## 5 Results  
The process of manual analysis of cold microtraps using Lunar QuickMap was very long and tedious. Several dozen places were analyzed, of which only a few were selected for further detailed analysis. Places were marked with a combination of the letter B and subsequent numbers. The following sections present the results for each of them. Table 1 summarizes the results for all five cold microtraps analyzed. Table 1 summarizes the results for five selected cold microtraps for which a detailed analysis was performed using Lunar QuickMap. The location marked B-1 is a crater with coordinates (\(-\)88.20990; 305.92639). You can choose an access road to a permanently shaded area with a slope angle of no more than 23\({}^{\circ}\). It contains deposits of water, CO\({}_{2}\), iron, and thorium. Does not contain titanium deposits. The presence of iron is important because metallic raw materials will be needed to build bases. The location marked B-5 is a crater with coordinates (\(-\)89.12808; 273.21226). You can choose an access road to a permanently  
shaded area for which the slope angle will not exceed 25\({}^{\circ}\), which is a slightly worse result than for site B-1. However, it contains more water deposits than site B-5, as well as deposits of CO\({}_{2}\), iron, and thorium. Like site B-1, site B-5 does not contain titanium deposits. With the data from Table 1, it is possible to estimate the value of the deposits contained therein. These estimates will be subject to a large error, because, as mentioned earlier, data obtained remotely from satellites provide information about probable deposits and should be confirmed by in situ research (e.g., drilling). Moreover, the information obtained concerns only the surface layer and larger amounts of deposits of a given raw material may lie deeper (this may be especially the case for water ice deposits), just as the deposits may turn out to be smaller than estimated. Therefore, assessing the thickness of the deposit-rich layer is a key issue when estimating deposits. Bearing in mind that this parameter will be subject to a large error, the thickness of this layer was conservatively assumed to be:  
* 1 cm--pessimistic scenario;
* 5 cm--nominal scenario;
* 1 m--optimistic scenario. The analysis was limited only to permanently shaded areas (PSR), where the probability of deposits is highest. The average regolith density value was assumed to be 1 g/cm\({}^{3}\), which is a great simplification. Having information about the area of the permanently shaded area, the thickness of the layer rich in deposits, and the density of the regolith, the mass of the material contained in this layer was determined. Taking into account the coefficients (wt%) of the content of individual raw materials given in Table 1, their estimated mass in the mentioned 1 cm thick layer was determined. A similar procedure was carried out for CO\({}_{2}\) deposits, assuming a conservative concentration value of 1000 ppm for places where the presence of CO\({}_{2}\) was detected and 0 ppm for places where no CO\({}_{2}\) was detected. When adopting these values, it was taken into account that the CO\({}_{2}\) concentration [45] in the lunar water ice detected by the LCROSS probe was 5000 ppm. The CO\({}_{2}\) concentration values given in Table 1 expressed in units [log10 kg/m\({}^{2}\)/Gyr] are highly imprecise and lead, for cold microtraps B-1 and B-5, to calculations giving astronomical CO\({}_{2}\) contents,