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<ri:Resource created="2014-10-06T07:58:31Z" status="active" updated="2025-05-19T09:50:00Z" 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>Spectra and radial velocities of nuclear stars</title><shortName>J/A+A/570/A2</shortName><identifier>ivo://CDS.VizieR/J/A+A/570/A2</identifier><altIdentifier>doi:10.26093/cds/vizier.35700002</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Feldmeier A.</name></creator><creator><name>Neumayer N.</name></creator><creator><name>Seth A.</name></creator><creator><name>Schodel R.</name></creator><creator><name>Lutzgendorf N.,de Zeeuw P.T.</name></creator><creator><name>Kissler-Patig M.</name></creator><creator><name>Nishiyama S.</name></creator><creator><name>Walcher C.J.</name></creator><date role="Updated">2017-06-26T11:49:52Z</date><date role="Created">2014-10-06T07:58:31Z</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>radial-velocity</subject><subject>infrared-astronomy</subject><subject>spectroscopy</subject><description>Within the central 10pc of our Galaxy lies a dense cluster of stars. This nuclear star cluster forms a distinct component of the Galaxy, and similar nuclear star clusters are found in most nearby spiral and elliptical galaxies. Studying the structure and kinematics of nuclear star clusters reveals the history of mass accretion and growth of galaxy nuclei and central massive black holes. Because the Milky Way nuclear star cluster is at a distance of only 8 kpc, we can spatially resolve the cluster on sub-parsec scales. 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