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----- Attempting Submission 1 (Fri Apr 10 05:50:30 GMT 2015) -----
HST Phase I Proposal 369 (Hot_APT.apt) successfully submitted.
Receipt: # 369-3

----- Attempting Submission 4 (Fri Apr 10 19:42:32 GMT 2015) -----</SubmissionLog>
            
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      <Title>A Young White Dwarf with an Infrared Excess: Dust Disk or Substellar Companion?</Title>
      
      <Abstract>We recently discovered the youngest white dwarf with 2-8 micron emission. Its SED can be fit by either a dust disk or a substellar companion. Two unique properties of this object favor the substellar companion hypothesis: (i) the color of the infrared excess; (ii) the non-detection of heavy elements with Keck/HIRES observations. We propose to use COS to look for heavy elements; which would be about two orders of magnitude more sensitive than the HIRES studies. If heavy elements are detected, the excess emission is likely to come from dust and this would be the hottest white dwarf with a ~1200 K dust disk; otherwise, the excess is likely to come from a substellar companion, possibly a rejuvenated planet, which would rank among the closest and lowest mass companions known to orbit a white dwarf.</Abstract>
      
      <PrincipalInvestigator
         Honorific="Dr."
         FirstName="Siyi"
         LastName="Xu"
         ESAMember="true"
         Retired="false"
         UniqueID="9028"
         Institution="European Southern Observatory - Germany"
         Country="DEU"
         Contact="true"
         AdminCoI="CoI: Dr. Michael Jura " />
      
      <CoInvestigator
         Honorific="Dr."
         FirstName="Michael"
         LastName="Jura"
         ESAMember="false"
         Retired="false"
         UniqueID="1055"
         Institution="University of California - Los Angeles"
         Country="USA"
         State="CA"
         Contact="false"
         AdminUSPI="true" />
      
      <CoInvestigator
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         FirstName="Ben"
         MiddleInitial="M."
         LastName="Zuckerman"
         ESAMember="false"
         Retired="false"
         UniqueID="4609"
         Institution="University of California - Los Angeles"
         Country="USA"
         State="CA"
         Contact="false"
         AdminUSPI="false" />
      
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            <ObservingDescription>Our goal is to look for heavy elements in the atmosphere of PG 0010+280 to understand the origin of its infrared excess. The strongest photospheric line comes from silicon, including Si II 1265 A, Si III 1299 A and Si IV 1392 A. 

We will employ the G130M grating with a central wavelength of 1291 A and a wavelength coverage of 1137-1274 A and 1292-1432 A.Extrapolating from the GALEX flux, we found that an average S/N of 45 can be reached with an exposure time of 2200 sec (1 orbit) according to the ETC. To minimize the fixed-pattern noise, all four FP-POS steps are used.</ObservingDescription>
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         Attachment="/Users/sxu/Work/Telescopes/HST/Cycle23/3_PG0010+280/phase1-GO.pdf"
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         <ScientificCategory>EXTRA-SOLAR PLANETS</ScientificCategory>
         
         <ScientificKeyword1
            Keyword="Circumstellar Disks" />
         
         <ScientificKeyword2
            Keyword="Giant Planets" />
         
         <ScientificKeyword3
            Keyword="Very Low Mass Stars And Brown Dwarfs" />
         
         <ScientificKeyword4
            Keyword="White Dwarfs" />
         
         <ProprietaryPeriod
            Default="true">12</ProprietaryPeriod>
         
         <CalibProp>false</CalibProp>
         
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         <Treasury>false</Treasury>
         
         <MultiCycleTreasury>false</MultiCycleTreasury>
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         <Availability>SUPPORTED</Availability>
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         ReferenceFrame="ICRS"
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         <Extended>NO</Extended>
         
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               <Polarimetry>No</Polarimetry>
               
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               <Wavelength>1291</Wavelength>
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