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<ri:Resource created="2019-08-30T07:32:17Z" status="active" updated="2025-06-13T15:25:00Z" 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>ALMA CO observations of the system 4C12.50</title><shortName>J/A+A/629/A30</shortName><identifier>ivo://CDS.VizieR/J/A+A/629/A30</identifier><altIdentifier>doi:10.26093/cds/vizier.36290030</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Fotopoulou C.M.</name></creator><creator><name>Dasyra K.M.</name></creator><creator><name>Combes F.</name></creator><creator><name>Salome P.</name></creator><creator><name>Papachristou M.</name></creator><date role="Updated">2019-09-02T08:14:55Z</date><date role="Created">2019-08-30T07:32:17Z</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>radio-galaxies</subject><subject>interstellar-medium</subject><subject>co-line-emission</subject><description>The nearby system 4C12.50, also known as IRAS 13451+1217 and PKS 1345+12, is a merger of gas-rich galaxies with infrared and radio activity. It has a perturbed interstellar medium (ISM) and a dense configuration of gas and dust around the nucleus. The radio emission at small (~100pc) and large (~100kpc) scales, as well as the large X-ray cavity in which the system is embedded, are indicative of a jet that could have affected the ISM. We carried out observations of the CO(1-0), (3-2), and (4-3) lines with the Atacama Large Millimeter Array (ALMA) to determine basic properties (i.e., extent, mass, and excitation) of the cold molecular gas in this system, including its already-known wind. The CO emission reveals the presence of gaseous streams related to the merger, which result in a small (4kpc-wide) disk around the western nucleus. The disk reaches a rotational velocity of 200km/s, and has a mass of 3.8(+/-0.4)10^9^M_{sun}_. It is truncated at a gaseous ridge north of the nucleus that is bright in [OIII]. Regions with high-velocity CO emission are seen at signal-to-noise ratios of between 3 and 5 along filaments that radially extend from the nucleus to the ridge and that are bright in [O iii] and stellar emission. A tentative wind detection is also reported in the nucleus and in the disk. The molecular gas speed could be as high as 2200km/s and the total wind mass could be as high as 1.5(+/-0.1)10^9^M_{sun}_. 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