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tokens: is hotter. Consequently these two effects increase the significance of the CS. The vertical red dashdotted line indicates the f sky of the Planck Common Field mask. 3.4 The ISW for the coldest spots The ISW contribution to the coldest spots in simulations was measured and is shown in Fig. 5 . Here, we display the mean and 1 contours for all the full-sky minima and the most extreme 3percent (which approximately corresponds to the CSs p-value). The profiles are poorly constrained and very similar, with the more extreme case tending to be slightly more negative. The result illustrates that it is very likely that the ISW plays a minor role in the CS profile: 10percent of the full profile. The reconstructed ISW profiles (Nadathur etal. 2014 ; Rassat etal. 2014 ; Finelli etal. 2016 ; Planck Collaboration XXI 2016c ) appear to be consistent with the predicted ISW shown in Fig. 5 . The presence of prominant voids in the LOS (see Szapudi etal. 2015 ; Kovcs Garca-Bellido 2016 ) are therefore precisely what we would expect from CDM. Figure 5. The 1 contours of the ISW of all the full-sky minima are shown in blue. The most extreme 3percent are indicated by the grey hatched area. The mean for all the coldest spots and the most extreme 3percent are indicated by the blue and grey dashed lines, respectively. The ISW in either case is not very well constrained and consistent with zero but, on average, appears to contribute 10percent to the minimas profiles. 3.5 Dependence on angular scale Up to this point, we have used a preselected angular scale, R 5, where the CS was measured to be most significant by Planck Collaboration XVI ( 2016b ). However, our conclusions for the CS significance may not necessarily hold true for other angular scales. To test this, R is varied between 4 and 7, roughly equaling the range of R over which Zhang Huterer ( 2010 ) found the CS to be significant. The same procedure is carried out as before except with a smaller number of realizations (10000). In Table 1 , we summarize these results. The probability, , is roughly equal to the fraction of unmasked pixels of the effective mask. However, is found to be 0.85 for the angular scales considered. When the cut-sky significance 2 the probability is even higher (0.93). This makes it appropriate to compare the CS to full-sky minima in simulations where it is 2 for 4 R 7. Combined with previous studies (e.g. Vielva etal. 2004 ) means the CS is 2 for all angular scales. Table 1. The probability that the full-sky and cut-sky minima (Cold Spot) are equivalent for any and for the CSs is indicated by and , respectively, for each angular scale R . The significance of the CS is shown in comparison to the cut-sky and full-sky minima in CMB realizations. For each value of R (except R 5, where 100000 realization were previously made) 10000 CMB realizations were simulated. 4 CONCLUSIONS We measure the cut-sky and full-sky minima (Cold Spot) in 100000 simulations using the Planck Common Field mask,