J/MNRAS/444/290ivo://CDS.VizieR/J/MNRAS/444/290doi:10.26093/cds/vizier.74440290CDSBuckner A.S.M.Froebrich D.2024-08-10T20:18:49Z2015-07-31T12:49:58ZCDS support team

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

cds-question@unistra.frstellar-associationsopen-star-clustersstellar-distanceextinctionUntil now, it has been impossible to observationally measure how star cluster scaleheight evolves beyond 1Gyr as only small samples have been available. Here, we establish a novel method to determine the scaleheight of a cluster sample using modelled distributions and Kolmogorov-Smirnov tests. This allows us to determine the scaleheight with a 25% accuracy for samples of 38 clusters or more. We apply our method to investigate the temporal evolution of cluster scaleheight, using homogeneously selected sub-samples of Kharchenko et al. (MWSC, 2012, Cat. J/A+A/543/A156, 2013, J/A+A/558/A53 ), Dias et al. (DAML02, 2002A&A...389..871D, Cat. B/ocl), WEBDA, and Froebrich et al. (FSR, 2007MNRAS.374..399F, Cat. J/MNRAS/374/399). We identify a linear relationship between scaleheight and log(age/yr) of clusters, considerably different from field stars. The scaleheight increases from about 40pc at 1Myr to 75pc at 1Gyr, most likely due to internal evolution and external scattering events. After 1Gyr, there is a marked change of the behaviour, with the scaleheight linearly increasing with log(age/yr) to about 550pc at 3.5Gyr. The most likely interpretation is that the surviving clusters are only observable because they have been scattered away from the mid-plane in their past. A detailed understanding of this observational evidence can only be achieved with numerical simulations of the evolution of cluster samples in the Galactic disc. Furthermore, we find a weak trend of an age-independent increase in scaleheight with Galactocentric distance. There are no significant temporal or spatial variations of the cluster distribution zero-point. We determine the Sun's vertical displacement from the Galactic plane as Z_{sun}_=18.5+/-1.2pc.2014MNRAS.444..290Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/444/290CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/374/399 : Infrared star clusters with |b|<20{deg} (Froebrich+, 2007)J/MNRAS/409/1281 : Old star clusters in the FSR catalogue (Froebrich+, 2010)J/MNRAS/436/1465 : Star clusters distances and extinctions (Buckner+, 2013)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/444/290https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/444/290http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/444/290https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/444/290https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/444/290http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/444/290GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/444/290/tablea1 (Summary table of the FSR cluster properties determined with our isochrone-fitting pipeline)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/444/290/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/444/290/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/444/290/tablea1?GETtext/xml+votable180.050000true273.9494-22.13720.0055555555555555566/1101 1117 1267 1285 1302 1308 1335 1446 1452 1457 1462 1481-1482 1514 1582 1782-1783 1801 1839 2940 3047 3052 3059 3061-3063 3091 3147 3149 3158 3168 3186 3227 3254 3274 3277 3298 3304-3305 3335 3362 3493 3584 3621-3623 3631-3634 3636 3638 3640 3642 3644 3649 3712 3715 3718 3723-3724 3743 6149 6307 12941 12990 13048 13050 13291 13996 14013-14014 14237 14242 14246 14251 14263 14268 14270 14280 14288 14295 14301 14306 14310 14314 14316 14320 14331 14400 14415 14427 14575 14604 14606 14620 14624 14626 14632 14643-14644 14653 14669 14740 14749 14752 14800 15363 15374 15379 15384 15386 15412 15430 15434 15443 15447-15448 15489 15622 15629 15632-15633 15670 15687 15709 15711 15716 15759 20833 20989 21513 21519 21550 21557 21586 21602 21633 21656 21658 21719 22021 22038 22065 22071 22130 22161 22163 22210-22211 22219 22245 22499 23620 23626 23645 23696 23745 23761 23768 23906 23976 24123 24291 24322 24326 24333 24344 24376 24466 24470 24476 24496 24510 24527 29066 29106 29870 30208 30215 30257 30335 30407 30427 30506 30595 30622 30654 30692 30704 32089 37230 37237 37297 37349 37364 37366 37368 37371 37373 37375 37592 37717-37718 37721 37753 37851 37863 37874 37883 37899-37901 37906 37914 37920 37924 37926 37929 37932 37934 37942 37971 38016 38024 38026 38048 38441 38529 38537 39189 39196 39233 39238 39249 39274 39278-39279 39284 39286 39359 39420 39752 39754 39756 39766 39770 39776 39779 39781 39879 39883 39906 39910 39919-39920 39944 39977 40064 40071 40101 40104 40451 40610 40620 40625 41466 41613 41620 41649 41682 41699 41768-41769 41809 42153 42177 42218 42274 42548 43014 43016 43018 43022 43033-43034 43140https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/444/290?format=asciidefaultJ/MNRAS/444/290/tablea1Summary table of the FSR cluster properties determined with our isochrone-fitting pipelinerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintpDetails from previous papers about this clustermeta.ref.urlintnullableFSR[32/1738] FSR number, <[FSR2007] NNNN> in Simbadmeta.id;meta.mainintTypeKnown open cluster or New clustermeta.codecharClass[OC PMS] Cluster class: OC (open cluster) or PMS (contains pre-Main-Sequence stars)meta.code.classcharGLONGalactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latDP1[1.1/11] Distance determined using our photometric method in Paper I (J/MNRAS/436/1465)kpcpos.distance;pos.heliocentricfloatDP2[0.4/12] Distance determined using our pipelinekpcpos.distance;pos.heliocentricfloate_DP2[0/1] rms uncertainty on DP2kpcstat.errorfloatAP1HH-band extinction values calculated from H-K excess using our photometric method in Paper I (Buckner & Froebrich 2013, J/MNRAS/436/1465)magphys.absorptionfloatAP2HH-band extinction values calculated from H-K excess using our pipelinemagphys.absorptionfloate_AP2Hrms uncertainty on AP2H (1)magstat.errorfloatlogAge[6.7/10] Agelog(yr)time.agefloate_logAge[0/0.4] rms uncertainty on logAge (1)log(yr)stat.error;time.agefloatSimbadSimbad column added by the CDSmeta.ref.urlchar_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data)degpos.eq.ranullableindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data)degpos.eq.decnullableindexed