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<ri:Resource created="2016-10-19T09:37:28Z" 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>K2 new planetary and EB candidates</title><shortName>J/A+A/594/A100</shortName><identifier>ivo://CDS.VizieR/J/A+A/594/A100</identifier><altIdentifier>doi:10.26093/cds/vizier.35940100</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Barros S.C.C.</name></creator><creator><name>Demangeon O.</name></creator><creator><name>Deleuil M.</name></creator><date role="Updated">2018-08-31T07:59:58Z</date><date role="Created">2016-10-19T09:37:28Z</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>surveys</subject><subject>multiple-stars</subject><subject>solar-system-planets</subject><description>With only two functional reaction wheels, Kepler cannot maintain stable pointing at its original target field and has entered a new mode of observation called K2. We describe a new pipeline to reduce K2 pixel files into light curves that are later searched for transit like features. Our method is based on many years of experience in planet hunting for the CoRoT mission. Owing to the unstable pointing, K2 light curves present systematics that are correlated with the target position in the ccd. Therefore, our pipeline also includes a decorrelation of this systematic noise. Our pipeline is optimised for bright stars for which spectroscopic follow-up is possible. We achieve a maximum precision on 6 hours of 6 ppm. The decorrelated light curves are searched for transits with an adapted version of the CoRoT alarm pipeline. We present 172 planetary candidates and 327 eclipsing binary candidates from campaigns 1, 2, 3, 4, 5, and 6 of K2. Both the planetary candidates and eclipsing binary candidates lists are made public to promote follow-up studies. The light curves will also be available to the community.</description><source format="bibcode">2016A&amp;A...594A.100B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/594/A100</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/V/133">V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/728/117">J/ApJ/728/117 : Kepler planetary candidates. I. (Borucki+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/579/A19">J/A+A/579/A19 : K2 Variable Catalogue (Armstrong+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/452/3561">J/MNRAS/452/3561 : Kepler eclipsing binaries. 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