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The brightest cluster galaxy (BCG) in the Abell 1664 cluster is unusuallyblue and is forming stars at a rate of ~ 23 M_{\sun} yr^{-1}. The BCG islocated within 5 kpc of the X-ray peak, where the cooling time of 3.5x10^8 yrand entropy of 10.4 keV cm^2 are consistent with other star-forming BCGs incooling flow clusters. The center of A1664 has an elongated, "bar-like" X-raystructure whose mass is comparable to the mass of molecular hydrogen, ~ 10^{10}M_{\sun} in the BCG. We show that this gas is unlikely to have been strippedfrom interloping galaxies. The cooling rate in this region is roughlyconsistent with the star formation rate, suggesting that the hot gas iscondensing onto the BCG. We use the scaling relations of Birzan et al. 2008 toshow that the AGN is underpowered compared to the central X-ray coolingluminosity by roughly a factor of three. We suggest that A1664 is experiencingrapid cooling and star formation during a low-state of an AGN feedback cyclethat regulates the rates of cooling and star formation. Modeling the emissionas a single temperature plasma, we find that the metallicity peaks 100 kpc fromthe X-ray center, resulting in a central metallicity dip. However, amulti-temperature cooling flow model improves the fit to the X-ray emission andis able to recover the expected, centrally-peaked metallicity profile.

A Chandra X-ray Analysis of Abell 1664: Cooling, Feedback and Star Formation in the Central Cluster Galaxy