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<ri:Resource created="2018-03-22T16:18:52Z" 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>Carbon stars in the Galaxy and its satellites</title><shortName>J/MNRAS/453/2653</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/453/2653</identifier><altIdentifier>doi:10.26093/cds/vizier.74532653</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Huxor A.P.</name></creator><creator><name>Grebel E.K.</name></creator><date role="Updated">2024-08-15T20:15:17Z</date><date role="Created">2018-03-22T16:18:52Z</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>milky-way-galaxy</subject><subject>galaxies</subject><subject>carbon-stars</subject><subject>infrared-photometry</subject><subject>stellar-distance</subject><description>We assemble 121 spectroscopically confirmed halo carbon stars, drawn from the literature, exhibiting measurable variability in the Catalina Surveys. We present their periods and amplitudes, which are used to estimate distances from period-luminosity relationships. The location of the carbon stars - and their velocities when available - allow us to trace the streams of the Sagittarius (Sgr) dwarf spheroidal galaxy. These are compared to a canonical numerical simulation of the accretion of Sgr. We find that the data match this model well for heliocentric distances of 15-50kpc, except for a virtual lack of carbon stars in the trailing arm just north of the Galactic plane, and there is only tentative evidence of the leading arm south of the plane. The majority of the sample can be attributed to the Sgr accretion. We also find groups of carbon stars which are not part of Sgr; most of which are associated with known halo substructures. A few have no obvious attribution and may indicate new substructure. We find evidence that there may be a structure behind the Sgr leading stream apocentre, at ~100kpc, and a more distant extension to the Pisces Overdensity also at ~100kpc. We study a further 75 carbon stars for which no good period data could be obtained, and for which NIR magnitudes and colours are used to estimate distances. 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23460 23462 23525 24020 24266 24708 25147 25283 25447 25722 25760 25876 25920 25938 25951 25997 26032 26087 26215 26264 26308 26313 26403 26420 26532 26590 26682 26806 27205 27820 27868 27917 27978 28029 28083 28361 29372 29976 30856 30877 30942 31184 31194 31236 31464 32524 32568 33034 33059 33159 33286 33290 33296 33302-33303 33310 33325 33337 33412 35468 35720 35883 35968-35969 37056 37415 37521 37557 39079 39100 40762 40788 40832 40836 43320 43671 43799 43864 44829 44845 44867 44924 45007 45021 45146 45221 45658 46215 46968 47039 47074 47163 47426 47542 47598 47897 47900 47903 47911 47950 47958 47961 47968 47978 48019 48025 48064 48216 48328 48690 48787 48856 48984 49100</spatial><footprint ivo-id="ivo://ivoa.net/std/moc">https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/453/2653?format=ascii</footprint><waveband>Infrared</waveband></coverage><tableset><schema><name>default</name><table><name>J/MNRAS/453/2653/table1</name><description>Catalogue of variable carbon 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