<?xml version="1.0" encoding="ISO-8859-1"?>

<HSTProposal
   Phase1ID="140"
   Phase2ID="11271"
   Phase="Phase I"
   AptVersion="Version 16.0 ">
   <!--**********************************************************************************************************************-->
   <!--This file is automatically generated and should not be edited by hand. Editing this file directly is at your own risk.-->
   <!--**********************************************************************************************************************-->
   
   <ToolData>
      
      <ToolDataItem
         Key="SubmissionData">
         
         <SubmissionData
            AptVersion="Version 16.0 "
            SubmissionCounter="2"
            SubmissionSuccessCounter="1"
            HasErrors="false"
            Cycle="16"
            IncludeSysInfo="true"
            NotificationAddress="bmcnamar@nmsu.edu"
            AssignedID="140">
            
            <SystemInformation
               os.arch="i386"
               os.name="Linux"
               os.version="2.4.21-27.0.2.ELsmp"
               java.version="1.5.0_08"
               linux.distribution="Red Hat Enterprise"
               linux.version="3 " />
            
            <SubmissionComments />
            
            <SubmissionLog>  Assigned ID: 140
----- Attempting Submission 2 (Thu Jan 25 19:20:25 GMT 2007) -----
</SubmissionLog>
            
            <DiagnosticJustification />
         </SubmissionData>
      </ToolDataItem>
   </ToolData>
   
   <ProposalInformation
      Category="AR"
      PureParallelProposal="false"
      Cycle="16"
      STScIEditNumber="0">
      
      <Title>Establishing a Zero Motion Reference Frame for the FGS</Title>
      
      <Abstract>We propose to measure the internal proper motions of the stars in M35 that are used to calibrate the HST/FGS. The goal of this effort is to remove the influence these stars have the FGS distortion map. Employing the approximately 108 orbits of available archival FGS data, these motions can be determined to an accuracy of 0.05 mas/year. By iteratively measuring these motions using successively longer time bases and then accounting for them in the distortion map, their influence on this map can be essentially eliminated.</Abstract>
      
      <PrincipalInvestigator
         Honorific="Dr."
         FirstName="Bernard"
         MiddleInitial="J."
         LastName="McNamara"
         ESAMember="false"
         UniqueID="1848"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="New Mexico State University"
            USState="NM"
            Country="USA" />
      </PrincipalInvestigator>
      
      <CoInvestigator
         Honorific="Dr."
         FirstName="Barbara"
         LastName="McArthur"
         ESAMember="false"
         UniqueID="4137"
         AdminUSPI="false"
         Contact="false"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="University of Texas at Austin"
            USState="TX"
            Country="USA" />
      </CoInvestigator>
      
      <CoInvestigator
         Honorific="Dr."
         FirstName="Thomas"
         LastName="Harrison"
         ESAMember="false"
         UniqueID="3839"
         AdminUSPI="false"
         Contact="false"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="New Mexico State University"
            USState="NM"
            Country="USA" />
      </CoInvestigator>
      
      <CoInvestigator
         Honorific="Mr."
         FirstName="Doug"
         LastName="Hoffman"
         ESAMember="false"
         AdminUSPI="false"
         Contact="false"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="New Mexico State University"
            USState="NM"
            Country="USA" />
      </CoInvestigator>
      
      <Questions>
         
         <Phase2Questions>
            
            <ObservingDescription />
            
            <RealtimeJustification />
            
            <CalibrationJustification />
            
            <AdditionalComments />
         </Phase2Questions>
      </Questions>
      
      <Orbits
         ThisCycle2GyroPrimary="1"
         ThisCycle2GyroParallel="0"
         NextCycle2GyroPrimary="0"
         NextCycle2GyroParallel="0"
         AfterNext2GyroPrimary="0"
         AfterNext2GyroParallel="0" />
      
      <Phase1ProposalInformation
         TotalTargets="1"
         Attachment="/home/ajax/bmcnamar/hst/cycle16/finalm35.pdf">
         
         <ScientificCategory>HOT STARS</ScientificCategory>
         
         <ScientificKeyword1
            Keyword="ASTROMETRY" />
         
         <ScientificKeyword2
            Keyword="DYNAMICS" />
         
         <ScientificKeyword3
            Keyword="CLUSTER BINARY STARS AND BLUE STRAGGLERS" />
         
         <ProprietaryPeriod>12</ProprietaryPeriod>
         
         <Budget>67000</Budget>
         
         <BudgetExplanation>see below</BudgetExplanation>
         
         <CalibProp>true</CalibProp>
         
         <SpitzerHours>0.0</SpitzerHours>
         
         <Treasury>false</Treasury>
         
         <Legacy>false</Legacy>
         
         <Theory>false</Theory>
         
         <LargeProgram>false</LargeProgram>
         
         <Spitzer>false</Spitzer>
         
         <Survey>false</Survey>
      </Phase1ProposalInformation>
      
      <Phase2ProposalInformation
         PCFlag="false">
         
         <Availability>SUPPORTED</Availability>
      </Phase2ProposalInformation>
   </ProposalInformation>
   
   <Targets />
   
   <Observations />
   
   <Datasets>
      
      <Dataset
         Instrument="FGS"
         Number="1"
         NumberOfDatasets="108"
         RetrievalMethod="FTP"
         RetrievalPlan="The FGS datasets will be provided to Dr. McNamara by B. McArthur of the FGS Astrometry Team" />
   </Datasets>
   
   <Patterns />
   
   <Visits />
</HSTProposal>


