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<ri:Resource created="2020-01-31T15:18:22Z" 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>MgII-BAL quasar variability in SDSS spectra</title><shortName>J/ApJS/242/28</shortName><identifier>ivo://CDS.VizieR/J/ApJS/242/28</identifier><altIdentifier>doi:10.26093/cds/vizier.22420028</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Yi W.</name></creator><creator><name>Brandt W.N.</name></creator><creator><name>Hall P.B.</name></creator><creator><name>Vivek M.</name></creator><creator><name>Grier C.J.</name></creator><creator><name>Ak N.F.,Schneider D.P.</name></creator><creator><name>McGraw S.M.</name></creator><date role="Updated">2020-04-20T13:45:10Z</date><date role="Created">2020-01-31T15:18:22Z</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>quasars</subject><subject>visible-astronomy</subject><subject>spectroscopy</subject><subject>redshifted</subject><subject>line-intensities</subject><description>We present absorption variability results for 134 bona fide MgII broad absorption-line (BAL) quasars at 0.46&lt;=z&lt;=2.3 covering days to ~10yr in the rest frame. We use multiple-epoch spectra from the Sloan Digital Sky Survey, which has delivered the largest such BAL variability sample ever studied. MgII-BAL identifications and related measurements are compiled and presented in a catalog. We find a remarkable time-dependent asymmetry in the equivalent width (EW) variation from the sample, such that weakening troughs outnumber strengthening troughs, the first report of such a phenomenon in BAL variability. Our investigations of the sample further reveal that (i) the frequency of BAL variability is significantly lower (typically by a factor of 2) than that in high-ionization BALQSO samples, (ii) MgII-BAL absorbers tend to have relatively high optical depths and small covering factors along our line of sight, (iii) there is no significant EW-variability correlation between MgII troughs at different velocities in the same quasar, and (iv) the EW-variability correlation between MgII and AlIII BALs is significantly stronger than that between MgII and CIV BALs at the same velocities. These observational results can be explained by a combined transverse-motion/ionization-change scenario, where transverse motions likely dominate the strengthening BALs while ionization changes and/or other mechanisms dominate the weakening BALs.</description><source format="bibcode">2019ApJS..242...28Y</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/242/28</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/VII/260">VII/260 : The SDSS-DR7 quasar catalog (Schneider+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/VII/279">VII/279 : SDSS quasar catalog: twelfth data release (Paris+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/106/848">J/AJ/106/848 : QSO MgII absorption line systems (Drinkwater+, 1993)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/165/1">J/ApJS/165/1 : BAL QSOs from SDSS DR3 (Trump+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/692/758">J/ApJ/692/758 : BAL QSOs in SDSS-DR5 (Gibson+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/405/2302">J/MNRAS/405/2302 : Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/194/45">J/ApJS/194/45 : QSO properties from SDSS-DR7 (Shen+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/748/131">J/ApJ/748/131 : MgII absorbers in SDSS-DR7 quasar catalog (Shen+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/777/168">J/ApJ/777/168 : CIV and SiIV BAL troughs in SDSS (Filiz+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/779/161">J/ApJ/779/161 : MgII absorbers in 0.4&lt;z&lt;2.3 SDSS QSOs (Seyffert+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/791/88">J/ApJ/791/88 : C IV BAL troughs properties in quasars (Filiz+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/440/799">J/MNRAS/440/799 : Low Ionization BALQSOs MgII &amp; AlIII var. (Vivek+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/814/150">J/ApJ/814/150 : Variability of SDSS broad absorption line QSOs (Wang+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/824/130">J/ApJ/824/130 : SDSS/BOSS/TDSS CIV BAL quasars (Grier+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/831/7">J/ApJ/831/7 : SDSS-RM project: peak velocities of QSOs (Shen+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/463/2640">J/MNRAS/463/2640 : SDSS-DR12 QSOs MgII absorption systems (Raghunathan+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/235/11">J/ApJS/235/11 : Absorption features in SDSS. I. 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