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We report the detection of the CO J=1-0 emission line in [H89]1821+643, oneof the most optically luminous QSOs in the local Universe and a templateULIRG-to-QSO transition object, located in a rich cool-core cluster at z=0.297.The CO emission is likely to be extended, highly asymmetric with respect to thecenter of the host elliptical where the QSO resides, and corresponds to amolecular gas mass of ~ 8.0 x 10^{9} M_sun. The dynamical mass enclosed by theCO line emission region could amount up to ~ 1.7x10^{12} M_sun (80% of thetotal mass of the elliptical host). The bulk of the CO emission is located at~9 kpc south-east from the nuclei position, and close to a faint opticalstructure, suggesting that the CO emission could either represent a gas-richcompanion galaxy merging with the elliptical host or a tail-like structurereminiscent of a previous interaction. We argue that the first scenario is morelikely given the large masses implied for the CO source, which would imply ahighly asymmetrical elliptical host. The close alignment between the COemission major axis and the radio-plume suggests a possible role of the latterexcitation of the ambient gas reservoir. The stacking technique was used tosearch for CO emission and 3mm continuum emission from galaxies in thesurrounding cluster, however no detection was found either toward individualgalaxies or the stacked ensemble of galaxies, with a 3 sigma limit of <1.1x10^9 M_sun for the molecular gas.

astrophysical journal/the astrophysical journal

Unveiling the mask on the ULIRG-to-QSO transition object [H89]1821+643  at z=0.3: a gas-poor/gas-rich galaxy merger and the implications for CO-based  dynamical mass estimates