We report on a deep , multiwavelength study of the galaxy cluster MACS J1931.8-2634 using Chandra X-ray , Subaru optical , and VLA 1.4 GHz radio data .
This cluster ( z = 0.352 ) harbors one of the most X-ray luminous cool cores yet discovered , with an equivalent mass cooling rate within the central 50 h _ { \mathrm { 70 } } ^ { -1 } { \thinspace kpc } is \sim 700 M _ { \mathrm { \odot } } { \thinspace yr } ^ { -1 } .
Unique features observed in the central core of MACS J1931.8-2634 hint to a wealth of past activity that has greatly disrupted the original cool core .
The X-ray and optical data suggest oscillatory motion of the cool core along a roughly north-south direction .
We also observe a spiral of relatively cool , dense , X-ray emitting gas connected to the cool core , as well as highly elongated intracluster light ( ICL ) surrounding the cD galaxy .
For a cluster with such a high nominal cooling rate , this cluster is missing the central metallicity peak almost always seen in cool core clusters , which suggests bulk transport of cool gas out to large distances from the center .
Extended radio emission is observed surrounding the central AGN , elongated in the east-west direction , spatially coincident with X-ray cavities .
The power input required to inflate these ‘ bubbles ’ is estimated from both the X-ray and radio emission to reside between P _ { \mathrm { jet } } \sim 4 – 14 \times 10 ^ { 45 } { \thinspace erg } { \thinspace s } ^ { -1 } , putting it among the most powerful jets ever observed .
This combination of a powerful AGN outburst and bulk motion of the cool core have resulted in two X-ray bright ridges to form to the north and south of the central AGN at a distance of approximately 25 kpc .
The northern ridge has spectral characteristics typical of cool cores : it contains low temperature , high density , metal rich gas and is consistent with being a remnant of the cool core after it was disrupted by the AGN and bulk motions .
It is also the site of H \alpha filaments and young stars .
The X-ray spectroscopic cooling rate associated with this ridge is \sim 165 M _ { \mathrm { \odot } } { \thinspace yr } ^ { -1 } , which agrees with the estimate of the star formation rate from broad-band optical imaging ( \sim 170 M _ { \mathrm { \odot } } { \thinspace yr } ^ { -1 } ) .
MACS J1931.8-2634 appears to harbor one of most profoundly disrupted low entropy cores observed in a cluster , and offers new insights into the survivability of cool cores in the context of hierarchical structure formation .