J/MNRAS/472/808ivo://CDS.VizieR/J/MNRAS/472/808doi:10.26093/cds/vizier.74720808CDSRipepi V.Cioni M.-R.L.Moretti M.I.Marconi M.Bekki K.,Clementini G.De Grijs R.Emerson J.Groenewegen M.A.T.Ivanov V.D.,Molinaro R.Muraveva T.Oliveira J.M.Piatti A.E.Subramanian S.,Van Loon J.T.2024-08-17T20:21:14Z2020-08-11T10:32:42ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frvariable-starsinfrared-photometryThe VISTA near-infrared YJKs survey of the Magellanic System (VMC) is collecting deep Ks-band time-series photometry of pulsating stars hosted by the two Magellanic Clouds and their connecting bridge. Here, we present Y, J, Ks light curves for a sample of 717 Small Magellanic Cloud (SMC) Classical Cepheids (CCs). These data, complemented with our previous results and V magnitude from literature, allowed us to construct a variety of period-luminosity and period-Wesenheit relationships, valid for Fundamental, First and Second Overtone pulsators. These relations provide accurate individual distances to CCs in the SMC over an area of more than 40 deg^2^. Adopting literature relations, we estimated ages and metallicities for the majority of the investigated pulsators, finding that (i) the age distribution is bimodal, with two peaks at 120+/-10 and 220+/-10Myr; (i) the more metal-rich CCs appear to be located closer to the centre of the galaxy. Our results show that the three-dimensional distribution of the CCs in the SMC is not planar but heavily elongated for more than 25-30kpc approximately in the east/north-east towards south-west direction. The young and old CCs in the SMC show a different geometric distribution. Our data support the current theoretical scenario predicting a close encounter or a direct collision between the Clouds some 200Myr ago and confirm the presence of a Counter-Bridge predicted by some models. The high-precision three-dimensional distribution of young stars presented in this paper provides a new test bed for future models exploring the formation and evolution of the Magellanic System.2017MNRAS.472..808Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/472/808CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/AcA/65/297 : OGLE4 LMC and SMC Cepheids (Soszynski+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/472/808https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/472/808http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/472/808https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/472/808https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/472/808http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/472/808GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapInfrareddefaultJ/MNRAS/472/808/table2Photometric results for all the 4793 classical Cepheids analysed in this paperrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLCindicates light curvesmeta.ref.urlcharNameOGLE name, OGLE-SMC-CEP-NNNN, from Soszynski et al., 2010, Cat J/AcA/60/17meta.id;meta.maincharprimaryModeMode(s) of pulsation (1)meta.code;src.varcharVMCTileVMC tile, SMC_N_N, in which the object is foundobs.fieldcharPerPerioddtime.perioddoubleNYNumber of epochs in Ymeta.numberint<Ymag>Intensity-averaged Y magnitudemagphot.mag;em.IR.Jfloate_<Ymag>rms uncertainty in <Ymag>magstat.error;phot.magfloatA(Y)Peak-to-peak amplitude in Ymagsrc.var.amplitude;em.opt.Bfloate_A(Y)rms uncertainty on A(Y)magstat.errorfloatNJNumber of epochs in Jmeta.numberint<Jmag>Intensity-averaged J magnitudemagphot.mag;em.IR.Jfloate_<Jmag>rms uncertainty in <Jmag>magstat.error;phot.magfloatA(J)Peak-to-peak amplitude in Jmagsrc.var.amplitude;em.IR.Jfloate_A(J)rms uncertainty on A(J)magstat.errorfloatNKsNumber of epochs in Ksmeta.numberint<Ksmag>Intensity-averaged Ks magnitudemagphot.mag;em.IR.Kfloate_<Ksmag>rms uncertainty in <Ksmag>magstat.error;phot.magfloatA(Ks)Peak-to-peak amplitude in Ksmagsrc.var.amplitudefloate_A(Ks)rms uncertainty on A(Ks)magstat.errorfloatE(V-I)Adoped E(V-I) value in this workmagphot.color.excessfloatJ/MNRAS/472/808/listlcList of Cepheids with light curvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameOGLE name, OGLE-SMC-CEP-NNNN, from Soszynski et al., 2010, Cat J/AcA/60/17meta.id;meta.maincharLCShow the light curvesmeta.ref.urlchar