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Star formation in galaxies at the center of cooling-flow galaxy clusters isan important phenomenon in the context of formation and evolution of massivegalaxies in the Universe. Yet, star formation rates (SFRs) in such systemscontinue to be elusive. We use our Bayesian-motivated spectral energydistribution (SED)-fitting code, BAYESCOOL, to estimate the plausible SFRvalues in the brightest cluster galaxy of a massive, X-ray luminous galaxycluster, Phoenix. Previous studies of Phoenix have resulted in the highestmeasurement of SFR for any galaxy, with the estimates reaching up to 1000 solarmasses/yr. However, a very small number of models have been considered in thosestudies. BAYESCOOL allows us to probe a large parameter space. We consider twomodels for star formation history, instantaneous bursts and continuous starformation, a wide range of ages for the old and the young stellar population,along with other discrete parameters, such as the initial mass function,metallicities, internal extinction and extinction law. We find that in theabsence of any prior except that the maximum cooling rate < 3000 solarmasses/yr, the SFR lies in the range (2230-2890) solar masses/yr. If we imposean observational prior on the internal extinction, E(B-V) < 0.6, the best-fitSFR lies in (454-494) solar masses/yr, and we consider this as the mostprobable range of SFR values for Phoenix. The SFR dependence on the extinctionis a reflection of the standard age-extinction degeneracy, which can beovercome by using a prior on one of the two quantities in question.

monthly notices of the royal astronomical society

The challenging task of determining star formation rates: the case of a  massive stellar burst in the brightest cluster galaxy of Phoenix galaxy  cluster