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We estimate the local density field in redshift shells to a maximum redshift of   z = 0.3 , using photometric redshifts for the Two‐Micron All‐Sky Survey galaxy catalogue, matched to optical data from the SuperCOSMOS galaxy catalogue. This density‐field map is used to predict the integrated Sachs–Wolfe (ISW) cosmic microwave background (CMB) anisotropies that originate within the volume at   z  &lt; 0.3 . We investigate the impact of this estimated ISW foreground signal on large‐scale anomalies in the  Wilkinson Microwave Anisotropy Probe (WMAP)  CMB data. We find that removal of the foreground ISW signal from  WMAP  data reduces the significance of a number of reported large‐scale anomalies in the CMB, including the low quadrupole power and the apparent alignment between the CMB quadrupole and octopole.

An estimate of the local integrated Sachs–Wolfe signal and its impact on cosmic microwave background anomalies