Measurements of the Power Spectrum and Redshift Distortions of the Las Campanas Redshift Survey

<p>I present a new method for extracting\&nbsp;<span class="e">power</span>\&nbsp;spectra from galaxy\&nbsp;<span class="f">redshift</span>\&nbsp;surveys called the pair weight compression method. I then apply the method to determine the\&nbsp;<span class="f">redshift</span>\&nbsp;<span class="e">power</span>\&nbsp;<span class="a">spectrum</span>\&nbsp;of the\&nbsp;<span class="c">Las</span>\&nbsp;<span class="b">Campanas</span>\&nbsp;<span class="f">Redshift</span>\&nbsp;<span class="b">Survey</span>\&nbsp;(LCRS). The measured\&nbsp;<span class="f">redshift</span>\&nbsp;<span class="e">power</span>\&nbsp;<span class="a">spectrum</span>\&nbsp;has the same shape as that found by Lin et al. (1996b) but is a factor of 2 smaller. Upon expanding the method to include linear\&nbsp;<span class="f">redshift</span>\&nbsp;distortions, the method is able to measure real space\&nbsp;<span class="e">power</span>\&nbsp;spectra and <em>β</em>. <em>β</em> ≈ Ω<sub>m</sub><sup>0.6</sup>/<em>b </em>where <em>β</em> is the linear\&nbsp;<span class="f">redshift</span>\&nbsp;distortion parameter, Ω<sub>m</sub> is the cosmological density of matter and<em> b</em> is the linear galaxy to mass "bias factor."\&nbsp; Applying the method to LCRS yields a real space\&nbsp;<span class="e">power</span>\&nbsp;<span class="a">spectrum</span>\&nbsp;that is very similar to the\&nbsp;<span class="f">redshift</span>\&nbsp;space\&nbsp;<span class="e">power</span>\&nbsp;<span class="a">spectrum</span>. The measured value of <em>β</em> ≈.55<sup>+.35</sup><sub>-.30</sub>\&nbsp;is larger than, but consistent with, a previous measurement by Matsubara et al. (2000).</p>
Year of Publication
University of Colorado Boulder
JILA PI Advisors
Publication Status