RR Lyrae stars in M31 globular clusters: B514
link https://repositorio.uc.cl/handle/11534/81273account_box Contreras, R.account_box Federici, L.account_box Clementini, G.account_box Cacciari, C.account_box Merighi, R.account_box Kinemuchi, K.account_box Catelan , Marcioaccount_box Fusi Pecci, F.account_box Marconi, M.account_box Pritzl, B.account_box Smith, H.
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We present preliminary results of a variable star search in the metal-poor globular cluster B514 of the Andromeda galaxy (M31), based on Hubble Space Telescope Wide Field Planetary Camera 2 and Advanced Camera for Surveys observations. A large number of RR Lyrae stars have been identified for the first time in a globular cluster of M31. The average period of the RR Lyrae variables (< Pab > = 0.58 days and < Pc > = 0.35 days, for fundamental-mode and first-overtone pulsators, respectively) and the position in the period-amplitude diagram both suggest that B514 is likely an Oosterhoff I cluster, contrary to the general behaviour of the metal-poor globular clusters in the Milky Way, which show instead Oosterhoff type II pulsation properties....
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| Autor | Contreras, R. Federici, L. Clementini, G. Cacciari, C. Merighi, R. Kinemuchi, K. Catelan , Marcio Fusi Pecci, F. Marconi, M. Pritzl, B. Smith, H. |
| Título | RR Lyrae stars in M31 globular clusters: B514 |
| Fecha de publicación | 2008 |
| Resumen | We present preliminary results of a variable star search in the metal-poor globular cluster B514 of the Andromeda galaxy (M31), based on Hubble Space Telescope Wide Field Planetary Camera 2 and Advanced Camera for Surveys observations. A large number of RR Lyrae stars have been identified for the first time in a globular cluster of M31. The average period of the RR Lyrae variables (< Pab > = 0.58 days and < Pc > = 0.35 days, for fundamental-mode and first-overtone pulsators, respectively) and the position in the period-amplitude diagram both suggest that B514 is likely an Oosterhoff I cluster, contrary to the general behaviour of the metal-poor globular clusters in the Milky Way, which show instead Oosterhoff type II pulsation properties.... |
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