UV provides a unique tool to identify and characterise hot subluminous compact stars (such as white dwarfs and subdwarfs). We used multi-wavelength spectral energy distributions to identify these cooler+hotter component systems. 

Many of the cooler components were blue stragglers (BSS) and main sequence (MS) stars. Importantly, many of the hot components are extremely low mass WD candidates (which are a result of mass transfer). This also resulted in the classification of the MS stars as blue lurkers (which are post-mass-transfer accreters on the main sequence).

Spectroscopic and time-domain follow-ups are ongoing.

Open clusters, celestial families of stars born together and bound by gravity, have perpetually intrigued astronomers with their enigmatic internal dynamics. Illuminating these cosmic enigmas, a pioneering study harnessing the latest data from the European Space Agency's (ESA) Gaia Data Release 3 (DR3) has unveiled a plethora of extraordinary discoveries regarding the behaviour of these stellar assemblages.

The study unveiled that the spin frequencies observed in certain clusters surpassed expectations predicated on simulated, initially non-rotating clusters. This implies that a noteworthy portion of clusters may be born rotating or have undergone substantial interactions throughout their lifespans (Jadhav et al. 2024).