J/MNRAS/520/2180ivo://CDS.VizieR/J/MNRAS/520/2180doi:10.26093/cds/vizier/bg-g8-244CDSClaeyssens A.Adamo A.Richard J.Mahler G.Messa M.,Dessauges-Zavadsky M.2026-08-03T07:32:38Z2026-04-24T15:17:02ZCDS support team

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

cds-question@unistra.frgalaxy-clustersgalaxiesgravitational-lensingphotometryinfrared-astronomyastrometryredshiftedstar-forming-regionsextinctionstellar-ageschemical-abundancesWe present the clump populations detected in 18 lensed galaxies at redshifts 1-- 8.5 within the lensing cluster field SMACS0723. The recent JWST Early Release Observations of this poorly known region of the sky have revealed numerous point-like sources within and surrounding their host galaxies, undetected in the shallower Hubble Space Telescope images. We use JWST multi-and photometry and the lensing model of this galaxy cluster to estimate the intrinsic sizes and magnitudes of the stellar clumps. We derive optical restframe effective radii from <10 to hundreds pc and masses ranging from ~10^5^ to 10^9^ M_{sun}_, overlapping with massive star clusters in the local universe. Clump ages range from 1 Myr to 1 Gyr. We compare the crossing time to the age of the clumps and determine that between 45 and 60 per cent of the detected clumps are consistent with being gravitationally bound. On average, the dearth of Gyr old clumps suggests that the dissolution time scales are shorter than 1 Gyr. We see a significant increase in the luminosity (mass) surface density of the clumps with redshift. Clumps in reionization era galaxies have stellar densities higher than star clusters in the local universe. We zoom in into single galaxies at redshift <6 and find for two galaxies, the Sparkler and the Firework, that their star clusters/clumps show distinctive colour distributions and location surrounding their host galaxy that are compatible with being accredited or formed during merger events. The ages of some of the compact clusters are between 1 and 4 Gyr, e.g. globular cluster precursors formed around 9--12 Gyr ago. Our study, conducted on a small sample of galaxies, shows the potential of JWST observations for understanding the conditions under which star clusters form in rapidly evolving galaxies.2023MNRAS.520.2180Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/520/2180CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/666/A80 : Star clusters and fields in the LMC (Narloch+, 2022)J/ApJ/884/85 : RELICS: Reionization Lensing Cluster Survey (Coe+, 2019)J/ApJ/686/948 : CO in extragalactic giant molecular clouds (Bolatto+,2008)J/ApJ/499/112 : HST CFRS and LDSS redshift surveys. I. (Brinchmann+ 1998)J/ApJS/157/1 : Red-Sequence Cluster Survey (Gladders+, 2005)J/AJ/140/75 : Antennae galaxies (NGC 4038/4039) revisitedJ/ApJS/107/1 : Morphologies of distant galaxies II (Abraham+ 1996)J/other/NatAs/2.76 : MACSJ1206.2-08474714 clumps photometry (Cava+, 2018)I/350 : Gaia EDR3 (Gaia Collaboration, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/520/2180https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/520/2180http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/520/2180https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/520/2180https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/520/2180http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/520/2180GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/520/2180/galaxies (Selected galaxies in SMACS J0723.3-7327 cluster)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/520/2180/galaxies?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/520/2180/galaxies?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/520/2180/galaxies?GETtext/xml+votable180.050000true110.8054167-73.45452780.005555555555555556Cone search capability for table J/MNRAS/520/2180/tableb1 (NIRCam photometry of our clumps sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/520/2180/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/520/2180/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/520/2180/tableb1?GETtext/xml+votable180.050000true110.84069-73.4510650.005555555555555556Cone search capability for table J/MNRAS/520/2180/tableb2 (Main astrometric informations and physical properties of our the clumps sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/520/2180/tableb2?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/520/2180/tableb2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/520/2180/tableb2?GETtext/xml+votable180.050000true110.84069-73.4510650.0055555555555555566/37395https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/520/2180?format=asciiInfrareddefaultJ/MNRAS/520/2180/galaxiesSelected galaxies in SMACS J0723.3-7327 clusterrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintImgGalaxy images name identifier (ImageID)meta.id;meta.maincharRAJ2000Right ascension of the component (J2000)pos.eq.ra;meta.mainDEJ2000Declination of the component (J2000)pos.eq.dec;meta.mainNclumpNumber of clumps identified in galaxy imagemeta.numberintSimbadNameSimbad column added by the CDSmeta.idcharnullableJ/MNRAS/520/2180/tableb1NIRCam photometry of our clumps samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintImgImage name identifier (ImageID)meta.id.part;meta.maincharClumpClump name identifier (ClumpID)meta.id.part;meta.maincharzRedshift (z)src.redshiftfloatRAJ2000Right ascension (J2000) (RA)degpos.eq.ra;meta.mainDEJ2000Declination (J2000) (DEC)degpos.eq.dec;meta.mainmuLensing magnification factor ({mu})phot.flux;arith.factor;meta.modelledfloatE_muUpper uncertainty of mustat.error;stat.maxfloate_muLower uncertainty of mustat.errorfloatF090WmagThe JWST NIRCam F090W magnitude in AB system (F090W)magphot.mag;em.opt.Ifloate_F090WmagUncertainty of F090Wmagmagstat.errorfloatF150WmagThe JWST NIRCam F150W magnitude in AB system (F150W)magphot.mag;em.IR.Hfloate_F150WmagUncertainty of F150Wmagmagstat.errorfloatF200WmagThe JWST NIRCam F200W magnitude in AB system (F200W)magphot.mag;em.IR.Kfloate_F200WmagUncertainty of F200Wmagmagstat.errorfloatF277WmagThe JWST NIRCam F277W magnitude in AB system (F277W)magphot.mag;em.IR.Kfloate_F277WmagUncertainty of F277Wmagmagstat.errorfloatF356WmagThe JWST NIRCam F356W magnitude in AB system (F356W)magphot.mag;em.IR.3-4umfloate_F356WmagUncertainty of F356Wmagmagstat.errorfloatF444WmagThe JWST NIRCam F444W magnitude in AB system (F444W)magphot.mag;em.IR.4-8umfloate_F444WmagUncertainty of F444Wmagmagstat.errorfloatJ/MNRAS/520/2180/tableb2Main astrometric informations and physical properties of our the clumps sampleReffIntrinsic effective radius measured on NIRCam/F150W with method described in section 5.3 (R_eff_)pcphys.size.radiusintE_Reff? Upper uncertainty of Reffpcstat.error;stat.maxintnullablee_Reff? Lower uncertainty of Reffpcstat.errorintnullableF150WMagThe NIRCam/F150W intrinsic absolute magnitude in AB system (F150Wabs)magphot.mag;em.IR.H;phys.magAbsfloate_F150WMagUncertainty of F150WMagmagstat.errorfloatlogM*? Derived stellar mass with SED analysis reference model explained in section 5 and 6 (logM*)log(solMass)phys.massfloatnullablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintImgImage name identifier (ImageID)meta.id.part;meta.maincharClumpClump name identifier (ClumpID)meta.id.part;meta.maincharzRedshift (z)src.redshiftfloatRAJ2000Right ascension (J2000) (RA)degpos.eq.ra;meta.mainDEJ2000Declination (J2000) (DEC)degpos.eq.dec;meta.mainmuLensing magnification factor ({mu})phot.flux;arith.factor;meta.modelledfloatE_muUpper uncertainty of mustat.error;stat.maxfloate_muLower uncertainty of mustat.errorfloatl_ReffUpper limit flag on Reff valuesmeta.code.errorcharE_logM*? Upper uncertainty of logM*log(solMass)stat.error;stat.maxfloatnullablee_logM*? Lower uncertainty of logM*log(solMass)stat.errorfloatnullableAge? Estimated age with SED analysis reference model explained in section 5 and 6 (Age)Myrmeta.ref;time.age;meta.modelledintnullableE_Age? Upper uncertainty of AgeMyrstat.error;stat.maxintnullablee_Age? Lower uncertainty of AgeMyrstat.error;time.ageintnullableE(B-V)? Estimated extinction with SED analysis reference model explained in section 5 and 6 (EB-V)magphot.color.excessfloatnullableE_E(B-V)? Upper uncertainty of E (B-V)magstat.error;stat.maxfloatnullablee_E(B-V)? Lower uncertainty of E (B-V)magstat.errorfloatnullablen_E(B-V)Note for clumps with an E(B-V) value at fitted with no extinctionmeta.notecharZ? Best estimates of the metallicity fixed to for SED fits either at 0.02, 0.008, 0.004 or 0.0004 (Metallicity)phys.abund.Z;meta.modelledfloatnullable