Upcoming LSST survey gives an unprecedented opportunity for studying populations of intrinsically faint objects using microlensing technique. Large field of view and aperture allow effective time-series observations of many stars in Galactic disk and bulge. Here, we combine Galactic models (for |b|<10 deg) and simulations of LSST observations to study how different observing strategies affect the number and properties of microlensing events detected by LSST. We predict that LSST will mostly observe long duration microlensing events due to the source stars with the averaged magnitude around 22 in r-band, rather than high-magnification events due to fainter source stars. In Galactic bulge fields, LSST should detect on the order of 400 microlensing events per square degree as compared to 15 in disk fields. Improving the cadence increases the number of detectable microlensing events, e.g., improving the cadence from 6 to 2 days approximately doubles the number of microlensing events throughout the Galaxy. According to the current LSST strategy, it will observe some fields 900 times during a 10-year survey with the average cadence of ~4-days (I) and other fields (mostly toward the Galactic disk) around 180 times during a 1-year survey only with the average 1-day cadence (II). We anticipate that the number of events corresponding to these strategies are 7900 and 34000, respectively. Toward similar lines of sight, LSST with the first observing strategy (I) will detect more and on average longer microlensing events than those observable with the second strategy. If LSST spends enough time observing near Galactic plane, then the large number of microlensing events will allow studying Galactic distribution of planets and finding isolated black holes among wealth of other science cases.
Maximizing Science in the Era of LSST, Stars Study Group Report: Rotation and Magnetic Activity in the Galactic Field Population and in Open Star Clusters
Rubin LSST observing strategies to maximize volume and uniformity coverage of Star Forming Regions in the Galactic Plane
在全天巡天时代，绘制银河系最年轻的恒星星族的完整地图是现代天体物理学中最具挑战性的目标之一。最年轻的恒星组成部分的特性是至关重要的，不仅对银河系结构的全球概览，银河系薄盘，其旋臂，但也为当地的研究。事实上，恒星形成区（SFR）的识别以及与它们形成的环境的比较，对于将它们置于周围巨大分子云的背景下以及理解与恒星和行星形成过程相关的未知物理机制也是至关重要的。在10年的观察中，Vera C. Rubin Legacy Survey of Space and Time（Rubin-LSST）将实现精致的光度深度，这将使我们能够显着扩展我们能够发现新SFR的体积，并扩大我们自己的银河系的详细知识领域。本文描述了一个度量，它估计了< 10 Myr and masses >Rubin LSST观测在5 σ星等显著性的GRI带中将探测到的年龄为t 0.3 M $_\odot$的年轻恒星的总数。我们采用最新的模拟Rubin-LSST调查策略来检查我们的指标结果，以评估不同的观察策略可能对我们的科学案例产生的影响。
