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The columns similarly increase in wavelength as you move across the page. The first row corresponds to all correlations with the 0.606-μm band, the second for all correlations with the 0.775-μm band not found in the first row, the third row corresponds to all correlations with the 0.850-μm band not found in any of the preceding rows, and the last row corresponds to correlations at 1.25 μm. This enables us to generate a noise power spectrum by computing (A–B) × (C–D), as opposed to taking the auto-spectrum of (A–B) for the autocorrelations. For each filter we have two maps, so for each cross-correlation between bands we have four maps (label them A and B for the first filter, and C and D for the second). However, the noise power spectra for the cross-correlations are calculated slightly differently. 3, which accounts for all sources of noise and error, including map-making, calibration, detector noise, and cosmic variance. The error bars are 1 σ uncertainties which are calculated in a similar way as in Fig. Excess signal is detected in the cross-correlations. Ten cross-correlations between the HST bands. The clustering signal of low- z galaxies is more than an order of magnitude below the lower limit plotted here, thus we did not include a low- z component in our modelling. Fluctuation power spectra and the best-fit models with 1 σ error bounds for the model components are shown at 0.775 μm in b and 1.60 μm in c The dominant model contributors to the total power spectrum are DGL at low multipoles, or angular scales greater than a few arcmin, IHL at intermediate multipoles corresponding to angular scales of about an arcmin, and shot noise associated with faint low-redshift dwarf galaxies dominating the high multipoles or sub-arcmin angular scales. We show the upper limit (denoted by a downard facing arrow) of fluctuations generated by 6< z<8 galaxies as a dot-dashed line.
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At 1.25 and 1.6 μm, the best-fit high-redshift galaxy signal is shown as dashed lines. We show the best-fit model which makes use of four components: ( a) z >8 high-redshift galaxies ( b) intrahalo light (IHL) ( c) faint low-redshift galaxies and ( d) diffuse Galactic light. Thus the 1 σ uncertainties account for all sources of noise and error, including map-making, calibration, detector noise and cosmic variance associated with finite size of the survey. at each multipole, δC ℓ, described in equation 11. The error bars are calculated by adding in quadrature the errors from the beam transfer function, map-making transfer function and calibration errors, to the s.d. ( a) Multiwavelength auto power spectra of optical to near-infrared intensity fluctuations in the GOODS-South field using Hubble Space Telescope data (see Supplementary Methods for data selection details).