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<ri:Resource created="2012-08-15T11:28:20Z" 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>Lick indices of type II Cepheid candidates</title><shortName>J/AJ/141/53</shortName><identifier>ivo://CDS.VizieR/J/AJ/141/53</identifier><altIdentifier>doi:10.26093/cds/vizier.51410053</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Schmidt E.G.</name></creator><creator><name>Rogalla D.</name></creator><creator><name>Thacker-Lynn L.</name></creator><date role="Updated">2017-10-12T13:00:18Z</date><date role="Created">2012-08-15T11:28:20Z</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>spectroscopy</subject><description>We present low-resolution spectra for variable stars in the Cepheid period range from the ROTSE-I Demonstration Project and the All Sky Automated Survey, some of which were previously identified as type II Cepheid candidates. We have derived effective temperatures, gravities, and metallicities from the spectra. Based on this, three types of variables were identified: Cepheid strip stars, cool stars that lie along the red subgiant and giant branch, and cool main-sequence stars. Many fewer type II Cepheids were found than expected and most have amplitudes less than 0.4mag. The cool variables include many likely binaries as well as intrinsic variables. Variation among the main-sequence stars is likely to be mostly due to binarity or stellar activity.</description><source format="bibcode">2011AJ....141...53S</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/141/53</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/J/AJ/133/665">J/AJ/133/665 : Photometry of type II Cepheid candidates (Schmidt+, 2007)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/137/4598">J/AJ/137/4598 : VR light curve of ASAS-North Cepheids (Schmidt+, 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