Ross, Ashley J., Percival, Will J., Carnero, Aurelio, Zhao, Gong-bo, Manera, Marc, Raccanelli, Alvise, Aubourg, Eric, Bizyaev, Dmitry, Brewington, Howard, Brinkmann, J., Brownstein, Joel R., Cuesta, Antonio J., da Costa, Luiz A. N., Eisenstein, Daniel J., Ebelke, Garrett, Guo, Hong, Hamilton, Jean-Christophe, Magaña, Mariana Vargas, Malanushenko, Elena, Malanushenko, Viktor, Maraston, Claudia, Montesano, Francesco, Nichol, Robert C., Oravetz, Daniel, Pan, Kaike et al. 2013. "The clustering of galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: constraints on primordial non-Gaussianity." Monthly Notices of the Royal Astronomical Society 428:1116-1127. https://doi.org/10.1093/mnras/sts094
We analyse the density field of 264 283 galaxies observed by the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS) and included in the SDSS Data Release 9 (DR9). In total, the SDSS DR9 BOSS data include spectroscopic redshifts for over 400 000 galaxies spread over a footprint of more than 3000 deg2. We measure the power spectrum of these galaxies with redshifts 0.43 . We measure the power spectrum of these galaxies with redshifts 0.43 0), is 99.5 per cent. After quantifying and correcting for the systematic bias and including the added uncertainty, we find - 45 0), is 99.5 per cent. After quantifying and correcting for the systematic bias and including the added uncertainty, we find - 45 0) = 91.0 per cent. A more conservative approach assumes that we have only learnt the k dependence of the systematic bias and allows any amplitude for the systematic correction; we find that the systematic effect is not fully degenerate with that of f{_N_L^local}, and we determine that -82 0) = 91.0 per cent. A more conservative approach assumes that we have only learnt the k dependence of the systematic bias and allows any amplitude for the systematic correction; we find that the systematic effect is not fully degenerate with that of f{_N_L^local}, and we determine that -82 0) = 68 per cent. This analysis demonstrates the importance of accounting for the impact of Galactic foregrounds on f{_N_L^local} measurements. We outline the methods that account for these systematic biases and uncertainties. We expect our methods to yield robust constraints on f{_N_L^local} for both our own and future large-scale structure investigations.
