2016, companion paper) to match the geometry, redshift distribution, and completeness of the survey. We then compute the FKP-weighted (Feldman, Kaiser & Peacock 1994) correlation functions using the Landy–Szalay estimator (Landy & Szalay 1993), with a random catalogue 2 generated by the mksample code (see Reid et al. For a comparison of volumes in different cosmologies and P 0 values, see Table 3. In Final Data Release paper, the value used is 10 000 h −3 Mpc 3 following Font-Ribera et al. 2014), and n( z) is the galaxy number density. From an analysis of the spherically averaged correlation function, we infer a distance to z = 0.57 of |$D_V(z)r^ (1)where P 0 is an estimate of the amplitude of the power spectrum at the BAO scale, here assumed to be P 0 = 20 000 h −3 Mpc 3 (as in Anderson et al. The total volume probed is 14.5 Gpc 3, a 10 per cent increment from Data Release 11. We present distance scale measurements from the baryon acoustic oscillation signal in the constant stellar mass and low-redshift sample samples from the Data Release 12 of the Baryon Oscillation Spectroscopic Survey.
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