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<ri:Resource created="2024-04-26T07:22:14Z" status="active" updated="2025-11-27T20:02:24Z" 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>UBV &amp; Gaia DR3 photometry of King 6 and NGC 1605</title><shortName>J/AJ/166/263</shortName><identifier>ivo://CDS.VizieR/J/AJ/166/263</identifier><altIdentifier>doi:10.26093/cds/vizier.51660263</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Gokmen S.</name></creator><creator><name>Eker Z.</name></creator><creator><name>Yontan T.</name></creator><creator><name>Bilir S.</name></creator><creator><name>Ak T.</name></creator><creator><name>Ak S.</name></creator><creator><name>Banks T.,Sarajedini A.</name></creator><date role="Updated">2025-11-27T20:02:24Z</date><date role="Created">2024-04-26T07:22:14Z</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>visible-astronomy</subject><subject>broad-band-photometry</subject><subject>proper-motions</subject><subject>trigonometric-parallax</subject><description>A detailed analysis of ground-based CCD UBV photometry and space-based Gaia Data Release 3 (DR3) data for the open clusters King-6 and NGC-1605 was performed. Using the pyUPMASK algorithm on Gaia astrometric data to estimate cluster membership probabilities, we have identified 112 stars in King 6 and 160 stars in NGC-1605 as the statistically most likely members of each cluster. We calculated reddening and metallicity separately using UBV two-color diagrams to estimate parameter values via independent methods. The color excess E(B-V) and photometric metallicity [Fe/H] for King-6 are 0.515{+/-}0.030mag and 0.02{+/-}0.20dex, respectively. For NGC-1605, they are 0.840{+/-}0.054mag and 0.01{+/-}0.20dex, respectively. With reddening and metallicity kept constant, we have estimated the distances and cluster ages by fitting PARSEC isochrones to color-magnitude diagrams based on the Gaia and UBV data. The photometric distances are 723{+/-}34pc for King-6 and 3054{+/-}243pc for NGC-1605. The cluster ages are 200{+/-}20Myr and 400{+/-}50 Myr for King-6 and NGC-1605, respectively. The mass function slopes were found to be 1.29{+/-}0.18 and 1.63{+/-}0.36 for King-6 and NGC-1605, respectively. These values are in good agreement with the value of Salpeter. The relaxation times were estimated as 5.8Myr for King-6 and60 Myr for NGC-1605. These indicate that both clusters are dynamically relaxed since these times are less than the estimated cluster ages. A Galactic orbit analysis shows that both clusters formed outside the solar circle and are members of the young thin-disk population.</description><source format="bibcode">2023AJ....166..263G</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/166/263</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, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/350">I/350 : Gaia EDR3 (Gaia Collaboration, 2020)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/164">V/164 : LAMOST DR5 catalogs (Luo+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/109/375">J/A+AS/109/375 : Blue stragglers in open clusters (Ahumada+, 1995)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/133/387">J/A+AS/133/387 : NGC 1817 and NGC 1807 proper motions (Balaguer-Nunnez+ 1998)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/115/592">J/AJ/115/592 : VI photometry of NGC 2157 (Fischer+, 1998)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/329/101">J/A+A/329/101 : Masses of Pleiades members (Raboud+ 1998)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+AS/141/491">J/A+AS/141/491 : Chemical composition of halo and disk stars (Nissen+, 2000)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/438/1163">J/A+A/438/1163 : Catalogue of Open Cluster Data (COCD) (Kharchenko+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/131/1184">J/AJ/131/1184 : Recalibration of optical photometry (Maiz-Apellaniz+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/137/4186">J/AJ/137/4186 : UBVRI standards around celestial equator (Landolt, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/141/92">J/AJ/141/92 : BVI photometry of 10 distant open clusters (Janes+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/543/A156">J/A+A/543/A156 : Milky Way global survey of star clusters (Kharchenko+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/764/73">J/ApJ/764/73 : HST VI photometry of HD 97950 cluster members (Pang+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/430/3350">J/MNRAS/430/3350 : Proper motions and membership in NGC 3766 (Yadav+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/147/139">J/AJ/147/139 : UBVRI CCD photo open clusters. 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Cluster</name><description>Cluster identifier</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="8*">char</dataType></column><column><name>Seq</name><description>[1/2474] Sequential identifier in Cluster</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>RAICRS</name><description>[3/4] Hour of Right Ascension (ICRS at Epoch=2016)</description><ucd>pos.eq.ra;meta.main</ucd></column><column><name>DEICRS</name><description>[45/56] Degree of Declination (ICRS at Epoch=2016)</description><ucd>pos.eq.dec;meta.main</ucd></column><column><name>Vmag</name><description>[9.99/21] TUG/T100 V band magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_Vmag</name><description>[0/0.2] Uncertainty in Vmag</description><unit>mag</unit><ucd>stat.error;phot.mag</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>U-B</name><description>[-4.52/2.3]? 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