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<ri:Resource created="2020-03-26T08:07:26Z" 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>M dwarfs at high spectral-resolution in Y band</title><shortName>J/AJ/159/52</shortName><identifier>ivo://CDS.VizieR/J/AJ/159/52</identifier><altIdentifier>doi:10.26093/cds/vizier.51590052</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Muirhead P.S.</name></creator><creator><name>Veyette M.J.</name></creator><creator><name>Newton E.R.</name></creator><creator><name>Theissen C.A.</name></creator><creator><name>Mann A.W.</name></creator><date role="Updated">2020-09-16T12:20:12Z</date><date role="Created">2020-03-26T08:07:26Z</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>infrared-astronomy</subject><subject>spectroscopy</subject><subject>line-intensities</subject><subject>stellar-masses</subject><subject>dwarf-stars</subject><subject>m-stars</subject><subject>proper-motions</subject><subject>stellar-spectral-types</subject><description>In young Sun-like stars and field M-dwarf stars, chromospheric and coronal magnetic activity indicators such as H{alpha}, X-ray, and radio emission are known to saturate with low Rossby number (Ro&lt;~0.1), defined as the ratio of rotation period to convective turnover time. The mechanism for the saturation is unclear. In this paper, we use photospheric TiI and CaI absorption lines in the Y band to investigate magnetic field strength in M dwarfs for Rossby numbers between 0.01 and 1.0. The equivalent widths of the lines are magnetically enhanced by photospheric spots, a global field, or a combination of the two. The equivalent widths behave qualitatively similar to the chromospheric and coronal indicators: we see increasing equivalent widths (increasing absorption) with decreasing Ro and saturation of the equivalent widths for Ro&lt;~0.1. The majority of M dwarfs in this study are fully convective. The results add to mounting evidence that the magnetic saturation mechanism occurs at or beneath the stellar photosphere.</description><source format="bibcode">2020AJ....159...52M</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/159/52</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/I/345">I/345 : Gaia DR2 (Gaia Collaboration, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/85/315">J/ApJS/85/315 : F, G and K dwarf stars of the Pleiades (Soderblom+ 1993)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/397/147">J/A+A/397/147 : Activity-rotation relationship in stars (Pizzolato+ 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/648/629">J/ApJ/648/629 : Radio observations of late M, L, and T dwarfs (Berger+,2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/743/48">J/ApJ/743/48 : Stars rotat. periods &amp; X-ray luminosities (Wright+,2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/754/44">J/ApJ/754/44 : The AstraLux Large M-dwarf Survey (Janson+ 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/784/156">J/ApJ/784/156 : Parallaxes for nearby mid-to-late M dwarfs (Dittmann+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/791/54">J/ApJ/791/54 : Nearby M Dwarfs parameters (Gaidos+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/795/161">J/ApJ/795/161 : Activity &amp; rotation in Praesepe &amp; the Hyades (Douglas+,2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/804/64">J/ApJ/804/64 : Empirical and model parameters of 183 M dwarfs (Mann+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/800/85">J/ApJ/800/85 : Teff, radii and luminosities of cool dwarfs (Newton+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/818/153">J/ApJ/818/153 : MEarth photometry: nearby M-dwarf mag (Dittmann+,2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/463/1844">J/MNRAS/463/1844 : M dwarfs rotation-activity relation (Stelzer+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/836/124">J/ApJ/836/124 : 2yrs of eclipse data &amp; RVs for LP661-13 (Dittmann+,2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/834/85">J/ApJ/834/85 : H{alpha} emission in nearby M dwarfs (Newton+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/851/26">J/ApJ/851/26 : Teff, metallicity &amp; Ti abundance of M dwarfs (Veyette+,2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/155/225">J/AJ/155/225 : M dwarf stars rotational broadening measure. 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