Hostname: page-component-6b989bf9dc-jks4b Total loading time: 0 Render date: 2024-04-12T21:57:43.697Z Has data issue: false hasContentIssue false

Detection of extended Red Clump in the SMC cluster Kron 3

Published online by Cambridge University Press:  11 March 2020

P. K. Nayak
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore, 560034, India email: nayakphy@gmail.com Pondicherry University, R. Venkataraman Nagar, Kalapet, Pondicherry-605014, India
A. Subramaniam
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore, 560034, India email: nayakphy@gmail.com
S. Subramanian
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore, 560034, India email: nayakphy@gmail.com
S. Sahu
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore, 560034, India email: nayakphy@gmail.com Pondicherry University, R. Venkataraman Nagar, Kalapet, Pondicherry-605014, India
C. Mondal
Affiliation:
Indian Institute of Astrophysics, Koramangala, Bangalore, 560034, India email: nayakphy@gmail.com Pondicherry University, R. Venkataraman Nagar, Kalapet, Pondicherry-605014, India
Maria-Rosa L. Cioni
Affiliation:
Leibniz-Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany
C. Bell
Affiliation:
Leibniz-Institute for Astrophysics Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

For 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.

Type
Contributed Papers
Copyright
© International Astronomical Union 2020

References

Alcaino, G., Liller, W., Alvarado, F., et al. 1996, AJ, 112, 2004CrossRefGoogle Scholar
Bayo, A., Rodrigo, C., Barrado, YNavascués, D., et al. 2008, A&A, 492, 277Google Scholar
Bica, E., Bonatto, C., Dutra, C. M., & Santos, J. F. C. 2008, MNRAS, 389, 67810.1111/j.1365-2966.2008.13612.xCrossRefGoogle Scholar
Cioni, M.-R. L., Clementini, G., Girardi, L., et al. 2011, A&A, 527, A116Google Scholar
Danziger, I. J. 1973, ApJ, 181, 641CrossRefGoogle Scholar
Dias, B., Coelho, P., Barbuy, B., Kerber, L., & Idiart, T. 2010, A&A, 520, A85Google Scholar
Gascoigne, S. C. B. 1966, MNRAS, 134, 5910.1093/mnras/134.1.59CrossRefGoogle Scholar
Gascoigne, S. C. B. 1980, in IAU Symposium, Vol. 85, Star Clusters, ed. Hesser, J. E., 30531310.1007/978-94-009-9007-4_46CrossRefGoogle Scholar
Gascoigne, S. C. B. & Kron, G. E. 1952, PASP, 64, 196CrossRefGoogle Scholar
Glatt, K., Grebel, E. K., Sabbi, E., et al. 2008, AJ, 136, 1703CrossRefGoogle Scholar
Hodge, P. W. 1982, ApJ, 256, 447CrossRefGoogle Scholar
Mighell, K. J., Sarajedini, A., & French, R. S. 1998, AJ, 116, 239510.1086/300591CrossRefGoogle Scholar
Rich, R. M., Da Costa, G. S., & Mould, J. R. 1984, ApJ, 286, 517CrossRefGoogle Scholar
Shapley, H. & Wilson, H. H. 1925, Harvard College Observatory Circular, 276, 1Google Scholar
Vandenberg, D. A. & Bell, R. A. 1985, ApJS, 58, 561CrossRefGoogle Scholar