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We have demonstrated the advantage of combining multi-wavelengthobservations, from the ultraviolet (UV) to near-infrared, to study Kron 3, amassive star cluster in the Small Magellanic Cloud. We have estimated theradius of the cluster Kron 3 to be 2.'0 and for the first time, we report theidentification of NUV-bright red clump (RC) stars and the extension of the RCincolour and magnitude in the NUV vs (NUV-optical) colour-magnitude diagram(CMD). We found that extension of the RC is an intrinsic property of thecluster and it is not due to contamination of field stars or differentialreddening across the field. We studied the spectral energy distribution of theRC stars and estimated a small range in temperature ~5000 - 5500K, luminosity~60 - 90 Land radius ~8.0 - 11.0 Supporting their RC nature. The range of UVmagnitudes amongst the RC stars (~23.3 to 24.8 mag) is likely caused by thecombined effect of variable mass loss, variation in initial helium abundance(Y_ini=0.23 to 0.28), and a small variation in age (6.5-7.5 Gyr) andmetallicity ([Fe/H]=-1.5 to -1.3). Spectroscopic follow-up observations of RCstars in Kron 3 are necessary to confirm the cause of the extended RC.

UVIT-HST-Gaia-VISTA study of KRON 3 in the Small Magellanic Cloud: A cluster with an extended red clump in UV