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<ri:Resource created="2015-10-08T11:02:54Z" 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>W51/e2 and G34.3+0.2 IRAM spectra</title><shortName>J/A+A/582/A64</shortName><identifier>ivo://CDS.VizieR/J/A+A/582/A64</identifier><altIdentifier>doi:10.26093/cds/vizier.35820064</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Lykke J.M.</name></creator><creator><name>Favre C.</name></creator><creator><name>Bergin E.A.</name></creator><creator><name>Jorgensen J.K.</name></creator><date role="Updated">2015-10-08T12:06:19Z</date><date role="Created">2015-10-08T11:02:54Z</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>stellar-associations</subject><subject>spectroscopy</subject><description>With only a few low- and high-mass star-formation regions studied in detail so far, it is unclear what role the environment plays in complex molecule formation. In this light, a comparison of relative abundances of related species between sources might be useful for explaining any observed differences. We seek to measure the relative abundance between three important complex organic molecules, ethylene glycol ((CH_2_OH)_2_), glycolaldehyde (CH_2_OHCHO) and methyl formate (HCOOCH_3_), toward high-mass protostars and thereby provide additional constraints on their formation pathways. 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