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brighter than G ∼ 20.7 mag, where G is the Gaia passband covering from 330 to 1050 nm), and not yet (all) saturated with the LSST. In a synergistic and complemental approach, all our selected targets contain red giant branch (RGB) stars which are within the reach of Gaia (e.g.
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In our joint project we propose to observe with the LSST six Local Group stellar systems of different morphological type, which are located from ∼30 to ∼400 kpc in distance from us. Observing strategy as to meet the goals of both projects. Synergy: from pulsating stars and star formation history to WDs” PI G.Ĭlementini, and “RR Lyrae, Cepheids and Luminous Blue Variables to constrain This is a joint proposal of the LSST projects:“The Gaia-LSST Our ultimate goal is: i) to provide a complete picture of these nearby stellar systems all the way through to their periphery, and: ii) to directly link and cross-calibrate theĪ valuable by-product will be the derivation, for the first time, of period-luminosity relations based on statistically significant samples of delta Scuti and SX Phoenicis stars, in different environments. Iv) search for tidal streams which are supposed to connect some of these systems and v) study their Star Formation Histories (SFHs) over an unprecedented large fraction of their bodies. Using variable stars of different type/parent stellar population and the Tip of the Red Giant Branch (TRGB) iii) map their 3D structures all the way through to the farther periphery of their halos I) trace their different stellar generations over the large spatial extension and magnitude depth allowed by the LSST ii) measure their distances Instability strip (namely: RR Lyrae stars, Cepheids of different types, SX Phoenicis andĭelta Scuti stars) and Long Period Variables (LPVs), along with the Color Magnitude Diagram (CMD) of the resolved stellar populations in these 6 systems to: Specifically, we plan to use pulsating variable stars populating the whole classical In five of them we will reachĪt least one magnitude below the TO of the oldest stellar component (t ≥ 10 Gyr) with the LSST. In a synergistic and complemental approach, we have selected targets that host red giant branch (RGB) stars which are within the reach of Gaia and not yet (all) saturated with the LSST. The adopted stellar tracers will be mainly red giants, pulsating variable stars of different types, and turn-off (TO) main sequence (MS) stars. In/around six Local Group stellar systems of different morphological type that are located from ∼30 to ∼400 kpc in distance from us. We provide example uses of these metrics and discuss some implications based on these metrics for optimization of the LSST survey for observations of stellar variables and transients.This project aims at exploiting the wide-field and limiting-magnitude capabilities of the LSST to fully characterise the resolved stellar populations The third metric provides a way to quantify the range of stellar parameters in the stellar populations that LSST will probe. Two of the metrics quantify the ability of LSST to detect non-periodic and/or non-recurring transient events, and the ability of LSST to reliably measure periodic signals of various timescales. In this paper we present three such metrics built on the LSST Metric Analysis Framework (MAF) model (Jones et al. In order to maximize the LSST science yield for a broad array of transient stellar phenomena, it is necessary to optimize the survey cadence, coverage, and depth via quantitative metrics that are specifically designed to characterize the time-domain behavior of various types of stellar transients.
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The Large Synoptic Survey Telescope (LSST) will be the largest time-domain photometric survey ever.