J/A+A/692/A194ivo://CDS.VizieR/J/A+A/692/A194doi:10.26093/cds/vizier.36920194CDSGupta A.Ivanov V.D.Preibisch T.Minniti D.2025-02-26T20:02:23Z2024-12-13T10:41:38ZCDS support team

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

cds-question@unistra.fropen-star-clustersstellar-associationsinfrared-photometryMilky Way star clusters provide important clues for the history of the star formation in our Galaxy. However, the dust in the disk and the innermost regions hides them from the observers. Our goal is twofold. First, to detect new clusters - we apply the newest methods for the detection of clustering with the best available wide-field sky surveys in the mid-infrared because they are the least affected by extinction. Second, we address the question of cluster detection's completeness, for now limiting it to the most massive star clusters. This search is based on the mid-infrared Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE), to minimize the effect of dust extinction. The search Ordering Points To Identify the Clustering Structure (OPTICS) clustering algorithm is applied to identify clusters, after excluding the bluest, presumably foreground sources, to improve the cluster-to-field contrast. The success rate for cluster identification is estimated with a semi-empirical simulation that adds clusters, based on the real objects, to the point source catalog, to be recovered later with the same search algorithm that was used in the search for new cluster candidates. As a first step, this is limited to the most massive star clusters with a total mass of ~10^4 M_sun. Our automated search, combined with inspection of the color-magnitude diagrams and images yielded 659 cluster candidates; 106 of these appear to have been previously identified, suggesting that a large hidden population of star clusters still exists in the inner Milky Way. However, the search for the simulated supermassive clusters achieves a recovery rate of 70-95%, depending on the distance and extinction toward them. The new candidates - if confirmed - indicate that the Milky Way still harbors a sizeable population of still unknown clusters. However, they must be objects of modest richness, because our simulation indicates that there is no substantial hidden population of supermassive clusters in the central region of our Galaxy.2024A&A...692A.194Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/692/A194CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/692/A194https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/692/A194http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/692/A194https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/692/A194https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/692/A194http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/692/A194GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/692/A194/table3 (The catalog of GLIMPSE clusters)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/692/A194/table3?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/692/A194/table3?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/692/A194/table3?GETtext/xml+votable180.050000true266.082945847-28.6802524290.0055555555555555565/7202-7203 7206 7229 7274 7376-7377 7383 7564-7565 7654 7679 10453 10556 10595 10597 10614-10615 6/12970-12971 12974 14337 14352-14353 14355-14356 14358-14359 14402-14403 14406 14409 14413 28806 28817-28818 28828 28830-28831 28836-28837 28849 28868 28874-28876 28878-28879 28891 28896 28898-28901 28912-28913 28915 28920-28921 29070 29088 29090-29091 29094 29101-29103 29112-29113 29115-29116 29118 29162-29163 29166 29440 29457 29460 29515 29522-29523 29528-29529 30216 30218 30240-30241 30243-30245 30267 30307 30312-30313 30315 30317-30319 30330 30405 30416-30417 30420-30422 30592 30594-30595 30600 30605 30622-30623 30645 30688 30691-30692 30694 30707 30710 30713-30714 37895 37904 41595 41598-41599 41654-41655 41658 41660-41662 41671 41673-41678 41681-41683 41688 41696-41697 41759 41763 41765-41768 41770 41772-41773 41776 41778-41782 41800 41802-41803 41806-41807 41817 41820 42157 42159 42170-42173 42175 42190 42206-42207 42210-42211 42213-42217 42221 42228-42230 42376 42378-42379 42387 42392-42393 42395-42398 42417 42434-42438 42440-42441 42444-42445 42447-42448 42450-42451 42454-42455 42497-42499 42501-42502 42512 42561 43013-43015 43017-43021 43024 43026 43040-43041https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/692/A194?format=asciiInfrareddefaultJ/A+A/692/A194/table3The catalog of GLIMPSE clustersoverdensOverdensitymeta.notefloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintObjectIdentifier of the object (GIPM NNN)meta.id;meta.maincharGLONGalactic Longitudedegpos.galactic.lonGLATGalactic Latitudedegpos.galactic.latRaddegRadius in degreesdegstat.fit.dof;phys.angSizedoubleRadarcminRadius in arcminarcminphys.angSizefloatNstarsNumber of stars in the clustermeta.numberintONamesExisting IDs from SIMBADmeta.idchar_RA.icrsRight ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.raindexed_DE.icrsDeclination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)degpos.eq.decindexed