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<ri:Resource created="2014-03-17T08:22:01Z" 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>IRAM 30m reduced spectra of 59 sources</title><shortName>J/A+A/563/A97</shortName><identifier>ivo://CDS.VizieR/J/A+A/563/A97</identifier><altIdentifier>doi:10.26093/cds/vizier.35630097</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Gerner T.</name></creator><creator><name>Beuther H.</name></creator><creator><name>Semenov D.</name></creator><creator><name>Linz H.</name></creator><creator><name>Vasyunina T.</name></creator><creator><name>Bihr S.,Shirley Y.L.</name></creator><creator><name>Henning T.</name></creator><date role="Updated">2015-10-06T13:20:58Z</date><date role="Created">2014-03-17T08:22:01Z</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>molecular-clouds</subject><subject>spectroscopy</subject><description>Understanding the chemical evolution of young (high-mass) star-forming regions is a central topic in star formation research. Chemistry is employed as a unique tool 1) to investigate the underlying physical processes and 2) to characterize the evolution of the chemical composition. With these aims in mind, we observed a sample of 59 high-mass star-forming regions at different evolutionary stages varying from the early starless phase of infrared dark clouds to high-mass protostellar objects to hot molecular cores and, finally, ultra-compact HII regions at 1mm and 3mm with the IRAM 30m telescope. 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