Program: GS-2019B-DD-103

Optical Raman OVI scattering emission lines have only been found in symbiotic stars and can therefore unequivocally identify these accreting white dwarf-red giant binaries. Moreover, because Raman OVI features are produced by the scattering of the OVI 1032-1038 lines in the UV, they likely reveal when quasi-steady shell burning makes a symbiotic white dwarf (WD) very hot and luminous. We request 2.75 hours of GMOS-S DDT to observe simultaneously with XMM-Newton the recently discovered Raman emitter LMC 1 to confirm its shell burning, which will manifest as super-soft X-ray emission or strong UV emission without rapid flickering. Supporting the link between shell burning and Raman OVI emission will enable our RAMSES II team to use a narrow-band Raman filter on Gemini/GMOS to find new symbiotics and probe the origin of their shell burning. These time critical observations should be executed during the second half of the September 23-24 night.