GHz with the RSR receiver on the LargeMillimetre Telescope. We detected the molecules SiO, HCN, SO, and $^{13}$CO.All molecular transitions, with the exception of the latter are detected forthe first time in this source, and all present emission with velocities up to afew hundred km s$^{-1}$. IRAS 16342-3814 is therefore the only source of thiskind presenting extreme outflow activity simultaneously in all these molecules,with SO and SiO emission showing the highest velocities found of these speciesin proto-Planetary Nebulae. To be confirmed is a tentative weak SO componentwith a FWHM $\sim$ 700 km s$^{-1}$. The extreme outflow gas consists of densegas (n$_{\rm H_2} >$ 10$^{4.8}$--10$^{5.7}$ cm$^{-3}$), with a mass larger than$\sim$ 0.02--0.15 M$_{\odot}$. The relatively high abundances of SiO and SO maybe an indication of an oxygen-rich extreme high velocity gas.

Early Science with the Large Millimetre Telescope: Molecules in the Extreme Outflow of a proto-Planetary Nebula