Mostrar el registro sencillo del ítem

dc.contributor.authorPiatti, Andres E.pt_BR
dc.contributor.authorClaria Olmedo, Juan Josept_BR
dc.contributor.authorBica, Eduardo Luiz Damianipt_BR
dc.contributor.authorGeisler, Dougpt_BR
dc.contributor.authorAhumada, Andrea Veronicapt_BR
dc.contributor.authorGirardi, Leo Albertopt_BR
dc.date.accessioned2014-04-13T01:49:53Zpt_BR
dc.date.issued2011pt_BR
dc.identifier.issn0035-8711pt_BR
dc.identifier.urihttp://hdl.handle.net/10183/93363pt_BR
dc.description.abstractWe present CCD photometry in the Washington system C, T1 and T2 passbands down to T1 ~ 23 in the fields of L3, L28,HW66, L100,HW79, IC 1708, L106, L108, L109, NGC643, L112, HW84, HW85 and HW86, 14 Small Magellanic Cloud (SMC) clusters, most of them poorly studied objects.We measured T1 magnitudes and C −T1 and T1 −T2 colours for a total of 213 516 stars spread throughout cluster areas of 14.7 × 14.7 arcmin2 each. We carried out an in-depth analysis of the field star contamination of the colour–magnitude diagrams (CMDs) and statistically cleaned the cluster CMDs. Based on the best fits of isochrones computed by the Padova group to the (T1, C − T1) CMDs, as well as from the δ(T1) index and the standard giant branch procedure, we derived ages and metallicities for the cluster sample. With the exception of IC1708, a relatively metal-poor Hyades-age cluster, the remaining 13 objects are between intermediate and old age (from 1.0 to 6.3 Gyr), their [Fe/H] values ranging from −1.4 to −0.7 dex. By combining these results with others available in the literature, we compiled a sample of 43 well-known SMC clusters older than 1 Gyr, with which we produced a revised age distribution. We found that the present clusters’ age distribution reveals two primary excesses of clusters at t ~ 2 and 5 Gyr, which engraves the SMC with clear signs of enhanced formation episodes at both ages. In addition, we found that from the birth of the SMC cluster system until approximately the first 4 Gyr of its lifetime, the cluster formation resembles that of a constant formation rate scenario.en
dc.format.mimetypeapplication/pdfpt_BR
dc.language.isoengpt_BR
dc.relation.ispartofMonthly notices of the royal astronomical society. Oxford. Vol. 417, no. 2 (Oct. 2011), p. 1559-1575pt_BR
dc.rightsOpen Accessen
dc.subjectPequena Nuvem de Magalhãespt_BR
dc.subjectTechniques: photometricen
dc.subjectGalaxies: individual: SMCen
dc.subjectAglomerados estelarespt_BR
dc.subjectFotometria astronômicapt_BR
dc.subjectMagellanic cloudsen
dc.subjectGalaxies: star clusters: general.en
dc.titleWashington photometry of 14 intermediate-age to old star clusters in the Small Magellanic Cloudpt_BR
dc.typeArtigo de periódicopt_BR
dc.identifier.nrb000826881pt_BR
dc.type.originEstrangeiropt_BR


Ficheros en el ítem

Thumbnail
   

Este ítem está licenciado en la Creative Commons License

Mostrar el registro sencillo del ítem