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   <!--Date: Wed Sep 14 23:25:15 GMT 2011-->
   
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            NotificationAddress="mulchaey@obs.carnegiescience.edu"
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            <SubmissionComments>This Phase II submission is associated with HST time awarded by the Chandra TAC.</SubmissionComments>
            
            <SubmissionLog>----- Attempting Submission 1 (Wed Sep 14 23:25:15 GMT 2011) -----</SubmissionLog>
            
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      Cycle="19"
      STScIEditNumber="0">
      
      <Title>The Impact of Brightest Cluster Galaxy Formation on the Intracluster Medium</Title>
      
      <Abstract>We propose Chandra and HST observations of a unique X-ray cluster in which the Brightest Cluster Galaxy (BCG) is in the late stages of formation. The Chandra observations will be used to study how the properties of the intracluster medium are impacted by BCG formation and the HST data will be used to map out the intracluster stellar light. We will test whether the formation of the BCG has destroyed the cool core and determine the role of intracluster stars in enriching the intracluster medium. The proposed observations will be combined with our existing Chandra and HST data for clusters where the BCG is in the early stages of formation, allowing us to develop a more complete evolutionary picture of how BCG formation has affected the intracluster medium.</Abstract>
      
      <PrincipalInvestigator
         Honorific="Dr."
         FirstName="John"
         MiddleInitial="S."
         LastName="Mulchaey"
         ESAMember="false"
         UniqueID="3657">
         
         <Address
            Institution="Carnegie Institution of Washington"
            USState="DC"
            Country="USA" />
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      <CoInvestigator
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         FirstName="Jesper"
         LastName="Rasmussen"
         ESAMember="false"
         UniqueID="8726"
         AdminUSPI="false"
         Contact="false">
         
         <Address
            Institution="Carnegie Institution of Washington"
            USState="DC"
            Country="USA" />
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      <CoInvestigator
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         FirstName="Tesla"
         LastName="Jeltema"
         ESAMember="false"
         UniqueID="12082"
         AdminUSPI="false"
         Contact="false">
         
         <Address
            Institution="University of California - Santa Cruz"
            USState="CA"
            Country="USA" />
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      <CoInvestigator
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         FirstName="Anthony"
         MiddleInitial="H."
         LastName="Gonzalez"
         ESAMember="false"
         UniqueID="7081"
         AdminUSPI="false"
         Contact="false">
         
         <Address
            Institution="University of Florida"
            USState="FL"
            Country="USA" />
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      <CoInvestigator
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         MiddleInitial="M."
         LastName="Lubin"
         ESAMember="false"
         UniqueID="3654"
         AdminUSPI="false"
         Contact="false">
         
         <Address
            Institution="University of California - Davis"
            USState="CA"
            Country="USA" />
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      <Questions>
         
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            <ObservingDescription>The center of a cluster of galaxies at moderate redshift will be observed with WFC3/IR to map out the stellar light near the center of the cluster.  We will observe the cluster in the F160W and F105W filters. The approximate exposure time is 4000 seconds for F160W and 8000 seconds for F105W. To achieve these exposure times we will observe the target using the WFC3-IR-DITHER-BOX-MIN dither pattern.</ObservingDescription>
            
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            <AdditionalComments />
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         Attachment="/Users/mulchaey/Chandra/A013/Highz/modz_groups.pdf">
         
         <ScientificCategory>UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE</ScientificCategory>
         
         <ScientificKeyword1
            Keyword="Clusters Of Galaxies" />
         
         <ScientificKeyword2
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         <Availability>SUPPORTED</Availability>
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               <Polarimetry>No</Polarimetry>
               
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                        <String>The scheduling data was generated by CASM 19.3.</String>
                        
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