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We present results of a comprehensive multi-frequency study of the radiogalaxy B3 J2330+3927. The 1.9" wide radio source, consisting of 3 components,is bracketed by 2 objects in our Keck K-band image. Optical and near-IR Keckspectroscopy of these two objects yield z=3.087+-0.004. The brightest (K=18.8)object has a standard type II AGN spectrum, and is the most likely location ofthe AGN, which implies a one-sided jet radio morphology. Deep 113 GHzobservations with the IRAM Plateau de Bure Interferometer reveal CO J=4-3emission, which peaks at the position of the AGN. The CO line is offset by 500km/s from the systemic redshift of the AGN, but corresponds very closely to thevelocity shift of an associated HI absorber seen in Lya. This strongly suggeststhat both originate from the same gas reservoir surrounding the AGN hostgalaxy. Simultaneous 230 GHz interferometer observations find a ~3x lowerintegrated flux density when compared to single dish 250 GHz observations withMAMBO at the IRAM 30m telescope. This can be interpreted as spatially resolvedthermal dust emission at scales of 0.5" to 6". Finally, we present a tau <1.3%limit to the HI 21 cm absorption against the radio source, which represents theseventh non-detection out of 8 z>2 radio galaxies observed to date with theWSRT. We present mass estimates for the atomic, neutral, and ionized hydrogen,and for the dust, ranging from M(HI)=2x10^7 M_Sun derived from the associatedHI absorber in Lya up to M(H_2)=7x10^{10} M_Sun derived from the CO emission.This indicates that the host galaxy is surrounded by a massive reservoir of gasand dust. The K-band companion objects may be concentrations within thisreservoir, which will eventually merge with the central galaxy hosting the AGN.Comment: 16 Pages, including 11 PostScript figures. Accepted for publication  in Astronomy & Astrophysic

CO emission and associated H I absorption from a massive gas reservoir surrounding thez= 3 radio galaxy B3 J2330+3927