## 5 Conclusions
In particular, the use of a correct and working likelihood for signal gluing, with or without the presence of photon counting baseline ringing and the incorporation of photon counting efficiency, background fitting, the correct introduction of the PMT excess noise, and the correct retrieval of fit parameter uncertainties, using the correct Poissonian variance from Garwood (1998), goes much beyond the method developed by Veberic (1999). Also novel is the use of robust statistics to obtain a reliable criterion for the number of time slices after the signal used for background estimation, as well as the use of precalculated molecular fit \(\chi^{2}\)'s for layer detection, in addition to the novel dynamic re-binning algorithm. The findings obtained from these tests will be valuable for the upgraded final version of the BRL, which is designed to become a reliable tool for accurate atmospheric monitoring of the CTAO, and thus ensure the quality of gamma-ray observations and the overall scientific output of the observatory. Conceptualization, R.G., M.D., M.G. ; methodology, O.B., A.C.-O., M.D., M.G., R.G. ; software, P.J.B.-R., A.C.-O., R.G., M.G. ; formal analysis, P.J.B.-R., A.C.-O., M.D., M.G., R.G. ; data acquisition, O.B., P.G.C., A.C.-O., S.M.C., M.D., L.F., M.G., R.G., C.M., M.M., S.S., S.U., M.Z. ; hardware contribution, O.B., M.D., L.F., M.G., M.M., S.S., M.Z. ; investigation, O.B., P.G.C., A.C.-O., M.D., L.F., M.G., R.G., D.K., M.M., S.S., U.M.Z. ; resources, O.B., M.D., L.F., M.G., M.M., S.S., M.Z. ; data curation, P.J.B.-R., M.G., R.G., M.Z. ; writing--original draft preparation, P.J.B.-R., A.C.-O., M.D., M.G., R.G., M.Z. ; writing--review and editing, all authors; supervision, O.B., M.D., M.G., M.M., S.S.; project administration, O.B., M.D., L.F., M.G., M.M. ; funding acquisition, O.B., M.D., L.F., M.G., M.M., S.S. All authors have read and agreed to the published version of the manuscript. This project has received funding from the European Union's Horizon Europe Research and Innovation Programme under Grant Agreement No 10131928; by the Spanish grants PID2022-139117 NB-C41 and PID2022-139117 NB-C43, funded by MCIN/AEI/10.13039/501100011033/FEDER, UE, the Departament de Recerca i Universitats de la Generalitat de Catalunya (grant SGR2021 00607), and by \"ERDF A way of making Europe\", the CERCA program of the Generalitat de Catalunya, and the European Union NextGenerationEU/PTRTR. In Slovenia, it was funded by the Slovenian Research and Innovation Agency, grants P1-0031, J1-3011, and I0-E018. M.D. acknowledges funds from the 2012 \"Bando Giovani Studios\" of the University of Padova. R.Gr. acknowledges funding from the FSE under the program Ayudas predoctorales of the Ministerio de Ciencia e Innovacion PRE2020-093561. The data supporting the conclusions of this article will be made available by the authors on request. A public image of the LPP v1.0.0 can be found at [[https://gitlab.cta-observatory.org/cta-array-elements/ccf/lpp_deployment](https://gitlab.cta-observatory.org/cta-array-elements/ccf/lpp_deployment)]([https://gitlab.cta-observatory.org/cta-array-elements/ccf/lpp_deployment](https://gitlab.cta-observatory.org/cta-array-elements/ccf/lpp_deployment)), accessed on 18 May 2025. To obtain access to the source code, please contact bauza@ieec.cat or markus.gaug@uab.cat. This work would have been impossible without the support of our colleagues from the MAGIC and LST collaboration and the CTAO Consortium, which we gratefully acknowledge. We thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos on La Palma. We also thank the funding agencies and institutions mentioned in the above section (Funding) for the financial support. Author Camilla Maggio was employed by the company CAEN Tools for Discovery S.p.A solely during the editing of this manuscript. Author Paolo G. Calisse is employed by Cherenkov Telescope Array Observatory gGmbH, (CTAO gGmbH).