Evolution of the luminosity from the black-body (red points) and hard X-ray emitting, cooling flow (black points) spectral components over time. The shaded areas mark the SAS, Dip and Recovery phase using the same color code as in Fig. 1. A WLS fit to the luminosity of the optically thick (BB) component (dotted red line) indicates that its slope is different from zero at the 2.58σ level. We include Nu2 and Nu3 observations taken in 2024 and Obs7 taken in 2025, whose spectra arise from the optically thin portion of the boundary layer, i.e., the cooling flow. Dotted black lines mark the WLS fit to the L_CF evolution whose slope is different than zero at the 4.49σ level. The increase in its luminosity suggests that the accretion rate in the disk decreased over time, with the boundary layer becoming optically thinner and hotter.