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<ri:Resource created="2026-01-16T09:47:25Z" status="active" updated="2026-03-02T06:25:50Z" 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>Physical properties study of planet systems</title><shortName>J/A+A/705/A142</shortName><identifier>ivo://CDS.VizieR/J/A+A/705/A142</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Rossi A.M</name></creator><creator><name>Rainer M.</name></creator><creator><name>Borsa F.</name></creator><creator><name>Facchini S.</name></creator><date role="Updated">2026-03-02T06:25:50Z</date><date role="Created">2026-01-16T09:47:25Z</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>multiple-stars</subject><subject>exoplanets</subject><subject>orbits</subject><subject>effective-temperature</subject><subject>radial-velocity</subject><subject>stellar-ages</subject><description>True spin-orbit obliquities offer valuable insights into the evolutionary history of exoplanetary systems. Previous studies have suggested that exoplanets tend to occupy either aligned or perpendicular orbits. However, recent research has indicated potential biases caused by the small sample, questioning whether this dichotomy would persist with a larger dataset. Simultaneously, a similar dichotomous behavior has been suggested for Neptune-sized planets. We aim to investigate the distribution of true spin-orbit obliquities with an enlarged sample, looking for confirmation of the disputed dichotomy previously found, with a focus also on the obliquities of Neptunes. Starting from a sample of 264 projected obliquities, we homogeneously compute true obliquities for 116 planets using the rotation period method. We combine them with 4 further values gathered from literature and we then study their distribution, also as a function of various star-planet system parameters. Our data-driven work based on 120 true obliquities - the largest sample to date - strongly confirms the presence of a single cluster of aligned planets, followed by an isotropic distribution of misaligned planets with no preferred misalignment. This result is based on a uniform distribution of stellar inclinations, for which non-uniformity could have biased previous interpretations of the arrangement of true obliquities. We confirm that Neptunians show a tentative dichotomous distribution with data available today, but its veracity needs confirmation with an enlarged sample, also because an anisotropic distribution of stellar inclination may be one of the factors hindering the real distribution. The future increase of the measured true obliquity sample over different planet types will allow better investigation of the relation between misalignment and system properties and help to depict a more comprehensive picture of the planetary evolution processes.</description><source format="bibcode">2026A&amp;A...705A.142R</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/705/A142</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/A+A/690/A379">J/A+A/690/A379 : Obliquities of exoplanet host stars (Knudstrup+, 2024)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/666/A47">J/A+A/666/A47 : MASCARA-4 b light and RV curves (Zhang+, 2022)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/658/A75">J/A+A/658/A75 : MASCARA-1 b occultation and transit light curves</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/650/A66">J/A+A/650/A66 : DS Tuc A radial velocity curve (Benatti+, 2021)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/635/A73">J/A+A/635/A73 : Multiplicity study of transiting exoplanet hosts. 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Upper error on planet mass</description><unit>(5.97236x10+24kg)</unit><ucd>stat.error;stat.max</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_Mpl</name><description>? Lower error on planet mass</description><unit>(5.97236x10+24kg)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>f_Mpl</name><description>[0/1] Mpl flag (0 = known value, 1 = upper limit)</description><ucd>meta.code</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>r_Mpl</name><description>Planet mass reference</description><ucd>meta.ref;pos.frame</ucd><dataType xsi:type="vs:VOTableType" arraysize="19*">char</dataType></column><column><name>lambda</name><description>? 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