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We re-analyse the cosmic microwave background (CMB) Cold Spot (CS) anomalywith particular focus on understanding the bias a mask (contaminated byGalactic and point sources) may introduce. We measure the coldest spot, foundby applying the Spherical Mexican Hat Wavelet transform on 100 000 cut-sky(masked) and full-sky CMB simulated maps. The CS itself is barely affected bythe mask; we estimate a 94 per cent probability that the CS is the full-skytemperature minimum. However, approximately 48 per cent (masked fraction of themask) of full-sky minima are obscured by the mask. Since the observed minimaare slightly hotter than the full-sky ensemble of minima, a cut-sky analysiswould have found the CS to be significant at approximately 2.2 sigma with awavelet angular scale of R = 5 degrees. None the less, comparisons to full-skyminima show the CS significance to be only approximately 1.9 sigma and lessthan 2 sigma for all R. The CS on the last scattering surface may be hotter dueto the integrated Sachs-Wolfe effect in the line of sight. However, oursimulations show that this on average only approximately 10 per cent (about 10micro K but consistent with zero) of the CS temperature profile. This isconsistent with Lambda and cold dark matter reconstructions of this effectbased on observed line-of-sight voids.

The cosmic microwave background Cold Spot anomaly: the impact of sky masking and the expected contribution from the Integrated Sachs-Wolfe effect