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<ri:Resource created="2000-11-19T10:06:38Z" 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>Kinematics of Mira stars</title><shortName>J/MNRAS/317/460</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/317/460</identifier><altIdentifier>doi:10.26093/cds/vizier.73170460</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Feast M.W.</name></creator><creator><name>Whitelock P.A.</name></creator><date role="Updated">2024-06-26T20:16:39Z</date><date role="Created">2000-11-19T10:06:38Z</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>variable-stars</subject><subject>radial-velocity</subject><subject>apparent-magnitude</subject><description>The space motions of Mira variables are derived from radial velocities, Hipparcos (&lt;I/239&gt;) proper motions and a period-luminosity relation. The previously known dependence of Mira kinematics on the period of pulsation is confirmed and refined. In addition, it is found that Miras with periods in the range 145-200d in the general Solar neighbourhood have a net radial outward motion from the Galactic Centre of 75+/-18km/s. This, together with a lag behind the circular velocity of Galactic rotation of 98+/-19km/s, is interpreted as evidence for an elongation of their orbits, with their major axes aligned at an angle of ~17{deg} with the Sun-Galactic Centre line, towards positive Galactic longitudes. This concentration seems to be a continuation to the Solar circle and beyond of the bar-like structure of the Galactic bulge, with the orbits of some local Miras probably penetrating into the bulge. These conclusions are not sensitive to the distance scale adopted. A further analysis is given of the short-period (SP) red group of Miras discussed in companion papers in this series. In Appendix A the mean radial velocities and other data for 842 oxygen-rich Mira-like variables are tabulated. These velocities were derived from published optical and radio observations.</description><source format="bibcode">2000MNRAS.317..460F</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/317/460</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/239">I/239 : The Hipparcos and Tycho Catalogues (ESA 1997)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL 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