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<ri:Resource created="2013-05-22T08:47:08Z" 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>LAEs between 0.19&lt;z&lt;1.25 with GALEX grism</title><shortName>J/ApJ/738/136</shortName><identifier>ivo://CDS.VizieR/J/ApJ/738/136</identifier><altIdentifier>doi:10.26093/cds/vizier.17380136</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Cowie L.L.</name></creator><creator><name>Barger A.J.</name></creator><creator><name>Hu E.M.</name></creator><date role="Updated">2017-07-03T14:25:32Z</date><date role="Created">2013-05-22T08:47:08Z</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>line-intensities</subject><subject>galaxies</subject><subject>spectroscopy</subject><subject>redshifted</subject><subject>ultraviolet-astronomy</subject><description>We present optical spectroscopy of two samples of Galaxy Evolution Explorer grism selected Ly{alpha} emitters (LAEs): one at z=0.195-0.44 and the other at z=0.65-1.25. We have also observed a comparison sample of galaxies in the same redshift intervals with the same UV magnitude distributions but with no detected Ly{alpha}. We use the optical spectroscopy to eliminate active galactic nuclei and to obtain the optical emission-line properties of the samples. We compare the luminosities of the LAEs in the two redshift intervals and show that there is dramatic evolution in the maximum Ly{alpha} luminosity over z=0-1. Focusing on the z=0.195-0.44 samples alone, we show that there are tightly defined relations between all of the galaxy parameters and the rest-frame equivalent width (EW) of H{alpha}. The higher EW(H{alpha}) sources all have lower metallicities, bluer colors, smaller sizes, and less extinction, consistent with their being in the early stages of the galaxy formation process.</description><source format="bibcode">2011ApJ...738..136C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/738/136</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/ApJ/711/928">J/ApJ/711/928 : Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/512/A12">J/A+A/512/A12 : VLT/VIMOS spectroscopy in GOODS-South field (Balestra+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/478/83">J/A+A/478/83 : GOODS-South Field VLT/FORS2 redshifts. 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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>S</name><description>Simbad column added by the CDS</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>m_GALEX</name><description>[abc] Multiplicity index (G1)</description><ucd>meta.code.multip</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>G</name><description>Correspondance with GALEX spectral sample identifications (table4)</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>RAJ2000</name><description>Right ascension in decimal degrees (J2000)</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd></column><column><name>DEJ2000</name><description>Declination in decimal degrees (J2000)</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd></column><column><name>z</name><description>GALEX redshift</description><ucd>src.redshift</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>logLnu</name><description>Log of the bolometric continuum luminosity, above 1216{AA}</description><unit>log(1e-07W)</unit><ucd>phys.luminosity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>logLa</name><description>Log of the Ly{alpha} luminosity</description><unit>log(1e-07W)</unit><ucd>phys.luminosity;em.UV</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>EWLya</name><description>Rest-frame equivalent width(Ly{alpha}) in {AA}</description><unit>0.1nm</unit><ucd>spect.line.eqWidth</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>e_EWLya</name><description>EWLya uncertainty</description><unit>0.1nm</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>zOpt</name><description>? 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