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<HSTProposal
   Phase1ID="953"
   Phase2ID="14300"
   Phase="Phase I"
   AptVersion="Version 23.0.1 ">
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   <!--Date: Fri Apr 10 23:56:47 GMT 2015-->
   
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            Cycle="23"
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            NotificationAddress="r.c.livermore@astro.as.utexas.edu"
            AssignedID="953">
            
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            <SubmissionLog>Assigned ID: 953

----- Attempting Submission 1 (Fri Apr 10 22:30:07 GMT 2015) -----
HST Phase I Proposal 953 (hff_submitted_v1.apt) successfully submitted.
Receipt: # 953-1

----- Attempting Submission 2 (Fri Apr 10 23:44:49 GMT 2015) -----
HST Phase I Proposal 953 (hff_submitted_v1.apt) successfully submitted.
Receipt: # 953-2

----- Attempting Submission 3 (Fri Apr 10 23:56:47 GMT 2015) -----</SubmissionLog>
            
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   <ProposalInformation
      Category="AR"
      PureParallelProposal="false"
      Cycle="23"
      STScIEditNumber="0">
      
      <Title>Searching for faint high-z galaxies in the Hubble Frontier Fields</Title>
      
      <Abstract>We request funding to support the study of the complete data from the Hubble Frontier Fields (HFF) program. We have developed a method for detecting the faintest lensed galaxies in the cluster fields using wavelet decomposition, and propose to use these data to study several key science areas:
1) The faint end of the rest-frame ultraviolet (UV) luminosity function at z=7-8: We will improve the estimates of the faint-end slope, which remains poorly constrained. The lensing fields will probe luminosities &lt;&lt;0.1L*, while the blank fields will increase the number of &lt;0.5L* galaxies by a factor of 3x. By the completion of the HFF survey, we expect to be able to measure the faint-end slope to within 10%, honing in on the contribution of galaxies to reionization.
2) The colors of faint galaxies: The HFF will probe low-metallicity stars at high-z. The cluster fields will yield galaxies with intrinsic absolute magnitudes fainter than -17, where we expect to see low-metallicity star formation, and the blank fields will increase the numbers of m=28-29 galaxies by 3x, strongly reducing the uncertainty on their mean color.
3) The abundance of galaxies at z=9: The inclusion of the F140W filter in all HFF observations will allow the robust two-band detection of z=9 galaxies. Using a larger sample over a wider dynamic range in luminosity, we will investigate the apparent discrepancy between previous studies at z=9 based on the HUDF.
With funding to carry out this work on the complete dataset, we will be able to place the most robust constraints yet on these high-z galaxies, maximizing the output from the HFF program in advance of JWST.</Abstract>
      
      <PrincipalInvestigator
         Honorific="Dr."
         FirstName="Rachael"
         LastName="Livermore"
         ESAMember="false"
         Retired="false"
         UniqueID="8991"
         Institution="University of Texas at Austin"
         Country="USA"
         State="TX"
         Contact="true" />
      
      <CoInvestigator
         Honorific="Prof."
         FirstName="Steven"
         MiddleInitial="L."
         LastName="Finkelstein"
         ESAMember="false"
         Retired="false"
         UniqueID="8349"
         Institution="University of Texas at Austin"
         Country="USA"
         State="TX"
         Contact="false"
         AdminUSPI="false" />
      
      <CoInvestigator
         Honorific="Dr."
         FirstName="Jennifer"
         LastName="Lotz"
         ESAMember="false"
         Retired="false"
         UniqueID="5502"
         Institution="Space Telescope Science Institute"
         Country="USA"
         State="MD"
         Contact="false"
         AdminUSPI="false" />
      
      <CoInvestigator
         Honorific="Prof."
         FirstName="Michael"
         LastName="Boylan-Kolchin"
         ESAMember="false"
         Retired="false"
         UniqueID="8951"
         Institution="University of Maryland"
         Country="USA"
         State="MD"
         Contact="false"
         AdminUSPI="false" />
      
      <CoInvestigator
         FirstName="Mimi"
         LastName="Song"
         ESAMember="false"
         Retired="false"
         UniqueID="13718"
         Institution="University of Texas at Austin"
         Country="USA"
         State="TX"
         Contact="false"
         AdminUSPI="false" />
      
      <Questions>
         
         <Phase2Questions>
            
            <ObservingDescription />
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      <Orbits
         ThisCycle2GyroPrimary="1" />
      
      <Phase1ProposalInformation
         TotalTargets="1"
         Attachment="/Users/r.c.livermore/work/Proposals/HST/C23/hff.pdf"
         ProposalSize="SMALL">
         
         <ScientificCategory>COSMOLOGY</ScientificCategory>
         
         <ScientificKeyword1
            Keyword="Dust" />
         
         <ScientificKeyword2
            Keyword="Galaxy Formation And Evolution" />
         
         <ScientificKeyword3
            Keyword="Gravitational Lensing" />
         
         <ScientificKeyword4
            Keyword="High Redshift Galaxies" />
         
         <ScientificKeyword5
            Keyword="Hubble Deep Fields" />
         
         <ProprietaryPeriod
            Default="true">0</ProprietaryPeriod>
         
         <Budget>Regular</Budget>
         
         <CalibProp>false</CalibProp>
         
         <UvInit>false</UvInit>
         
         <Treasury>false</Treasury>
         
         <MultiCycleTreasury>false</MultiCycleTreasury>
         
         <Theory>false</Theory>
      </Phase1ProposalInformation>
      
      <Phase2ProposalInformation
         PCFlag="false">
         
         <Availability>SUPPORTED</Availability>
      </Phase2ProposalInformation>
   </ProposalInformation>
   
   <Targets />
   
   <Datasets>
      
      <Dataset
         Instrument="WFC3"
         Number="1"
         NumberOfDatasets="12"
         RetrievalMethod="FTP"
         RetrievalPlan="We will use the WFC3 imaging from the archive for the six Hubble Frontier Field clusters and their associated blank fields. The data released to date are already in our possession, and we will download the remainder as soon as they are released. We anticipate 8 images per field; four filters, and for each filter, a science and weight-map image." />
      
      <Dataset
         Instrument="ACS"
         Number="2"
         NumberOfDatasets="12"
         RetrievalMethod="FTP"
         RetrievalPlan="We will use the ACS imaging from the archive for the six Hubble Frontier Field clusters and their associated blank fields. The data released to date are already in our possession, and we will download the remainder as soon as they are released. We anticipate 6 images per field; four filters, and for each filter, a science and weight-map image." />
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   <Patterns />
   
   <Visits />
</HSTProposal>
