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<ri:Resource created="2021-05-22T16:15:11Z" status="active" updated="2025-06-13T15:25:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>Updated parameters of 1743 open clusters</title><shortName>J/MNRAS/504/356</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/504/356</identifier><altIdentifier>doi:10.26093/cds/vizier.75040356</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Dias W.S.</name></creator><creator><name>Monteiro H.</name></creator><creator><name>Moitinho A.</name></creator><creator><name>Lepine J.R.D.</name></creator><creator><name>Carraro G.</name></creator><creator><name>Paunzen E.,Alessi B.</name></creator><creator><name>Villela L.</name></creator><date role="Updated">2024-08-21T20:17:41Z</date><date role="Created">2021-05-22T16:15:11Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>open-star-clusters</subject><subject>proper-motions</subject><subject>visible-astronomy</subject><subject>trigonometric-parallax</subject><subject>radial-velocity</subject><description>In this study, we follow up our recent paper (Monteiro et al., 2020MNRAS.499.1874M) and present a homogeneous sample of fundamental parameters of open clusters in our Galaxy, entirely based on Gaia DR2 data. We used published membership probability of the stars derived from Gaia DR2 data and applied our isochrone fitting code, updated as in Monteiro et al. (2020MNRAS.499.1874M), to G_BP_ and G_RP_Gaia DR2 data for member stars. In doing this, we take into account the nominal errors in the data and derive distance, age, and extinction of each cluster. This work therefore provides parameters for 1743 open clusters and, as a by-product, a list of likely not physical or dubious open clusters is provided as well for future investigations. Furthermore, it was possible to estimate the mean radial velocity of 831 clusters (198 of which are new and unpublished so far), using stellar radial velocities from Gaia DR2 catalogue. By comparing the open cluster distances obtained from isochrone fitting with those obtained from a maximum likelihood estimate of individual member parallaxes, we found a systematic offset of (-0.05+/-0.04) mas.</description><source format="bibcode">2021MNRAS.504..356D</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/504/356</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 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