J/MNRAS/417/L6ivo://CDS.VizieR/J/MNRAS/417/L6doi:10.26093/cds/vizier.74179006CDSBastian N.Adamo A.Gieles M.Lamers H.J.G.L.M.Larsen S.S.,Silva-Villa E.Smith L.J.Kotulla R.Konstantopoulos I.S.Trancho G.,Zackrisson E.2024-07-15T20:17:06Z2011-11-04T07:07:23ZCDS support team

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

cds-question@unistra.frgalaxiesopen-star-clustersinfrared-photometryvisible-astronomybroad-band-photometryh-alpha-photometryWe study the stellar cluster population in two adjacent fields in the nearby, face-on spiral galaxy, M83, using multi-wavelength WFC3/HST imaging. After automatic detection procedures, the clusters are selected through visual inspection to be centrally concentrated, symmetric, and resolved on the images, which allows us to differentiate between clusters and likely unbound associations. We compare our sample with previous studies and show that the differences between the catalogues are largely due to the inclusion of large numbers of diffuse associations within previous catalogues as well as the inclusion of the central starburst region, where the completeness limit is significantly worse than in the surrounding regions. We derive the size distribution of the clusters, which is well described by a log-normal distribution with a peak at ~2.5pc, and find evidence for an expansion in the half-light radius of clusters with age. The luminosity function of the clusters is well approximated by a power-law with index, -2, over most of the observed range, however a steepening is seen at M_V=-9.3 and -8.8 in the inner and outer fields, respectively. Additionally, we show that the cluster population is inconsistent with a pure power-law mass distribution, but instead exhibits a truncation at the high mass end. If described as a Schechter function, the characteristic mass is 1.6 and 0.5x10^5^M_{sun}_, for the inner and outer fields, respectively, in agreement with previous estimates of other cluster populations in spiral galaxies. Comparing the predictions of the mass independent disruption (MID) and mass dependent disruption (MDD) scenarios with the observed distributions, we find that both models can accurately fit the data. However, for the MID case, the fraction of clusters destroyed (or mass lost) per decade in age is dependent on the environment, hence, the age/mass distributions of clusters are not universal. In the MDD case, the disruption timescale scales with galactocentric distance (being longer in the outer regions of the galaxy) in agreement with analytic and numerical predictions. Finally, we discuss the implications of our results on other extragalactic surveys, focussing on the fraction of stars that form in clusters and the need (or lack thereof) for infant mortality.2011MNRAS.417L...6Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/417/L6CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/AJ/122/3046 : HST photometry of star clusters in NGC 5236 (Harris+, 2001)J/ApJ/591/L111 : Period of Cepheids in M 83 (Bonanos+, 2003)J/A+A/410/53 : M83 X-ray sources (Soria+, 2003)J/A+A/439/265 : Wolf-Rayet population in M83 (Hadfield+, 2005)J/A+A/489/533 : M83 volume densities of giant molecular clouds (Heiner+, 2008)J/AJ/136/479 : IRAC observations of M83 extended UV disk (Dong+, 2008)J/ApJ/695/580 : Oxygen abundance in M83 (Bresolin+, 2009)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/417/L6https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/417/L6http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/417/L6https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/417/L6https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/417/L6http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/417/L6GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tap2.0401237512456292e-19 4.2441532724171825e-19OpticalInfrareddefaultJ/MNRAS/417/L6/catalogCluster positions, photometry, propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintF[1/2] WFC3 Field: 1=Inner, 2=Outer (1)obs.fieldintIDCluster ID within the fieldmeta.id;meta.mainintXposx-position of cluster in WFC3 FOVpixpos.cartesian.x;instr.detfloatYposy-position of cluster in WFC3 FOVpixpos.cartesian.y;instr.detfloatlogAgeLogarithm of the cluster agelog(yr)time.agefloatlogMLogarithm of the cluster masslog(solMass)phys.massfloatAVV-band extinctionmagphys.absorption;em.opt.VfloatR(B)? Effective radius in the B-bandpcphys.size.radiusfloatnullableR(V)? Effective radius in the V-bandpcphys.size.radiusfloatnullableR(I)? Effective radius in the I-bandpcphys.size.radiusfloatnullableUmagU-band (F336W) corrected magnitude (2)magphot.mag;em.opt.Ufloate_UmagU-band errormagstat.error;phot.mag;em.opt.UfloatBmagB-band (F438W) corrected magnitude (2)magphot.mag;em.opt.Bfloate_BmagB-band errormagstat.error;phot.mag;em.opt.BfloatVmagV-band (F555W) corrected magnitude (2)magphot.mag;em.opt.Vfloate_VmagV-band errormagstat.error;phot.mag;em.opt.VfloatHamag? H{alpha}-band (F657N) magnitude (2)magphot.flux;em.line.Halphafloatnullablee_Hamag? H{alpha}-band errormagstat.error;phot.mag;em.IR.HfloatnullableImagI-band (F814W) corrected magnitude (2)magphot.mag;em.opt.Ifloate_ImagI-band errormagstat.error;phot.mag;em.opt.Ifloat