J/MNRAS/510/32ivo://CDS.VizieR/J/MNRAS/510/32doi:10.26093/cds/vizier.75100032CDSDeger S.Lee J.C.Whitmore B.C.Thilker D.A.Boquien M.Chandar R.,Dale D.A.Ubeda L.White R.Grasha K.Glover S.C.O.Schruba A.,Barnes A.T.Klessen R.Kruijssen J.M.D.Rosolowsky E.Williams T.G.2025-02-13T20:15:36Z2024-11-14T15:22:59ZCDS support team

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

cds-question@unistra.frgalaxiesstellar-associationsglobular-star-clustersopen-star-clustersstar-forming-regionsultraviolet-astronomyvisible-astronomyinfrared-photometrybroad-band-photometryphotometryclassificationastrometrystellar-agesstellar-massestwo-color-diagramsgalaxy-classification-systemsUsing PHANGS-HST NUV-U-B-V-I imaging of 17 nearby spiral galaxies, we study samples of star clusters and stellar associations, visually selected to be bright and relatively isolated, for three purposes: to compute aperture corrections for star cluster photometry, to explore the utility of quantitative morphologies in the analysis of clusters and associations, and to compare to synthetic stellar population models. We provide a technical summary of our procedures to determine aperture corrections, a standard step in the production of star cluster candidate catalogues, and compare to prior work. We also use this specialized sample to launch an analysis into the measurement of star cluster light profiles. We focus on one measure, M20 (normalized second-order moment of the brightest 20 per cent of pixels), applied previously to study the morphologies of galaxies. We find that M_20_ in combination with UB-VI colours, yields a parameter space where distinct loci are formed by single-peaked symmetric clusters, single-peaked asymmetric clusters, and multipeaked associations. We discuss the potential applications for using M_20_ to gain insight into the formation and evolution of clusters and associations. Finally, we compare the colour distributions of this sample with various synthetic stellar population models. One finding is that the standard procedure of using a single-metallicity SSP track to fit the entire population of clusters in a given galaxy should be revisited, as the oldest globular clusters will be more metal- poor compared to clusters formed recently.2022MNRAS.510...32Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/510/32CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJ/841/92 : Young massive star clusters in 2 LEGUS galaxies (Ryon+, 2017)J/A+A/622/A103 : Python Code Investigating GALaxy Emission (Boquien+, 2019)J/AJ/128/163 : Galaxy morphological classification (Lotz+, 2004)J/MNRAS/458/963 : CANDELS galaxy structure classification (Peth+, 2016)https://archive.stsci.edu/hst/search_retrieve.html : Mikulski Archive home pagehttps://archive.stsci.edu/hlsp/phangs/phangs-hst : PHANGS-HST home pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/510/32https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/510/32http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/510/32https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/510/32https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/510/32http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/510/32GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/510/32/galaxy (Lists of the 17 nearby galaxies in this study)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/510/32/galaxy?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/510/32/galaxy?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/510/32/galaxy?GETtext/xml+votable180.050000true53.4019083-36.14065830.005555555555555556Cone search capability for table J/MNRAS/510/32/tablea1 (The bright, isolated specialized star clusters and associations sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/510/32/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/510/32/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/510/32/tablea1?GETtext/xml+votable180.050000true194.1903738921.695518890.0055555555555555566/4149 26472 27514 27728 27917-27918 27937 27942 28015 28167 33228 33958 34272 34343 34531 40328https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/510/32?format=asciiUVOpticalInfrareddefaultJ/MNRAS/510/32/galaxyLists of the 17 nearby galaxies in this studyrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalaxyName of the nearby galaxy (galaxy)meta.id;meta.maincharNumberNumber of associated stars in the tablea1 (N)meta.numberintSimbadNameSimbad column added by the CDSmeta.idcharnullable_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.mainnullable_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainnullableJ/MNRAS/510/32/tablea1The bright, isolated specialized star clusters and associations sampleUmagU apparent magnitude in Vega Systems four pixel circular aperture photometry HST/WFC3 UVIS-F336W Stromgren u filter (m_{U}_) (1)magphot.mag;em.opt.Ufloate_UmagMean error of e_Umag ({delta}m_{U}_)magstat.error;phot.magfloatBmagB apparent magnitude in Vega Systems four pixel circular aperture photometry HST/WFC3 UVIS-F438W WFPC2 B filter (m_{B}_) (1)magphot.mag;em.opt.Bfloate_BmagMean error of Bmag ({delta}m_{B}_)magstat.error;phot.magfloatVmagV apparent magnitude in Vega Systems four pixel circular aperture photometry HST/WFC3 UVIS-F555W WFPC2 V filter (m_{V}_) (1)magphot.mag;em.opt.VfloatRAJ2000Right ascension (J2000) (RA)degpos.eq.ra;meta.mainE(B-V)Color excess of (B-V) as discussed in the section 3.2 sample properties (E(B-V))magphot.color.excessfloate_E(B-V)({delta}E(B-V)magstat.errorfloatM20Normalized second-order moment (M_{20}_) (3)stat.fit.paramfloatCIThe morphology concentration index (CI) (4)src.morph.paramfloatClassThe visual morphology class (Class) (5)meta.code.classintrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalaxyHost galaxy name as in the list seen in section 2 PHANGS-HST Imaging (Galaxy)meta.id;meta.maincharDEJ2000Declination (J2000) (Dec)degpos.eq.dec;meta.mainXpixel position (X)pixpos;instr.pixelfloatYpixel position (Y)pixpos;instr.pixeldoubleNUVmagNear-UV apparent magnitude in Vega Systems four pixel circular aperture photometry HST/WFC3 UVIS-F275W UV wide filter (m_{NUV}_) (1)magphot.mag;em.UV.200-300nmfloate_NUVmagMean error of NUVmag ({delta}m_{NUV}_)magstat.error;phot.magfloate_VmagMean error of Vmag ({delta}m_{V}_)magstat.error;phot.magfloatImagI apparent magnitude in Vega Systems four pixel circular aperture photometry HST/WFC3 UVIS-F814W WFPC2 Wide I filter (m_{I}_) (1)magphot.mag;em.opt.Ifloate_ImagMean error of Imag ({delta}m_{I}_)magstat.error;phot.magfloatAgeThe {Chi}^2^ minimization age (Age) (2)Myrtime.agedoublee_AgeMean error of Age ({delta}Age)Myrstat.error;time.agedoubleM*{Chi}^2^ minimization stellar mass (Mass) (2)solMassphys.massdoublee_M*Mean error of M* ({delta}Mass)solMassstat.errordouble