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We report on interferometric imaging of the CO J=1--0 and J=3--2 lineemission from the controversial QSO/galaxy pair HE 0450--2958. {\it Thedetected CO J=1--0 line emission is found associated with the disturbedcompanion galaxy not the luminous QSO,} and implies $\rm M_{gal}(H_2)\sim(1-2)\times 10^{10} M_{\odot}$, which is $\ga 30% $ of the dynamical mass inits CO-luminous region. Fueled by this large gas reservoir this galaxy is thesite of an intense starburst with $\rm SFR\sim 370 M_{\odot} yr^{-1}$, placingit firmly on the upper gas-rich/star-forming end of Ultra Luminous InfraredGalaxies (ULIRGs, $\rm L_{IR}>10^{12} L_{\odot}$). This makes HE 0450--2958 thefirst case of extreme starburst and powerful QSO activity, intimately linked(triggered by a strong interaction) but not coincident. The lack of CO emissiontowards the QSO itself renews the controversy regarding its host galaxy bymaking a gas-rich spiral (the typical host of Narrow Line Seyfert~1 AGNs) lesslikely. Finally, given that HE 0450--2958 and similar IR-warm QSOs areconsidered typical ULIRG$\to $(optically bright QSO) transition candidates, ourresults raise the possibility that some may simply be {\it gas-rich/gas-poor(e.g. spiral/elliptical) galaxy interactions} which ``activate'' an opticallybright unobscured QSO in the gas-poor galaxy, and a starburst in the gas-richone. We argue that such interactions may have gone largely unnoticed even inthe local Universe because the combination of tools necessary to disentagle theprogenitors (high resolution and S/N optical {\it and} CO imaging) becameavailable only recently.

A new twist to an old story: HE 0450-2958, and the ULIRG$\to $(optically bright QSO) transition hypothesis