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VERSION:2.0
CALSCALE:GREGORIAN
PRODID:UW-Madison-Physics-Events
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SEQUENCE:0
UID:UW-Physics-Event-3350
DTSTART:20140501T203000Z
DTEND:20140501T220000Z
DTSTAMP:20260312T105744Z
LAST-MODIFIED:20140416T123448Z
LOCATION:4421 Sterling Hall
SUMMARY:Gas Flows in Galaxy Clusters\, Astronomy Colloquium\, Brian Mc
 Namara\, University of Waterloo
DESCRIPTION:Galaxies and clusters are embedded in gaseous hot atmosphe
 res that serve as repositories of unused fuel for galaxy formation\, e
 jecta from evolved stars\, and mechanical energy released by supermass
 ive black holes.  The hot gas located within the central galaxy is exp
 ected to cool and fuel star formation.  Yet most giant elliptical gala
 xies are "red and dead."  Instead\, cooling is suppressed by powerful 
 radio jets that periodically heat the gas in a self-regulating feedbac
 k loop.  Radio-mechanical feedback may explain the the dearth of  lumi
 nous\, blue galaxies predicted by standard Lambda-CDM models and the e
 xcess of hot baryons in the Universe.  I will discuss recent studies s
 howing that radio-mechanical feedback  also drives hot outflows at rat
 es of tens of solar masses per year from central cluster galaxies.  I 
 will highlight new results from the Atacama Large Millimeter Array (AL
 MA) showing that the hot gas that has cooled resides in nascent molecu
 lar gas disks and plumes of molecular gas clouds flying in and out of 
 the galaxy.  The ALMA data for the Abell 1835 BCG indicate a molecular
  outflow at a rate of ~200 solar masses per year behind a pair of buoy
 antly rising radio/X-ray bubbles.  Apparently\, X-ray bubbles couple e
 fficiently to molecular clouds\,  and this may have broader implicatio
 n for the evolution of galaxies and supermassive black holes.
URL:https://www.physics.wisc.edu/events/?id=3350
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