J/MNRAS/482/2530ivo://CDS.VizieR/J/MNRAS/482/2530doi:10.26093/cds/vizier.74822530CDSRandriamanakoto Z.Vaisanen P.Ryder S.D.Ranaivomanana P.2024-08-19T20:14:49Z2022-08-02T08:39:45ZCDS support team

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

cds-question@unistra.frgalaxiesphotometryvisible-astronomyArchival WFC3/UVIS imaging of Arp 299 (NGC3690E+NGC3690W) is retrieved to investigate the young massive cluster (YMC) population of this ongoing merger. We extract 2182 cluster candidates, including 1323 high confidence photometric sources. Multiband photometry is matched with Yggdrasil models to estimate the age, mass, and extinction of each cluster. A Schechter fit of the truncated cluster mass function results in a characteristic mass M_*_=1.6x10^6^M_{sun}_. Ou results confirm that intensely star-forming galaxies such as Arp299 host more massive clusters than quiescent dwarf and normal spirals. In the case of NGC3690E, we find that the cluster masses decrease with an increasing galactocentric radius likely due to the gas density distribution. On the other hand, the fitted age distributions of a mass-limited sample suggest that YMCs of the western component undergo stronger disruption than those hosted by the eastern galaxy. This is in agreement with the properties of the underlying cluster luminosity functions: a clear truncation at high luminosities with slopes generally shallower by ~0.3dex than the ones of the NGC3690E. Finally, the derived cluster formation efficiency, {Gamma}~19 per cent, indicates that Arp299 has ~3-5 times more star formation happening in bound clusters compared to the cases of gas-poor spirals like NGC2997 and NGC4395. The merger generally follows the {Gamma} - star formation rate density relation from the literature. The YMC photometric study of Arp299 thus reveals that both formation and disruption mechanisms of the star cluster population are most likely environment dependent.2019MNRAS.482.2530Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/482/2530CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/482/2530https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/482/2530http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/482/2530https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/482/2530https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/482/2530http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/482/2530GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/482/2530/table3 (Catalogue of the SSC candidates in the field of Arp299)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/482/2530/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/482/2530/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/482/2530/table3?GETtext/xml+votable180.050000true172.10572916758.5713222220.0055555555555555566/60982.0401237512456292e-19 2.706461185444514e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/482/2530?format=asciiOpticaldefaultJ/MNRAS/482/2530/table3Catalogue of the SSC candidates in the field of Arp299recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintIDSuper star cluster (SCS) candidate identificationmeta.id;meta.mainintRAJ2000Right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Declination (J2000)degpos.eq.dec;meta.mainUmagVega-based apparent magnitude in the U-band (F336W)magphot.mag;em.opt.Ufloate_UmagError on instrumental Umag (1)magstat.error;phot.magfloatBmagVega-based apparent magnitude in the B-band (F438W)magphot.mag;em.opt.Bfloate_BmagError on instrumental Bmag (1)magstat.error;phot.magfloatImagVega-based apparent magnitude in the I-band (F814W)magphot.mag;em.opt.Ifloate_ImagError on instrumental Imag (1)magstat.error;phot.magfloatAVDerived extinctionmagphys.absorptionfloatAgeLog of cluster agelog(yr)time.agefloatMassLog of cluster masslog(solMass)phys.massfloat