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<ri:Resource created="2021-04-07T10:47:01Z" 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>Spiral structure in the gas disc of CQ Tau</title><shortName>J/A+A/648/A19</shortName><identifier>ivo://CDS.VizieR/J/A+A/648/A19</identifier><altIdentifier>doi:10.26093/cds/vizier.36480019</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Woelfer L.</name></creator><creator><name>Facchini S.</name></creator><creator><name>Kurtovic N.T.</name></creator><creator><name>Teague R.</name></creator><creator><name>van Dishoeck E.F.,Benisty M.</name></creator><creator><name>Ercolano B.</name></creator><creator><name>Lodato G.</name></creator><creator><name>Miotello A.</name></creator><creator><name>Rosotti G.</name></creator><creator><name>Testi L.,Ubeira Gabellini M.G.</name></creator><date role="Updated">2021-07-05T08:59:42Z</date><date role="Created">2021-04-07T10:47:01Z</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>young-stellar-objects</subject><subject>millimeter-astronomy</subject><subject>submillimeter-astronomy</subject><subject>co-line-emission</subject><description>We used spatially resolved ALMA observations of the three CO isotopologues ^12^CO, ^13^CO and C^18^O (J=2-1) from CQ Tau to analyse the brightness temperature and kinematics of the gas disc. We detect significant spiral structures in both the brightness temperature and the rotation velocity of ^12^CO after subtraction of an azimuthally symmetric model, which may be tracing planet-disc interactions with an embedded planet or low-mass companion. The brightness temperature spirals are morphologically connected to spirals observed in NIR scattered light in the same disc, indicating a common origin. 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