Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3556
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dc.contributor.authorArellano Ferro, A-
dc.contributor.authorArévalo, M. J-
dc.contributor.authorLázaro, C-
dc.contributor.authorRey, M-
dc.contributor.authorBramich, D. M-
dc.contributor.authorGiridhar, S-
dc.date.accessioned2008-09-11T16:16:50Z-
dc.date.available2008-09-11T16:16:50Z-
dc.date.issued2004-10-
dc.identifier.citationRevista Mexicana de Astronomía y Astrofísica Vol. 40, No. 2, pp. 209 - 221en
dc.identifier.issn0185-1101-
dc.identifier.urihttp://hdl.handle.net/2248/3556-
dc.description.abstractWe report the results of CCD V and R photometry of the RRstars known in NGC4147. The periodicities of most variables are revised and new ephemerides are calculated. The Blazhko effect has been detected in V2 and V6. Three previously reported variables; V5, V9, and V15 are found to be non-variable. A new variable V18 was discovered with a period of 0.49205 days and an amplitude of 0.15. Using the approach of Fourier decomposition of the light curves, the physical parameters of the RRab and RRc variables were estimated. The cluster is of the Oosterhoff type. With the newly values [Fe/H]= -1.22+/-0.31 and 16.8+/-1.3, the cluster fits very well into the Oosterhoff type-metallicity and metallicity-temperature sequence found in globular clusters. A comparison with ZAHB models indicates that the RRab stars have not yet evolved off the horizontal branch, a result consistent with the mean period of the RRab variables and with the metallicity of the cluster derived in this work.en
dc.language.isoenen
dc.publisherInstituto de Astronomía, Universidad Nacional Autónoma de Méxicoen
dc.relation.urihttp://adsabs.harvard.edu/abs/2004RMxAA..40..209Aen
dc.relation.urihttp://www.astroscu.unam.mx/~rmaa/rmaa.htmlen
dc.subjectGlobular Clusters: NGC4147en
dc.subjectStars: Variables: RR Lyraeen
dc.titleCCD Photometry of the RR Lyrae Stars in NGC4147en
dc.typeArticleen
Appears in Collections:IIAP Publications

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