## 3 Experimental Methods and Results
For each image, the average of the differences between measured magnitude and calibrated was computed and then used to correct the debris measured magnitude into calibrated magnitude. This result is shown in Table 3 as 'Calibrated magnitude'. The magnitude of each source in each image was computed by placing the stars inside circles and the debris/streaks inside rectangles and counting the flux measured in every selected element. The background flux was also computed in each image and extracted from the measured flux of every element before converting it into the logarithmic magnitude scale. \begin{table}
\begin{tabular}{l c c c c c} \hline  & \multicolumn{4}{c}{**Stars**} & \multicolumn{2}{c}{**Observed Object**} \\ \hline Object & 30 Vul & 29 Vul & 22 Vul & 25 Vul & Starlink-1346 \\ \hline Measured magnitude & \(-\)4.506 & \(-\)4.1944 & \(-\)3.9902 & \(-\)3.8428 & \(-\)3.9606 \\ \hline Real magnitude & 4.91 & 4.82 & 5.15 & 5.54 & \\ \hline Calibration constant & 8.96 & 9.01 & 9.14 & 9.38 & Mean: 9.08 \\ \hline \multicolumn{6}{c}{Calibrated magnitude: 5.12} \\ \hline Object & 56 Cyg & Ruchba & 51 Cyg & 46 Cyg & Starlink-3601 \\ \hline Measured magnitude & \(-\)3.9874 & \(-\)4.4262 & \(-\)3.8194 & \(-\)3.955 & \(-\)2.6156 \\ \hline Real magnitude & 5.04 & 2.68 & 5.39 & 5.45 & \\ \hline Calibration constant & 9.03 & 7.11 & 9.21 & 9.35 & Mean: 9.12 \\ \hline \multicolumn{6}{c}{Calibrated magnitude: 6.50} \\ \hline Object & 62 Cyg & 57 Cyg & 60 Cyg & 58 Cyg & Starlink-2602 \\ \hline Measured magnitude & \(-\)5.2612 & \(-\)4.6111 & \(-\)4.0145 & \(-\)4.9218 & \(-\)2.1060 \\ \hline Real magnitude & 3.7 & 4.76 & 5.37 & 3.93 & \\ \hline Calibration constant & 8.96 & 9.37 & 9.38 & 8.85 & Mean: 9.17 \\ \hline \end{tabular}
\end{table} 
Table 3: Measured magnitudes for the observed objects. From a theoretical approach, the predicted camera's limiting magnitude was 11.4 for an integration time of 3 s (see Section 2.3). Analysing our images, we were able to detect stars with magnitudes from 10.0 to 10.6 in all of them. Since these measured magnitudes are closer to the \(SNR=5\) limit, they should have a magnitude error of \(\Delta m\ \approx\frac{1.0887}{SNR}=0.2\). Therefore, our test results were in a rather good agreement with the theoretical estimation. Also, for typical observations at an elevation above 30 deg, the atmosphere absorbs roughly 0.2 magnitudes to 0.3 magnitudes, meaning that our camera on the ground would not detect objects fainter than 11.1-11.2 with an integration time of 3 s. Since our tests were made with a ground-based configuration, we also dealt with the unavoidable issue of the direct link between the sky trailing rates and the orbital distance of the objects moving at each one of those rates. In a space-based configuration, orbiting the Earth, that link is far more complex, allowing even the detection of orbit-crossing and almost co-orbiting debris of the under-catalogued size-scale from 10 cm up to 110 km of distance, at a pessimistic phase angle of 120 deg, and up to 320 km distance, at an optimistic phase angle of 20 deg. * Starlink satellites size estimation  
With the Starlinks magnitude values and observation data, it was possible to compute an approximate size for each satellite in every image using (10), considering the average albedo of 0.175 and spherical geometry. The orbit information of Starlinks in the TLE (Two Line Element) format is public and can be requested at the CelesTrack website [31]. This data is necessary for this calculation, which is why the Starlinks were chosen among the other observed objects.