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<ri:Resource created="2016-02-10T13:06:44Z" 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>MEarth mid-to-late M dwarfs rotation &amp; kinematics</title><shortName>J/ApJ/812/3</shortName><identifier>ivo://CDS.VizieR/J/ApJ/812/3</identifier><altIdentifier>doi:10.26093/cds/vizier.18120003</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>West A.A.</name></creator><creator><name>Weisenburger K.L.</name></creator><creator><name>Irwin J.</name></creator><creator><name>Berta-Thompson Z.K.,Charbonneau D.</name></creator><creator><name>Dittmann J.</name></creator><creator><name>Pineda J.S.</name></creator><date role="Updated">2017-09-27T05:55:57Z</date><date role="Created">2016-02-10T13:06:44Z</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>proper-motions</subject><subject>radial-velocity</subject><subject>stellar-distance</subject><subject>line-intensities</subject><subject>m-stars</subject><description>Using spectroscopic observations and photometric light curves of 238 nearby M dwarfs from the MEarth exoplanet transit survey, we examine the relationships between magnetic activity (quantified by H{alpha} emission), rotation period, and stellar age. Previous attempts to investigate the relationship between magnetic activity and rotation in these stars were hampered by the limited number of M dwarfs with measured rotation periods (and the fact that v sin i measurements probe only rapid rotation). However, the photometric data from MEarth allows us to probe a wide range of rotation periods for hundreds of M dwarf stars (from shorter than one to longer than 100 days). Over all M spectral types that we probe, we find that the presence of magnetic activity is tied to rotation, including for late-type, fully convective M dwarfs. We also find evidence that the fraction of late-type M dwarfs that are active may be higher at longer rotation periods compared to their early-type counterparts, with several active, late-type, slowly rotating stars present in our sample. Additionally, we find that all M dwarfs with rotation periods shorter than 26 days (early-type; M1-M4) and 86 days (late-type; M5-M8) are magnetically active. This potential mismatch suggests that the physical mechanisms that connect stellar rotation to chromospheric heating may be different in fully convective stars. A kinematic analysis suggests that the magnetically active, rapidly rotating stars are consistent with a kinematically young population, while slow-rotators are less active or inactive and appear to belong to an older, dynamically heated stellar population.</description><source format="bibcode">2015ApJ...812....3W</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/812/3</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/I/298">I/298 : LSPM-North Catalog (Lepine+ 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/III/198">III/198 : Palomar/MSU 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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>LSPM</name><description>M Dwarf identifier (JHHMM+DDMMW)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="11*">char</dataType></column><column><name>RAJ2000</name><description>[0/23] Hour of Right Ascension (J2000)</description><ucd>pos.eq.ra;meta.main</ucd></column><column><name>DEJ2000</name><description>[0/83] Degree of Declination (J2000)</description><ucd>pos.eq.dec;meta.main</ucd></column><column><name>Dist</name><description>[5.4/65]? 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The W velocity perpendicular to the plane (3)</description><unit>km/s</unit><ucd>phys.veloc;pos.cartesian.z</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_W</name><description>? Uncertainty in W</description><unit>km/s</unit><ucd>stat.error;pos.cartesian.z</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Per</name><description>[0.16/154.2]? Rotation period</description><unit>d</unit><ucd>time.period</ucd><dataType xsi:type="vs:VOTableType">double</dataType><flag>nullable</flag></column><column><name>Amp</name><description>[0.002/0.05]? Rotation semi-amplitude</description><unit>mag</unit><ucd>src.var.amplitude</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>Season</name><description>Rotation season</description><unit>yr</unit><ucd>phys</ucd><dataType xsi:type="vs:VOTableType" arraysize="9*">char</dataType></column><column><name>HaEW</name><description>[0.7/29]? H{alpha} equivalent width; Angstroms (4)</description><unit>0.1nm</unit><ucd>spect.line.eqWidth;em.line.Halpha</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_HaEW</name><description>[0.2/6.3]? 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