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<ri:Resource created="2026-06-24T11:43:26Z" status="active" updated="2026-06-24T10:52:52Z" 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>Classifying intermediate-z galaxies in SDSS</title><shortName>J/ApJ/962/104</shortName><identifier>ivo://CDS.VizieR/J/ApJ/962/104</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Feuillet L.M.</name></creator><creator><name>Melendez M.</name></creator><creator><name>Kraemer S.</name></creator><creator><name>Schmitt H.R.</name></creator><creator><name>Fischer T.C.,Reeves J.N.</name></creator><date role="Updated">2026-06-24T10:52:52Z</date><date role="Created">2026-06-24T11:43:26Z</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>active-galactic-nuclei</subject><subject>visible-astronomy</subject><subject>spectroscopy</subject><subject>redshifted</subject><subject>seyfert-galaxies</subject><description>We select a sample of 1437 active galactic nuclei (AGN) from the catalog of the Sloan Digital Sky Survey galaxy properties from the Portsmouth group by detection of the high-ionization [NeV]3426{AA} emission line. We compare the fluxes of [NeIII]3869{AA}, [OIII]5007{AA}, [OII]3726,3728{AA}, and [OI]6300{AA} to that of [NeV]. All four lines show a strong linear correlation with [NeV], although lines from ions with lower ionization potentials have a lower correlation coefficient. We investigate the use of two forbidden line ratio diagnostic diagrams that do not rely on H{alpha} in order to classify high-redshift galaxies. These use the [NeIII]/[OII] line ratio plotted against [OIII]/[OI] and [OIII]/[OII], respectively. We use photoionization modeling to characterize the behavior of the narrow-line region in AGN and star-forming regions and test the validity of our diagnostic diagrams. We also use a luminosity cutoff of logL[OIII][erg/s]=42, which lowers the contamination of the AGN region by star-forming galaxies down to 10% but does not remove green pea and purple grape galaxies from the AGN region. We also investigate the OHNO diagram, which uses [NeIII]/[OII] plotted against [OIII]/H{beta}. Using our new diagnostic diagrams, we are able to reliably classify AGN up to a redshift of z&lt;=1.06 and add more than 822 new AGN to the [NeV]-selected AGN sample.</description><source format="bibcode">2024ApJ...962..104F</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/962/104</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/V/147">V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/154">V/154 : Sloan Digital Sky Surveys (SDSS), Release 16 (DR16) (Ahumada+, 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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>Type</name><description>Portsmouth group BPT classification (1)</description><ucd>src.class</ucd><dataType xsi:type="vs:VOTableType" arraysize="12*">char</dataType></column><column><name>z</name><description>[0.168/1.1] Galaxy spectroscopic redshift</description><ucd>src.redshift</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>RAJ2000</name><description>Right Ascension (J2000)</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd></column><column><name>DEJ2000</name><description>[-10.81/68.3] Declination (J2000)</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd></column><column><name>NeV</name><description>[0/7.8e+15] The [NeV] emission line flux (2)</description><unit>1e-19W.m**-2.nm**-1</unit><ucd>phot.flux;spect.line</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>NeIII</name><description>[0/5.7e+9] The [NeIII] emission line flux (2)</description><unit>1e-19W.m**-2.nm**-1</unit><ucd>phot.flux;spect.line</ucd><dataType xsi:type="vs:VOTableType">double</dataType></column><column><name>OI</name><description>[/1.71e+18]? 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