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<ri:Resource created="2024-04-18T11:50:52Z" status="active" updated="2025-06-19T20:10:35Z" 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>Rot. distributions from TESS-APOGEE-Kepler-Gaia</title><shortName>J/ApJ/930/7</shortName><identifier>ivo://CDS.VizieR/J/ApJ/930/7</identifier><altIdentifier>doi:10.26093/cds/vizier.19300007</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Avallone E.A.</name></creator><creator><name>Tayar J.N.</name></creator><creator><name>van Saders J.L.</name></creator><creator><name>Berger T.A.</name></creator><creator><name>Claytor Z.R.,Beaton R.L.</name></creator><creator><name>Teske J.</name></creator><creator><name>Godoy-Rivera D.</name></creator><creator><name>Pan K.</name></creator><date role="Updated">2025-06-19T20:10:35Z</date><date role="Created">2024-04-18T11:50:52Z</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>chemical-abundances</subject><subject>stellar-radii</subject><subject>stellar-masses</subject><subject>photometry</subject><subject>visible-astronomy</subject><subject>spectroscopic-binary-stars</subject><subject>infrared-sources</subject><description>Stellar rotation is a complex function of mass, metallicity, and age and can be altered by binarity. To understand the importance of these parameters in main-sequence stars, we have assembled a sample of observations that spans a range of these parameters using a combination of observations from The Transiting Exoplanet Survey Satellite (TESS) and the Kepler Space Telescope. We find that while we can measure rotation periods and identify other classes of stellar variability (e.g., pulsations) from TESS light curves, instrument systematics prevent the detection of rotation signals longer than the TESS orbital period of 13.7 days. Due to this detection limit, we also use rotation periods constrained using rotational velocities measured by the APOGEE spectroscopic survey and radii estimated using the Gaia mission for both TESS and Kepler stars. From these rotation periods, we (1) find we can track rotational evolution along discrete mass tracks as a function of stellar age, (2) find we are unable to recover trends between rotation and metallicity that were observed by previous studies, and (3) note that our sample reveals that wide binary companions do not affect rotation, while close binary companions cause stars to exhibit more rapid rotation than single stars.</description><source format="bibcode">2022ApJ...930....7A</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/930/7</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/II/246">II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/133">V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/IV/38">IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/III/284">III/284 : APOGEE-2 data from DR16 (Johnsson+, 2020)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/154">V/154 : Sloan Digital Sky Surveys (SDSS), Release 16 (DR16) (Ahumada+, 2020)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/IV/39">IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/355">I/355 : Gaia DR3 Part 1. 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Lower uncertainty in Mass</description><unit>solMass</unit><ucd>stat.error;stat.min;phys.mass</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Class</name><description>Classification flag (2)</description><ucd>meta.code.class;src.class</ucd><dataType xsi:type="vs:VOTableType" arraysize="22*">char</dataType></column><column><name>PRot</name><description>Display the rotation periods for our TESS sample (link to Table 2)</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>MQ14</name><description>Display data from McQuillan+ 2014, J/ApJS/211/24</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>APOGEE</name><description>Display data from APOGEE DR16 (III/284)</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>_RA</name><description>Right Ascension (J2000) from SIMBAD (not part of the original data)</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd></column><column><name>_DE</name><description>Declination (J2000) from SIMBAD (not part of the original data)</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd></column></table><table><name>J/ApJ/930/7/table2</name><description>Rotation periods for our TESS sample</description><column><name>ID</name><description>[25080230/391903064] TIC identifier</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType">long</dataType></column><column><name>recno</name><description>Record number assigned by the VizieR team. Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Seq</name><description>[0/168] Internal index number</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>Bin</name><description>Binary flag ("Single Star": 166 sources vs "Spectroscopic Binary": 3 occurrences)</description><ucd>meta.code.class</ucd><dataType xsi:type="vs:VOTableType" arraysize="20*">char</dataType></column><column><name>PLS</name><description>[0.4/12.2] Period from Lomb-Scargle periodogram</description><unit>d</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_PLS</name><description>[0/1.3] Uncertainty in PLS</description><unit>d</unit><ucd>stat.error;time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>PWave</name><description>[0.8/11.7] Period from Wavelet analysis</description><unit>d</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_PWave</name><description>[0.09/6.3] Uncertainty in Pwave</description><unit>d</unit><ucd>stat.error;time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>PAcf</name><description>[0.8/19.5] Period from autocorrelation function analysis</description><unit>d</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_PAcf</name><description>[0.09/7.6] Uncertainty in Pacf</description><unit>d</unit><ucd>stat.error;time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>PRot</name><description>[0.9/10.5] Mean photometric rotational period (1)</description><unit>d</unit><ucd>time.period;stat.mean</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_PRot</name><description>[0.1/0.8] Uncertainty in PRot</description><unit>d</unit><ucd>stat.error;time.period;stat.mean</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>PRotc</name><description>[1/44.2]? Rotational period divided by sini (1)</description><unit>d</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>E_PRotc</name><description>[0.06/71]? Upper uncertainty in PRotc</description><unit>d</unit><ucd>stat.error;stat.max;time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_PRotc</name><description>[0.06/27.1]? Lower uncertainty in PRotc</description><unit>d</unit><ucd>stat.error;stat.min;time.period</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Mission</name><description>Mission identifier (always "TESS")</description><ucd>meta.id;instr.obsty</ucd><dataType xsi:type="vs:VOTableType" arraysize="4*">char</dataType></column></table></schema></tableset></ri:Resource>