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      <Title>Extended X-ray Emission From A Quasar-Driven Superbubble</Title>
      
      <Abstract>We propose to look for the X-ray component of a bona-fide quasar-driven wind, manifested as a 20 kpc-scale superbubble in the warm ionized gas of its host galaxy. With ALMA and JVLA observations, we have ruled out star formation or a radio jet as the source of the outflow, and we have detected very soft (&lt;1 keV) X-ray photons spatially coincident with the superbubble. With our existing 20 ks observation, we cannot determine whether the X-rays arise from the hot outflow or photoionized gas. With an additional 80ks observation (100ks total), we will use the X-ray morphology and spectrum to distinguish these two possibilities. A single-orbit HST observation will allow us to both build a pure emission-line map of the outflow and (via scattered light) teach us about the ambient density in the outflow.</Abstract>
      
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         FirstName="Jenny"
         MiddleInitial="E."
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         Institution="Princeton University"
         Country="USA"
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         Institution="Eureka Scientific Inc."
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         Institution="The Johns Hopkins University"
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            <ObservingDescription>We will perform a single-orbit observation of the obscured quasar and ULIRG SDSS J1356+1026. 
We will use the medium-band filter F621M with WFC3, to match our existing broad-band 
data but focus exclusively on the continuum.  By comparing the line emission in the broad-band 
image with a line-free image, we will map the line emission with high fidelity and use the scattered 
light fraction to determine the electron density.</ObservingDescription>
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