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<ri:Resource created="2019-10-11T07:04:08Z" 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>List of new asteroid models</title><shortName>J/A+A/631/A2</shortName><identifier>ivo://CDS.VizieR/J/A+A/631/A2</identifier><altIdentifier>doi:10.26093/cds/vizier.36310002</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Durech J.</name></creator><creator><name>Hanus J.</name></creator><creator><name>Vanco R.</name></creator><date role="Updated">2020-04-08T10:43:50Z</date><date role="Created">2019-10-11T07:04:08Z</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>photometry</subject><subject>asteroids</subject><description>Rotation properties (spin-axis direction and rotation period) and coarse shape models of asteroids can be reconstructed from their disk-integrated brightness when measured from various viewing geometries. These physical properties are essential for creating a global picture of structure and dynamical evolution of the main belt. The number of shape and spin models can be increased not only when new data are available, but also by combining independent data sets and inverting them together. Our aim was to derive new asteroid models by processing readily available photometry. We used asteroid photometry compiled in the Lowell Observatory photometry database with photometry from the Gaia Data Release 2. Both data sources are available for about 5400 asteroids. In the framework of the Asteroids@home distributed computing project, we applied the light curve inversion method to each asteroid to find its convex shape model and spin state that fits the observed photometry. Due to the limited number of Gaia DR2 data points and poor photometric accuracy of Lowell data, we were able to derive unique models for only ~1100 asteroids. Nevertheless, 762 of these are new models that significantly enlarge the current database of about 1600 asteroid models. Our results demonstrate the importance of a combined approach to inversion of asteroid photometry. While our models in general agree with those obtained by separate inversion of Lowell and Gaia data, the combined inversion is more robust, model parameters are more constrained, and unique models can be reconstructed in many cases when individual data sets alone are not sufficient.</description><source format="bibcode">2019A&amp;A...631A...2D</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/631/A2</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></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Number</name><description>Asteroid number</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Name</name><description>Asteroid name or designation</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="20*">char</dataType></column><column><name>ELON1</name><description>Ecliptic pole longitude (J2000.0) for model 1, lambda1</description><unit>deg</unit><ucd>pos.ecliptic.lon</ucd></column><column><name>ELAT1</name><description>Ecliptic pole latitude (J2000.0) for model 1, beta1</description><unit>deg</unit><ucd>pos.ecliptic.lat</ucd></column><column><name>ELON2</name><description>[0/360]? Ecliptic pole longitude (J2000.0) for model 2, lambda2</description><unit>deg</unit><ucd>pos.ecliptic.lon</ucd><flag>nullable</flag></column><column><name>ELAT2</name><description>? Ecliptic pole latitude (J2000.0) for model 2, beta2</description><unit>deg</unit><ucd>pos.ecliptic.lat</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>P</name><description>Sidereal period of rotation</description><unit>h</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>l_PLCDB</name><description>Limit flag on PLCDB</description><ucd>meta.code.error</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>PLCDB</name><description>? 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Note according to LCDB</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>NL</name><description>Number of Lowell photometric points</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>NG</name><description>Number of Gaia photometric points</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Method</name><description>Method used for period determination (1)</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType" arraysize="2*">char</dataType></column><column><name>_RA.icrs</name><description>Right ascension (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)</description><unit>deg</unit><ucd>pos.eq.ra</ucd><flag>nullable</flag><flag>indexed</flag></column><column><name>_DE.icrs</name><description>Declination (ICRS) (computed by VizieR, not part of the original data. The format may include more digits than the original data because of internal accuracy requirements in VizieR and across other CDS services)</description><unit>deg</unit><ucd>pos.eq.dec</ucd><flag>nullable</flag><flag>indexed</flag></column></table></schema></tableset></ri:Resource>