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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7497
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dc.contributor.authorNayak, P. K-
dc.contributor.authorSubramaniam, A-
dc.contributor.authorSubramanian, S-
dc.contributor.authorSahu, S-
dc.contributor.authorMondal, C-
dc.contributor.authorCioni, Maria-Rosa L-
dc.contributor.authorBell, C-
dc.date.accessioned2020-11-27T12:52:39Z-
dc.date.available2020-11-27T12:52:39Z-
dc.date.issued2019-05-
dc.identifier.citationProceedings of the International Astronomical Union, Vol. 351, pp. 135-138en_US
dc.identifier.issn1743-9213-
dc.identifier.urihttp://prints.iiap.res.in/handle/2248/7497-
dc.descriptionRestricted Access © International Astronomical Union https://doi.org/10.1017/S1743921319007002en_US
dc.description.abstractFor the first time, we report the identification of NUV bright red clump (RC) stars and the extension of RC stars over two magnitudes both in color and magnitude axis in NUV vs (NUV – optical) color magnitude diagram. We find that the extension of RC is not due to photometric uncertainties. We suggest that the extension could be an effect of field star contamination. We also suggest that if it is an intrinsic property of the cluster then age and/or metallicity spread within the cluster could be the possible reasons for extended RC.en_US
dc.language.isoenen_US
dc.publisherCambridge University Pressen_US
dc.relation.ispartofseriesIAU Symposium No. 351;-
dc.subjectgalaxies:Magellanic Cloudsen_US
dc.subjectgalaxies: star clustersen_US
dc.subjectstars:ultravioleten_US
dc.titleDetection of extended Red Clump in the SMC cluster Kron 3en_US
dc.typeArticleen_US
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