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RZ2109 is the first of several extragalactic globular clusters shown to hostan ultraluminous X-ray source. RZ2109 is particularly notable because opticalspectroscopy shows it has broad, luminous [OIII] 4959,5007 emission, while alsohaving no detectable hydrogen emission. The X-ray and optical characteristicsof the source in RZ2109 make it a good candidate for being a stellar mass blackhole accreting from a white dwarf donor (i.e. an ultracompact black hole X-raybinary). In this paper we present optical spectroscopic monitoring of the[OIII]5007 emission line from 2007 to 2018. We find that the flux of theemission line is significantly lower in recent observations from 2016-2018 thanit was in earlier observations in 2007-2011. We also explore the behaviour ofthe emission line shape over time. Both the core and the wings of the emissionline decline over time, with some evidence that the core declines more rapidlythan the wings. However, the most recent observations (in 2019) unexpectedlyshow the emission line core re-brightening.

Slow Decline and Rise of the Broad [OIII] Emission Line in Globular Cluster Black Hole Candidate RZ2109