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We present Northern Extended Millimeter Array (NOEMA) CO(2-1) maps of thez=0.4418 cluster-central QSO IRAS 09104+4109, which trace ~4.5x10^10 Msol ofmolecular gas in and around the galaxy. As in many low redshift cool coreclusters, the molecular gas is located in a series of clumps extending alongthe old radio jets and lobes. It has a relatively low velocity dispersion (336[+39,-35] km/s FWHM) and shows no velocity gradients indicative of outflow orinfall. Roughly half the gas is located in a central clump on the northeastside of the galaxy, overlapping a bright ionized gas filament and a spur ofexcess X-ray emission, suggesting that this is a location of rapid cooling. Themolecular gas is unusually extended, out to ~55 kpc radius, comparable to thescale of the filamentary nebula in the Perseus cluster, despite the much higherredshift of this system. The extent falls within the thermal instability radiusof the intracluster medium (ICM), with t_cool/t_ff<25 and t_cool}/t_eddy~1within ~70 kpc. Continuum measurements at 159.9 GHz from NOEMA and 850 micronfrom the JCMT SCUBA-2 show excess far infrared emission, which we interpret asfree-free emission arising from the ongoing starburst. These observationssuggest that ICM cooling is not strongly affected by the buried QSO, and thatcooling from the ICM can build gas reservoirs sufficient to fuel quasar-modeactivity and drive the reorientation of the central AGN.

Molecular gas along the old radio jets of the cluster-central type 2 quasar IRAS 09104+4109