Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies

Abstract This investigation is mainly focused on the LSST Survey Strategy Optimization process, a bottom-up approach that turned out to be quite effective in involving scientific community definition of observing strategy. We are interested using radial variables (RR Lyrae, classical Cepheids, long-period variables) as stellar tracers and distance indicators, we developed new tool called PulsationStarRecovery quantify recovery light-curve period amplitude from an LSST-simulated time series. The outputs this code pulsation parameters (period, amplitude, mean magnitude) together with quantitative information concerning difference between shape light curve template curves. Furthermore, apply newborn metric simulate observations different types pulsating stars hosted by selected massive systems (19 Local Group dwarf galaxies Large Magellanic Cloud) show how changes according variable-star type. exercise essential understand potential field since excellent necessary optimize use predicted period–luminosity, period–amplitude, color–color relations constrain cosmic scale metallicity distribution function populations.