An Energetic AGN Outburst Powered by a Rapidly Spinning Supermassive Black Hole Export

@article{citeulike:3649630, abstract = {Powering the 10E62 erg AGN outburst in the MS0735.6+7421 cluster's central galaxy by accretion implies that its putative supermassive black hole (SMBH) grew by \~{}6E8 solar masses or nearly 1/3 of its mass over the past 100 Myr. Guided by data at several wavelengths, we place restrictive upper limits on the amount of cold gas and star formation near the nucleus of \<10E9 solar masses and \<2 solar masses per year, respectively. These limits imply that much of the preexisting gas in the inner several kpc must have been consumed by its SMBH during the past 100 Myr at the rate of \~{}3-5 solar masses per year, or roughly 1/10 of the Eddington rate, while leaving no trace of star formation. These properties are inconsistent with an accretion-powered AGN. We suggest instead that MS0735's AGN is powered by a rapidly-spinning black hole. The rotational energy and power are consistent with the cavity and shock energetics and their ages inferred from X-ray observations. The host galaxy's unusually large, 3.8 kpc stellar core may have been scoured-out in part during the inspiral of one or more SMBH's, thus endowing the merged remnant with its enormous size and spin. A maximally-spinning, 1E9 solar mass SMBH contains enough rotational energy, \~{}10E62 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. We suggest two modes of AGN feedback are 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 that operates at modest accretion rates. The central galaxy's large core and demanding AGN power suggest it harbors a \>10E10 solar mass ultramassive black hole.}, archivePrefix = {arXiv}, author = {Mcnamara, B. R. and Kazemzadeh, F. and Rafferty, D. A. and Birzan, L. and Nulsen, P. E. J. and Kirkpatrick, C. C. and Wise, M. W.}, citeulike-article-id = {3649630}, citeulike-linkout-0 = {http://arxiv.org/abs/0811.3020}, citeulike-linkout-1 = {http://arxiv.org/pdf/0811.3020}, day = {18}, eprint = {0811.3020}, keywords = {active, clusters, cooling, flows, galactic, galaxy, individual, ms073567421, nuclei}, month = {Nov}, posted-at = {2008-11-21 15:09:03}, priority = {3}, title = {An Energetic AGN Outburst Powered by a Rapidly Spinning Supermassive Black Hole}, url = {http://arxiv.org/abs/0811.3020}, year = {2008} }

TY - JOUR ID - citeulike:3649630 L3 - citeulike-article-id:3649630 N2 - Powering the 10E62 erg AGN outburst in the MS0735.6+7421 cluster's central galaxy by accretion implies that its putative supermassive black hole (SMBH) grew by ~6E8 solar masses or nearly 1/3 of its mass over the past 100 Myr. Guided by data at several wavelengths, we place restrictive upper limits on the amount of cold gas and star formation near the nucleus of <10E9 solar masses and <2 solar masses per year, respectively. These limits imply that much of the preexisting gas in the inner several kpc must have been consumed by its SMBH during the past 100 Myr at the rate of ~3-5 solar masses per year, or roughly 1/10 of the Eddington rate, while leaving no trace of star formation. These properties are inconsistent with an accretion-powered AGN. We suggest instead that MS0735's AGN is powered by a rapidly-spinning black hole. The rotational energy and power are consistent with the cavity and shock energetics and their ages inferred from X-ray observations. The host galaxy's unusually large, 3.8 kpc stellar core may have been scoured-out in part during the inspiral of one or more SMBH's, thus endowing the merged remnant with its enormous size and spin. A maximally-spinning, 1E9 solar mass SMBH contains enough rotational energy, ~10E62 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. We suggest two modes of AGN feedback are 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 that operates at modest accretion rates. The central galaxy's large core and demanding AGN power suggest it harbors a >10E10 solar mass ultramassive black hole. TI - An Energetic AGN Outburst Powered by a Rapidly Spinning Supermassive Black Hole KW - active KW - clusters KW - cooling KW - flows KW - galactic KW - galaxy KW - individual KW - ms073567421 KW - nuclei AU - Mcnamara, BR AU - Kazemzadeh, F AU - Rafferty, DA AU - Birzan, L AU - Nulsen, PEJ AU - Kirkpatrick, CC AU - Wise, MW PY - 2008/Nov/18/ UR - http://arxiv.org/abs/0811.3020 ER -