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<ri:Resource created="2009-02-16T22:39:06Z" 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>Velocities of blue stars near (l,b)=(198,-27)</title><shortName>J/ApJ/588/824</shortName><identifier>ivo://CDS.VizieR/J/ApJ/588/824</identifier><altIdentifier>doi:10.26093/cds/vizier.15880824</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Yanny B.</name></creator><creator><name>Newberg H.J.</name></creator><creator><name>Grebel E.K.</name></creator><creator><name>Kent S.</name></creator><creator><name>Odenkirchen M.</name></creator><creator><name>Rockosi C.M.,Schlegel D.</name></creator><creator><name>Subbarao M.</name></creator><creator><name>Brinkmann J.</name></creator><creator><name>Fukugita M.</name></creator><creator><name>Ivezic Z.</name></creator><creator><name>Lamb D.Q.,Schneider D.P.</name></creator><creator><name>York D.G.</name></creator><date role="Updated">2009-02-16T21:43:39Z</date><date role="Created">2009-02-16T22:39:06Z</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>halo-stars</subject><subject>radial-velocity</subject><subject>visible-astronomy</subject><subject>sloan-photometry</subject><description>We present evidence for a ring of stars in the plane of the Milky Way, extending at least from l=180{deg} to 227{deg} with turnoff magnitude g~19.5; the ring could encircle the Galaxy. We infer that the low Galactic latitude structure is at a fairly constant distance of R=18+/-2kpc from the Galactic center above the Galactic plane and has R=20+/-2kpc in the region sampled below the Galactic plane. The evidence includes 500 Sloan Digital Sky Survey spectroscopic radial velocities of stars within 30{deg} of the plane. The velocity dispersion of the stars associated with this structure is found to be 27km/s at (l, b)=(198, -27), 22km/s at (l, b)=(225, 28), 30km/s at (l, b)=(188, 24), and 30km/s at (l, b)=(182, 27). The structure rotates in the same prograde direction as the Galactic disk stars but with a circular velocity of 110+/-25km/s. 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