A Scalar Field Dark Matter Model and Its Role in the Large-Scale Structure Formation in the Universe

<table> (a) Evolution of the power spectrum for the case which there is no SF. (b) The power spectrum including SF for several values of parameter <svg height="7.9499998" id="M419" style="vertical-align:-0.1638pt" version="1.1" viewbox="0 0 9.7749996 7.9499998" width="9.7749996" xmlns="http://www.w3.org/2000/svg" xmlns:xlink="http://www.w3.org/1999/xlink">
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</svg>. Experimental data are from galaxies in the Sloan Digital Sky Survey (SDSS) catalog and from an analysis of the Lyman-<svg height="7.9499998" id="M421" style="vertical-align:-0.1638pt" version="1.1" viewbox="0 0 9.7749996 7.9499998" width="9.7749996" xmlns="http://www.w3.org/2000/svg" xmlns:xlink="http://www.w3.org/1999/xlink">
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</svg> forest [<a href="/journals/aa/2012/509682/#B54">54</a>].</table>

Advances in Astronomy

fig4

Figure 4

Figure 4: A Scalar Field Dark Matter Model and Its Role in the Large-Scale Structure Formation in the Universe 