Embeded Code

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          <mods:titleInfo>
            <mods:title>A Position-Sensitive Liquid Xenon 
Time-Projection Chamber for Direct Detection of Dark Matter: The XENON10 
Experiment</mods:title>
          </mods:titleInfo>
          <mods:name type="personal">
            <mods:namePart>Sorensen, Peter F</mods:namePart>
            <mods:role>
              <mods:roleTerm type="text">creator</mods:roleTerm>
            </mods:role>
          </mods:name>
          <mods:originInfo>
            <mods:copyrightDate>2008</mods:copyrightDate>
          </mods:originInfo>
          <mods:physicalDescription>
            <mods:extent>x, 195 p.</mods:extent>
            <mods:digitalOrigin>born digital</mods:digitalOrigin>
          </mods:physicalDescription>
          <mods:note>Thesis (Ph.D. -- Brown University (2008)</mods:note>
          <mods:name type="personal">
            <mods:namePart>Gaitskell, Richard</mods:namePart>
            <mods:role>
              <mods:roleTerm type="text">Director</mods:roleTerm>
            </mods:role>
          </mods:name>
          <mods:name type="personal">
            <mods:namePart>Robert, Lanou</mods:namePart>
            <mods:role>
              <mods:roleTerm type="text">Reader</mods:roleTerm>
            </mods:role>
          </mods:name>
          <mods:name type="personal">
            <mods:namePart>Dell'Antonio, Ian</mods:namePart>
            <mods:role>
              <mods:roleTerm type="text">Reader</mods:roleTerm>
            </mods:role>
          </mods:name>
          <mods:name type="corporate">
            <mods:namePart>Brown University. Physics</mods:namePart>
            <mods:role>
              <mods:roleTerm type="text">sponsor</mods:roleTerm>
            </mods:role>
          </mods:name>
          <mods:genre authority="aat">theses</mods:genre>
          <mods:abstract>Recent astrophsyical observations indicate that 
about 23% of the matter in the universe exists as non-luminous, 
non-baryonic dark matter.  General thermodynamic arguments suggest that 
if an as-yet undiscovered weakly interacting particle were in thermal 
equilibrium in the early universe, it could have a cosmologically 
interesting relic abundance today.  Dark matter particles are predicted 
to have collapsed into isothermal halos on a galactic scale.   Minimal 
super-symmetric extensions of the standard model predict the existence 
of a stable particle with a mass in the range 10-1000 GeV 
c&lt;sup&gt;-2&lt;/sup&gt;, and a an interaction cross section with ordinary matter 
σχ &lt; 10&lt;sup&gt;-36&lt;/sup&gt; cm&lt;sup&gt;2&lt;/sup&gt;.  For the past two 
decades, numerous experiments have been deployed with the aim of direct 
or indirect detection of dark matter.  XENON10 is a direct-detection 
liquid Xe experiment, with event-by-event 3D position reconstruction.  
Since dark matter does not interact electromagnetically, it's signature 
in a Xe detector is expected to be a low-energy nuclear recoil.  
Particle interactions in Xe create scintillation light (&lt;em&gt;S&lt;/em&gt;1) and 
ionization.  The ionization is drifted across the active Xe target and 
converted into a proportional scintillation signal (&lt;em&gt;S&lt;/em&gt;2) by an 
external electric field.  The ratio y = log10(&lt;em&gt;S&lt;/em&gt;2/&lt;em&gt;S&lt;/em&gt;1) 
is larger for β and ɣ background events than for nuclear 
recoils, as determined by neutron calibration data.  This allows 
event-by-event discrimination of background from the expected signal.  
In 2007 XENON10 eclipsed CDMS II as the most sensitive direct-detection 
experiment, excluding the existence of particle dark matter with a 
cross-section (normalized to a single nucleon) σχ &gt; 
10&lt;sup&gt;-43&lt;/sup&gt; cm&lt;sup&gt;2&lt;/sup&gt; at a particle mass of 100 GeV 
c&lt;sup&gt;-2&lt;/sup&gt; (90% C.L.).  Liquid Xe technology is extremely promising 
since it is easily scaled to larger target mass, which will allow 
greater sensitivity to particle dark matter interactions.  I discuss the 
XENON10 detector, deployment, operation, analysis and dark matter 
exclusion results.  I also present a new method to determine the light 
yield of Xe for nuclear recoils, which is essential for calibrating the 
nuclear recoil energy scale and understanding the detector 
threshold.</mods:abstract>
          <mods:subject>
            <mods:topic>WIMP</mods:topic>
          </mods:subject>
          <mods:subject>
            <mods:topic>dark matter</mods:topic>
          </mods:subject>
          <mods:subject>
            <mods:topic>liquid Xe</mods:topic>
          </mods:subject>
          <mods:subject authority="FAST" authorityURI="http://id.worldcat.org/fast" valueURI="http://id.worldcat.org/fast/887854"><mods:topic>Dark matter (Astronomy)</mods:topic></mods:subject><mods:recordInfo>
            <mods:recordContentSource authority="marcorg">RPB</mods:recordContentSource>
            <mods:recordCreationDate encoding="iso8601">20110926</mods:recordCreationDate>
          </mods:recordInfo>
        <mods:language><mods:languageTerm type="code" authority="iso639-2b">eng</mods:languageTerm><mods:languageTerm type="text">English</mods:languageTerm></mods:language>
    <mods:identifier type="doi">10.7301/Z0V1231M</mods:identifier>
<mods:accessCondition type="rights statement" xlink:href="http://rightsstatements.org/vocab/InC/1.0/">In Copyright</mods:accessCondition><mods:accessCondition type="restriction on access">Collection is open for research.</mods:accessCondition><mods:typeOfResource authority="primo">dissertations</mods:typeOfResource></mods:mods>