We present an optical , X-ray , and radio analysis of the starburst in the Abell 1835 cluster ’ s central cD galaxy .
The dense gas surrounding the galaxy is radiating X-rays with a luminosity of \sim 10 ^ { 45 } erg s ^ { -1 } as its temperature ranges from \sim 9 keV to \sim 2 keV , consistent with a cooling rate of \sim 1000 - 2000 { { { M } _ { \odot } } { yr } ^ { -1 } } .
However , Chandra and XMM-Newton observations found less than 200 { { { M } _ { \odot } } { yr } ^ { -1 } } of gas cooling below \sim 2 keV , a level that is consistent with the cD ’ s current star formation rate of 100 - 180 { { { M } _ { \odot } } { yr } ^ { -1 } } .
One or more heating agents ( feedback ) must then be replenishing the remaining radiative losses .
The heat fluxes from supernova explosions and thermal conduction alone are unable to do so .
However , a pair of X-ray cavities from an AGN outburst has deposited \simeq 1.7 \times 10 ^ { 60 } erg into the surrounding gas over the past 40 Myr .
The corresponding jet power \simeq 1.4 \times 10 ^ { 45 } ~ { } { erg~ { } s ^ { -1 } } is enough to offset most of the radiative losses from the cooling gas .
The jet power exceeds the radio synchrotron power by \sim 4000 times , making this one of the most radiatively inefficient radio sources known .
The large jet power implies that the cD ’ s supermassive black hole accreted at a mean rate of \sim 0.3 { { { M } _ { \odot } } { yr } ^ { -1 } } over the last 40 Myr or so , which is a small fraction of the Eddington accretion rate for a \sim 10 ^ { 9 } { { M } _ { \odot } } black hole .
The ratio of the bulge growth rate through star formation and the black hole growth rate through accretion is consistent with the slope of the ( Magorrian ) relationship between bulge and central black hole mass in nearby quiescent galaxies .
The surface densities of molecular gas and star formation follow the Schmidt-Kennicutt parameterizations , indicating that the high pressure environment does not substantially alter the IMF and other conditions leading to the onset of star formation .
The cD in Abell 1835 appears in many respects to be a textbook example of galaxy formation governed by the gravitational binding energy released by accretion onto a supermassive black hole .
The consistency between net cooling , heating ( feedback ) , and the cooling sink ( star formation ) in this system resolves the primary objection to traditional cooling flow models .