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<HSTProposal
   Phase2ID="11311"
   Phase="Phase II"
   AptVersion="Version 17.0 ">
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   <!--This file is automatically generated and should not be edited by hand. Editing this file directly is at your own risk.-->
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   <!---->
   <!--APT Version: Version 17.0 -->
   <!--Date: Wed Jan 23 18:14:42 GMT 2008-->
   
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   <ProposalInformation
      Category="GO/DD"
      PureParallelProposal="false"
      Cycle="15"
      STScIEditNumber="6">
      
      <Title>The high-amplification microlensing event OGLE-2007-BLG-224: a substellar lens in the Galactic disk or a low-mass stellar lens in the halo?</Title>
      
      <Abstract>OGLE-2007-BLG-224/MOA-2007-BLG-163 is a remarkable microlensing event towards the Galactic bulge, which peaked on May 12, 2007. The light curve reached a peak magnification of ~3700, which is the highest magnification ever observed. The color and magnitude of the source indicate that it is a G-dwarf in the Galactic bulge, and source radius crossing time of t* = 8.2 minutes implies that the lens-source relative proper motion is 45 mas/yr. This indicates that the lens must either be a very nearby brown dwarf, or a halo star. The HST observations proposed here provide a very good chance to distinguish between these two possibilities and to determine the distance and mass of the lens. If it is a nearby brown dwarf, it is likely to be associated with a high-proper-motion star that is found close to the source. HST observations taken at two epochs will resolve out the geocentric and the heliocentric the proper-motions, thus providing unambiguous proof that it is a substellar lens. If the lens is a halo star, then it should be detectable as it separates from the source star over the next year. This would be the first definitive detection of a lens star in the Galatic halo and it would help to resolve the long running controversy over whether a significant fraction of the microlensing events seen towards the Magellanic Clouds are due to lens objects in the halo. Thus, it will either be the first clear proof of a substellar lens in the Galactic disk, or the first clear detection of a halo lens.</Abstract>
      
      <PrincipalInvestigator
         Honorific="Dr."
         FirstName="Kailash"
         LastName="Sahu"
         ESAMember="false"
         UniqueID="2253"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="Space Telescope Science Institute"
            USState="MD"
            Country="USA" />
      </PrincipalInvestigator>
      
      <CoInvestigator
         Honorific="Dr."
         FirstName="David"
         MiddleInitial="P."
         LastName="Bennett"
         ESAMember="false"
         UniqueID="3564"
         AdminUSPI="false"
         Contact="false"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="University of Notre Dame"
            USState="IN"
            Country="USA" />
      </CoInvestigator>
      
      <CoInvestigator
         Honorific="Dr."
         FirstName="Andrew"
         LastName="Gould"
         ESAMember="false"
         UniqueID="791"
         AdminUSPI="false"
         Contact="false"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="The Ohio State University Research Foundation"
            USState="OH"
            Country="USA" />
      </CoInvestigator>
      
      <CoInvestigator
         Honorific="Dr."
         FirstName="Martin"
         LastName="Dominik"
         ESAMember="false"
         UniqueID="791"
         AdminUSPI="false"
         Contact="false"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="University of St. Andrews"
            Country="UK" />
      </CoInvestigator>
      
      <CoInvestigator
         Honorific="Dr."
         FirstName="Andrzej"
         LastName="Udalski"
         ESAMember="false"
         UniqueID="7531"
         AdminUSPI="false"
         Contact="false"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="Warsaw University"
            Country="Poland" />
      </CoInvestigator>
      
      <CoInvestigator
         Honorific="Dr."
         FirstName="Takahiro"
         LastName="Sumi"
         ESAMember="false"
         UniqueID="7206"
         AdminUSPI="false"
         Contact="false"
         AddressVerifiedCycle="16">
         
         <Address
            Institution="Nagoya University"
            Country="Japan" />
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      <Questions>
         
         <Phase2Questions>
            
            <ObservingDescription>We will use WFPC2 to image the field in V and I filters, with the object placed in the PC chip. Given its magnitude of I~18.1, we will require about ~(5 +5) min exposures in V and I filters, which should allow us to see fainter objects in the field without saturating the source.  We will also use NICMOS/NIC1 to image the field in J and H bands. The observations will be repeated about 8 months later. Note that the galactic bulge can be observed from about February to June, which allows the observations to be taken 8 months apart, in the 2-gyro mode.</ObservingDescription>
            
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      <Phase1ProposalInformation
         TotalTargets="1"
         Attachment="/usr/local/APT/APT1622/C:\Users\ksahu\Desktop\phase16-ks.pdf">
         
         <ScientificCategory>COOL STARS</ScientificCategory>
         
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            Keyword="Astrometry" />
         
         <ScientificKeyword2
            Keyword="Galactic Bulge" />
         
         <ScientificKeyword3
            Keyword="Gravitational Lensing" />
         
         <ScientificKeyword4
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            <Description>G V-IV</Description>
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