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Revisiting the variable star population in NGC 6229 and the structure of the horizontal branch

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dc.contributor.author Arellano Ferro, A
dc.contributor.author Mancera Pina, P. E
dc.contributor.author Bramich, D. M
dc.contributor.author Giridhar, S
dc.contributor.author Ahumada, J. A
dc.contributor.author Kains, N
dc.contributor.author Kuppuswamy, K
dc.date.accessioned 2020-11-17T14:46:15Z
dc.date.available 2020-11-17T14:46:15Z
dc.date.issued 2015-09-01
dc.identifier.citation Monthly Notices of the Royal Astronomical Society, Vol. 452, No. 1, pp. 727-746 en_US
dc.identifier.issn 1365-2966
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7201
dc.description Restricted Access © Royal Astronomical Society http://dx.doi.org/10.1093/mnras/stv1299 en_US
dc.description.abstract We report an analysis of new V and I CCD time series photometry of the distant globular cluster NGC 6229. The principal aims were to explore the field of the cluster in search of new variables, and to Fourier decompose the RR Lyrae light curves in pursuit of physical parameters. We found 25 new variables: 10 RRab, 5 RRc, 6 SR, 1 CW, 1 SX Phe, and 2 that we were unable to classify. Secular period changes were detected and measured in some favourable cases. The classifications of some of the known variables were rectified. The Fourier decomposition of RRab and RRc light curves was used to independently estimate the mean cluster value of [Fe/H] and distance. From the RRab stars we found [Fe/H]UVES = −1.31 ± 0.01(statistical) ± 0.12(systematic) ([Fe/H]ZW = −1.42) and a distance of 30.0 ± 1.5 kpc, and from the RRc stars we found [Fe/H]UVES = −1.29 ± 0.12 and a distance of 30.7 ± 1.1 kpc, respectively. Absolute magnitudes, radii and masses are also reported for individual RR Lyrae stars. Also discussed are the independent estimates of the cluster distance from the tip of the red giant branch, 34.9 ± 2.4 kpc and from the period–luminosity relation of SX Phe stars, 28.9 ± 2.2 kpc. The distribution of RR Lyrae stars in the horizontal branch shows a clear empirical border between stable fundamental and first overtone pulsators which has been noted in several other clusters; we interpret it as the red edge of the first overtone instability strip. en_US
dc.language.iso en en_US
dc.publisher Oxford University Press on behalf of the Royal Astronomical Society en_US
dc.subject Stars: horizontal branch en_US
dc.subject Stars: variables: RR Lyrae en_US
dc.subject Globular clusters: individual: NGC 6229 en_US
dc.title Revisiting the variable star population in NGC 6229 and the structure of the horizontal branch en_US
dc.type Article en_US


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