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<ri:Resource created="2011-11-02T12:13:43Z" 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>Column densities for HI, AlIII, SiIV, CIV, OVI</title><shortName>J/ApJ/702/1472</shortName><identifier>ivo://CDS.VizieR/J/ApJ/702/1472</identifier><altIdentifier>doi:10.26093/cds/vizier.17021472</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Savage B.D.</name></creator><creator><name>Wakker B.P.</name></creator><date role="Updated">2017-10-18T08:24:17Z</date><date role="Created">2011-11-02T12:13:43Z</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>ultraviolet-astronomy</subject><subject>interstellar-medium</subject><subject>milky-way-galaxy</subject><description>Column densities for HI, AlIII, SiIV, CIV, and OVI toward 109 stars and 30 extragalactic objects have been assembled to study the extensions of these species away from the Galactic plane into the Galactic halo. HI and AlIII mostly trace the warm neutral and warm ionized medium, respectively, while SiIV, CIV, and OVI trace a combination of warm photoionized and collisionally ionized plasmas. The much larger object sample compared to previous studies allows us to consider and correct for the effects of the sample bias that has affected earlier but smaller surveys of the gas distributions. The observations are compared to the predictions of the various models for the production of the transition temperature gas in the halo.</description><source format="bibcode">2009ApJ...702.1472S</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/702/1472</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/J/ApJS/176/59">J/ApJS/176/59 : FUSE survey of OVI in the disk of the Milky Way (Bowen+, 2008)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/647/312">J/ApJ/647/312 : FUSE survey of OVI in the Milky Way (Otte+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/125/2502">J/AJ/125/2502 : Spectral indices of Galactic halo (Morrison+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/146/1">J/ApJS/146/1 : O VI absorption in FUSE survey (Wakker+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/136/631">J/ApJS/136/631 : IUE absorption toward 164 early-type stars (Savage+, 2001)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/93/211">J/ApJS/93/211 : IUE survey of H I Ly{alpha} absorption. 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Logarithmic AlIII column density</description><unit>log(cm**-2)</unit><ucd>phys.columnDensity</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>u_lgN(Al3)</name><description>[:] Uncertainty flag on lgN(Al3)</description><ucd>meta.code.error</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>e_lgN(Al3)</name><description>? lgN(Al3) uncertainty</description><unit>log(cm**-2)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>l_lgN(Si4)</name><description>Limit flag on lgN(Si4)</description><ucd>meta.code.error</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>lgN(Si4)</name><description>? Logarithmic SiIV column density</description><unit>log(cm**-2)</unit><ucd>phys.columnDensity</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_lgN(Si4)</name><description>? lgN(Si4) uncertainty</description><unit>log(cm**-2)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>l_lgN(C4)</name><description>Limit flag on lgN(C4)</description><ucd>meta.code.error</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>lgN(C4)</name><description>? 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