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<ri:Resource created="2007-11-25T14:36:56Z" 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>A search for pre-biotic molecules</title><shortName>J/A+A/473/177</shortName><identifier>ivo://CDS.VizieR/J/A+A/473/177</identifier><altIdentifier>doi:10.26093/cds/vizier.34730177</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Wirstrom E.S.</name></creator><creator><name>Bergman P.</name></creator><creator><name>Hjalmarson A.</name></creator><creator><name>Nummelin A.</name></creator><date role="Updated">2017-10-10T07:10:01Z</date><date role="Created">2007-11-25T14:36:56Z</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>interstellar-medium</subject><subject>radio-astronomy</subject><subject>molecular-clouds</subject><description>Low-noise, 0.8MHz resolution spectra around 90GHz towards four hot core sources: Orion KL, W51 e1/e2, S140, and W3(OH), are presented. The observations were performed using the 3mm SIS receiver at the Onsala 20m telescope. The observations were made in the beam-switching mode, the spectrum intensity is given in T_A_^*^ and high-order polynomial baselines have been subtracted. At 90GHz the Onsala 20m telescope has a beam FWHM of ~42arcsec and a main-beam efficiency of ~0.6. Due to changes in frequency setting during the observing period the frequency ranges are not identical for each source, but in all cases the ranges include the transitions used to determine the upper column densities of amino acetonitrile (H_2_NCH_2_CN), vinyl acetylene (C_2_H_3_CCH), oxiranecarbonitrile (c-C_3_H_3_NO), and amino-ethanol (NH_2_CH_2_CH_2_OH), presented in the paper. 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