演講資訊

摘要：

Revealing the acceleration of the cosmic expansion is one of the most important issues in cosmology. To investigate the origin of the acceleration, observations of large-scale structure of the Universe traced by galaxy surveys are considered as the best probe. In analyzing galaxy clustering from redshift surveys, one of the most difficult parts to model it is an unclear relation between halo and galaxy distributions. While halo motions are well described by bulk flows, motions of galaxies inside the halos are virialized motions, known as the Finger-of-God effect. Reconstructing the halo density field from the observed galaxy positions is not straightforward because the radial positions of galaxies are distorted along the line of sight (redshift space distortions). In this talk, I present a method to measure the halo power spectrum from the galaxy distribution. I also show how well the method works using a mock galaxy catalog at z=0.5, constructed from N-body simulations and designed to resemble SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) CMASS galaxies, and demonstrate our model can predict the power spectrum of the halos up to k < 0.5h/Mpc to within 5 per cent.