The study identifies the peak of the WD cooling sequence luminosity function (LF) at m_F606W=30.1±0.2 and extends its analysis to fainter magnitudes. However, the completeness of the dataset at these faint magnitudes drops below 50%, as shown in Fig. 3c. This low completeness significantly limits the reliability of the observed star counts at the faint end of the WD CS, potentially impacting conclusions about the termination of the CS and the age distribution of the cluster. Could the authors elaborate on how the completeness correction was validated, especially at these faint magnitudes? Additionally, were alternative approaches, such as deeper artificial star experiments or complementary observations with other instruments (e.g., JWST), considered to corroborate the findings at the faint end?
