J/ApJ/970/113ivo://CDS.VizieR/J/ApJ/970/113doi:10.26093/cds/vizier.19700113CDSNavarete F.Ticiani Dos Santos P.Carciofi A.C.Figueiredo A.L.2024-11-06T20:28:01Z2024-08-30T15:21:54ZCDS support team

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

cds-question@unistra.frmagellanic-cloudsopen-star-clustersbe-starsinfrared-photometryvisible-astronomybroad-band-photometryh-alpha-photometryH{alpha} emission is a clear indicator of circumstellar activity in Be stars, historically employed to assess the classical Be star (CBe) population in young open clusters (YOCs). The YOC NGC 330 in the Small Magellanic Cloud exhibits a large known fraction of CBe stars and was selected for a pilot study to establish a comprehensive methodology for identifying H{alpha} emitters in the Magellanic Clouds, encompassing the entire B-type spectral range. Using the SOAR Adaptive Module Imager (SAMI), we investigated the stellar population of NGC 330 using multiband BVRI+H{alpha} imaging. We identified H{alpha} emitters within the entire V-band range covered by SAMI/SOAR observations (V<~22), comprising the complete B-type stellar population and offering a unique opportunity to explore the Be phenomenon across all spectral subclasses. The stellar radial distribution shows a clear bimodal pattern between the most massive (B5 or earlier) and the lower mass main-sequence objects (later than B6) within the cluster. The former is concentrated toward the cluster center (showing a dispersion {sigma}=4.26+/-0.20pc), whereas the latter extends across larger radii ({sigma}=10.83+/-0.65pc), indicating mass stratification within NGC 330. The total fraction of emitters is 4.4%+/-0.5%, notably smaller than previous estimates from flux- or seeing- limited observations. However, a higher fraction of H{alpha} emitters is observed among higher mass stars (32.8%+/-3.4%) than within lower mass (4.4%+/-0.9%). Consequently, the putative CBe population exhibits distinct dynamical characteristics compared to the bulk of the stellar population in NGC 330. These findings highlight the significance of the current observations in providing a complete picture of the CBe population in NGC 330.2024ApJ...970..113Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/970/113CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/472/577 : NGC 330 Be stars and binaries (Martayan+, 2007)J/A+A/634/A51 : NGC 330 seen by MUSE. I (Bodensteiner+, 2020)J/A+A/652/A70 : NGC 330 seen by MUSE. II (Bodensteiner+, 2021)J/A+A/680/A32 : NGC 330 seen by MUSE. III (Bodensteiner+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/970/113https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/970/113http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/970/113https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/970/113https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/970/113http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/970/113GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJ/970/113/table3 (Calibrated BVRI+Halpha SAMI Photometry for NGC330)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJ/970/113/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJ/970/113/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJ/970/113/table3?GETtext/xml+votable180.050000true14.07056789-72.463073730.0055555555555555566/333172.367228618189496e-19 5.042107639525881e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJ/970/113?format=asciiOpticalInfrareddefaultJ/ApJ/970/113/table3Calibrated BVRI+Halpha SAMI Photometry for NGC330recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeqNumber the object in the SAMI catalogmeta.id;meta.mainintRAJ2000Right Ascension J2000 (degrees)degpos.eq.ra;meta.mainindexedDEJ2000Declination J2000 (degrees)degpos.eq.dec;meta.mainindexedNfiltNumber of filtersmeta.numberintBmag? Apparent magnitude in Kron-Cousins B filtermagphot.mag;em.opt.Bfloatnullablee_Bmag? Error on apparent magnitude in B filtermagstat.error;phot.magfloatnullableVmag? Apparent magnitude in Kron-Cousins V filtermagphot.mag;em.opt.Vfloatnullablee_Vmag? Error on apparent magnitude in V filtermagstat.error;phot.magfloatnullableRmag? Apparent magnitude in Kron-Cousins R filtermagphot.mag;em.opt.Rfloatnullablee_Rmag? Error on apparent magnitude in R filtermagstat.error;phot.magfloatnullableImag? Apparent magnitude in Kron-Cousins I filtermagphot.mag;em.opt.Ifloatnullablee_Imag? Error on apparent magnitude in I filtermagstat.error;phot.magfloatnullableHamag? Apparent magnitude in H-alpha filtermagphot.flux;em.line.Halphafloatnullablee_Hamag? Error on apparent magnitude in H-alpha filtermagstat.error;phot.magfloatnullableE(B-V)? Total color excessmagphot.color.excessfloatnullableTeff? Effective temperatureKphys.temperature.effectiveintnullablelogg? Stellar surface gravitylog(cm.s**-2)phys.gravityfloatnullable[Fe/H]? Stellar metallicityphys.abund.Zfloatnullablealpha? Stellar alpha exponentphot.color;em.opt.V;em.line.Halphafloatnullablesigma-mu? Internal mean photometric offset errormagstat.errorfloatnullableTypePhotometric classification of the source (1)src.classchar