SIMBAD references

We investigate the use of simple colour cuts applied to the Sloan Digital Sky Survey (SDSS) optical imaging to perform photometric selections of emission-line galaxies (ELGs) out to z < 1. Our selection is aimed at discerning three separate redshift ranges: 0.2 ≲ z ≲ 0.4, 0.4 ≲ z ≲ 0.6 and 0.6 ≲ z ≲ 1.0, which we calibrate using data taken by the COMBO-17 survey in a single field (S11). We thus perform colour cuts using the SDSS g, r and i bands and obtain mean photometric redshifts of and. We further calibrate our high-redshift selection using spectroscopic observations with the AAOmega spectrograph on the 4-m Anglo-Australian Telescope, observing ~50-200 galaxy candidates in four separate fields. With just 1h of integration time and seeing of ~ 1.6arcsec, we successfully determined redshifts for ~65 per cent of the targeted candidates. We compare our spectroscopic redshifts to the photometric redshifts from the COMBO-17 survey and find reasonable agreement between the two. We calculate the angular correlation functions of these samples and find correlation lengths of r₀= 2.78±0.08, 3.71±0.11 and 5.50±0.13h^–1Mpc for the low-, mid- and high-redshift samples, respectively. Comparing these results with predicted dark matter clustering, we estimate the bias parameter for each sample to be b = 0.72±0.02, b = 0.93±0.03 and b = 1.43±0.03. We calculate the two-point redshift-space autocorrelation function at z ~ 0.6 and find a clustering amplitude of s_o = 6.4±0.8h^–1Mpc. Finally, we use our photometric sample to search for the integrated Sachs-Wolfe signal in the Wilkinson Microwave Anisotropy Probe (WMAP) 5-yr data. We cross-correlate our three redshift samples with the WMAP W, V, Q and K bands and find an overall trend for a positive signal similar to that expected from models. However, the signal in each is relatively weak, with the results in the WMAP W band being w_Tg(<100arcmin) = 0.25±0.27, 0.17 ±0.20 and 0.17±0.16µK for the low-, mid- and high-redshift samples, respectively. Combining all three galaxy samples, we find a signal of w_Tg(<100arcmin) = 0.20±0.12µK in the WMAP W band, a significance of 1.7σ. However, in testing for systematics where the WMAP data are rotated with respect to the ELG sample, we found similar results at several different rotation angles, implying the apparent signal may be produced by systematic effects.