dc.creator | Navarrete, C. | |
dc.creator | Catelan, M. | |
dc.creator | Contreras Ramos, R. | |
dc.creator | Alonso-García, J. | |
dc.creator | Gran, F. | |
dc.creator | Dékány, I. | |
dc.creator | Minniti, D. | |
dc.date.accessioned | 2022-07-07T17:29:16Z | |
dc.date.accessioned | 2024-05-02T14:50:27Z | |
dc.date.available | 2022-07-07T17:29:16Z | |
dc.date.available | 2024-05-02T14:50:27Z | |
dc.date.created | 2022-07-07T17:29:16Z | |
dc.date.issued | 2017-08 | |
dc.identifier | Astronomy and Astrophysics Volume 6041 August 2017 Article number A120 | |
dc.identifier | 0004-6361 | |
dc.identifier | https://repositorio.unab.cl/xmlui/handle/ria/23209 | |
dc.identifier | 10.1051/0004-6361/201630102 | |
dc.identifier.uri | https://repositorioslatinoamericanos.uchile.cl/handle/2250/9259206 | |
dc.description.abstract | Aims. The globular cluster ω Centauri (NGC 5139) hosts hundreds of pulsating variable stars of different types, thus representing a treasure trove for studies of their corresponding period-luminosity (PL) relations. Our goal in this study is to obtain the PL relations for RR Lyrae and SX Phoenicis stars in the field of the cluster, based on high-quality, well-sampled light curves in the near-infrared (IR). Methods. Observations were carried out using the VISTA InfraRed CAMera (VIRCAM) mounted on the Visible and Infrared Survey Telescope for Astronomy (VISTA). A total of 42 epochs in J and 100 epochs in KS were obtained, spanning 352 days. Point-spread function photometry was performed using DoPhot and DAOPHOT crowded-field photometry packages in the outer and inner regions of the cluster, respectively. Results. Based on the comprehensive catalog of near-IR light curves thus secured, PL relations were obtained for the different types of pulsators in the cluster, both in the J and KS bands. This includes the first PL relations in the near-IR for fundamental-mode SX Phoenicis stars. The near-IR magnitudes and periods of Type II Cepheids and RR Lyrae stars were used to derive an updated true distance modulus to the cluster, with a resulting value of (m-M)0 = 13.708 ± 0.035 ± 0.10 mag, where the error bars correspond to the adopted statistical and systematic errors, respectively. Adding the errors in quadrature, this is equivalent to a heliocentric distance of 5.52 ± 0.27 kpc. © 2017 ESO. | |
dc.language | en | |
dc.publisher | Astronomy and Astrophysics | |
dc.subject | Globular clusters: individual: NGC 5139 | |
dc.subject | Infrared: stars | |
dc.subject | Stars: variables: Cepheids | |
dc.subject | Stars: variables: delta Scuti | |
dc.subject | Stars: variables: RR Lyrae | |
dc.subject | Surveys | |
dc.title | Near-IR period-luminosity relations for pulsating stars in ω Centauri (NGC 5139) | |
dc.type | Artículo | |