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<ri:Resource created="2025-09-24T14:04:01Z" status="active" updated="2026-08-03T06:57:26Z" 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>[CI] and CO lines across cosmic time</title><shortName>J/A+A/701/A288</shortName><identifier>ivo://CDS.VizieR/J/A+A/701/A288</identifier><altIdentifier>doi:10.26093/cds/vizier/bc-nx/lcii</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Topkaras T.</name></creator><creator><name>Bisbas T.G.</name></creator><creator><name>Zhang Z.-Y.</name></creator><creator><name>Ossenkopf-Okada V.</name></creator><date role="Updated">2026-08-03T06:57:26Z</date><date role="Created">2025-09-24T14:04:01Z</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>galaxies</subject><subject>infrared-sources</subject><subject>interstellar-medium</subject><subject>co-line-emission</subject><description>Cold molecular gas tracers, such as CI and CO lines, have been widely used to infer specific characteristics of the ISM and to derive star-formation relations among galaxies. However, there is still a lack of systematic studies of the star-formation scaling relation of CO and [CI] lines across cosmic time on multiple physical scales. We used observations of the ground state transitions of [CI], CO, and [CII], for 885 sources collected from the literature, to infer possible correlations between line luminosities of L' [CI](1-0), L'CO(1-0), and L'[CII] with star formation rates (SFR). With linear regression, we fit the relations between SFR and molecular mass derived from CO, CI, and CII lines. The relation between [CI] and CO based total molecular masses is weakly super linear. Nevertheless, they can be calibrated against each other. For {alpha}CO=0.8 and 4.0M_{sun}_/(K.(km/s).pc^2^) we derive {alpha}[CI]=3.9 and ~17M_{sun}_/(K.(km/s).pc^2^) , respectively. Using the lmfit package, we derived relation slopes of SFR-L'[CI](1-0), SFR-L'CO(1-0), and SFR-L'[CII](1-0) to be {beta}=1.06+/-0.02, 1.24+/-0.02, and 0.74+/-0.02, respectively. With a Bayesian-inference linmix method, we find consistent results. Our relations for [CI](1-0) and CO(1-0) indicate that they trace similar molecular gas contents, across different redshifts and different types of galaxies. 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