@article {273, title = {A CHANDRA X-ray Analysis of ABELL 1664: Cooling, Feedback, and Star Formation in the Central Cluster Galaxy}, journal = {The Astrophysical Journal}, volume = {697}, year = {2010}, chapter = {867}, abstract = {

The brightest cluster galaxy (BCG) in the Abell 1664 cluster is unusually blue and is forming stars at a rate of \∼ 23 M_{sun} yr^{\−1}. The BCG is located within 5 kpc of the X-ray peak, where the cooling time of 3.5 \× 108 yr and entropy of 10.4 keV cm2 are consistent with other star-forming BCGs in cooling flow clusters. The center of A1664 has an elongated, \“barlike\” X-ray structure 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 stripped from interloping galaxies. The cooling rate in this region is roughly consistent with the star formation rate, suggesting that the hot gas is condensing onto the BCG.We use the scaling relations of B{\i}rzan et al. to show that the active galactic nucleus (AGN) is underpowered compared
to the central X-ray cooling luminosity by roughly a factor of three. We suggest that A1664 is experiencing rapid cooling and star formation during a low state of an AGN feedback cycle that regulates the rates of cooling and star formation. Modeling the emission as a single-temperature plasma, we find that the metallicity peaks 100 kpc from the X-ray center, resulting in a central metallicity dip. However, a multi-temperature cooling flow model improves the fit to the X-ray emission and is able to recover the expected, centrally peaked metallicity profile.

}, keywords = {clusters, cooling flows - galaxies, galaxies, individual (A1664) - galaxies, starburst - X-rays}, doi = {http://dx.doi.org/10.1088/0004-637X/697/1/867}, author = {CC Kirkpatrick and B R. McNamara and D A. Rafferty and P E. J. Nulsen and L Birzan and F Kazemzadeh and M W. Wise and M Gitti and K W. Cavagnolo} } @article {276, title = {An Energetic AGN Outburst Powered by a Rapidly Spinning Supermassive Black Hole or an Accreting Ultramassive Black Hole}, journal = {The Astrophysical Journal}, volume = {698}, year = {2010}, chapter = {594}, abstract = {

Powering the 10^{62} erg nuclear outburst in the MS0735.6+7421 cluster central galaxy by accretion with a 10\% mass-to-energy conversion efficiency implies that its putative supermassive black hole (SMBH) grew by \∼ 6 \× 10^{8}M_{sun} over the past 100 Myr. Guided by data at several wavelengths, we place upper limits on the amount of cold gas and star formation near the nucleus of \< 10^{9} M_{sun} and \< 2 M_{sun} yr^{\−1}, respectively. These limits imply that an implausibly
large fraction of the preexisting cold gas in the inner several kpc must have been consumed by its SMBH at the rate of \∼ 3\–5 M_{sun} yr^{\−1} during the past 100 Myr while leaving no trace of star formation. Such a high accretion rate would be difficult to maintain by stellar accretion or the Bondi mechanism, unless the black hole mass approaches 10 ^{11} M_{sun}. Furthermore, its feeble nuclear luminosities in the UV, I, and X-ray bands compared to its enormous mechanical power are inconsistent with rapid accretion onto a \∼ 5 \× 10^{9} M_{sun} black hole. We suggest instead that the active galactic nucleus (AGN) outburst is powered by angular momentum released from a rapidly spinning
black hole. The rotational energy and power available from a spinning black hole are consistent with the cavity and shock energetics inferred from X-ray observations. A maximally spinning 10 ^{9} M_{sun} black hole contains enough rotational energy, \∼ 10^{62} erg, to quench a cooling flow over its lifetime and to contribute significantly to the excess entropy found in the hot atmospheres of groups and clusters. Two modes of AGN feedback may be quenching star formation in elliptical galaxies centered in cooling halos at late times. An accretion mode that operates in gas-rich systems, and a spin mode operating at modest accretion rates. The spin conjecture may be avoided in MS0735 by appealing to Bondi accretion onto a central black hole whose mass greatly exceeds 10^{10} M_{sun}. The host galaxy\’s unusually large 3.8 kpc stellar core radius (light deficit) may witness the presence of an ultramassive black hole.

}, keywords = {active-galaxies, clusters, galaxies, individual (MS0735.6+7421) - X-rays}, doi = {http://dx.doi.org/10.1088/0004-637X/698/1/594}, author = {B R. McNamara and F Kazemzadeh and D A. Rafferty and L Birzan and P E. J. Nulsen and C C. Kirkpatrick and M W. Wise} }