Technology has advanced to the point that it is possible to image the entire sky every night and process the data in real time. The sky is hardly static: many interesting phenomena occur, including variable stationary objects such as stars or QSOs, transient stationary objects such as supernovae or M dwarf flares, and moving objects such as asteroids and the stars themselves. Funded by NASA, we have designed and built a sky survey system for the purpose of finding dangerous near-Earth asteroids (NEAs). This system, the "Asteroid Terrestrial-impact Last Alert System" (ATLAS), has been optimized to produce the best survey capability per unit cost, and therefore is an efficient and competitive system for finding potentially hazardous asteroids (PHAs) but also for tracking variables and finding transients. While carrying out its NASA mission, ATLAS now discovers more bright ($m < 19$) supernovae candidates than any ground based survey, frequently detecting very young explosions due to its 2 day cadence. ATLAS discovered the afterglow of a gamma-ray burst independent of the high energy trigger and has released a variable star catalogue of 5$\times10^{6}$ sources. This, the first of a series of articles describing ATLAS, is devoted to the design and performance of the ATLAS system. Subsequent articles will describe in more detail the software, the survey strategy, ATLAS-derived NEA population statistics, transient detections, and the first data release of variable stars and transient lightcurves.
小行星撞击地球最后警报系统（ATLAS）每天晚上观察大部分天空，寻找危险的小行星。它的数据也用于搜索光度变化，其中对变化的敏感性受到光度精度的限制。由于每个曝光角到角跨越7.6度，超过0.01 mag的大气透明度变化是常见的，并且0.01 mag测光不能通过使用恒定的平场校准图像来实现。因此，我们已经收集了一个全天空的参考目录约10亿颗恒星，以m~19从各种来源，以校准每个曝光的天体测量和测光。盖亚DR 2是ATLAS Refcat 2的天体测量来源。g，r，i，z测光的来源包括Pan-STARRS DR 1、ATLAS Pathfinder测光计划、ATLAS重新展平的APASS数据、SkyMapper DR 1、APASS DR 9、Tycho-2星表和Yale Bright Star Catalog。我们试图使这个目录至少99%完整到m<19，包括天空中最亮的恒星。我们相信，系统误差不大于5毫等RMS，虽然误差是大到20毫等的小补丁附近的银道。
Optimization of the Observing Cadence for the Rubin Observatory Legacy Survey of Space and Time: a pioneering process of community-focused experimental design
Minute-cadence Observations of the LAMOST Fields with the TMTS: I. Methodology of Detecting Short-period Variables and Results from the first-year Survey
The Herschel-ATLAS Data Release 2, Paper I. Submillimeter and Far-infrared Images of the South and North Galactic Poles: The Largest Herschel Survey of the Extragalactic Sky
Adaptive elliptical aperture photometry: a software package for high-cadence ground-based photometry. I. Application to rapid oscillators observed from SAAO
Microlensify: a Transformer Based Machine Learning Classifier for Microlensing Events Trained on TESS Light Curves
Institute for Advanced Studies in Basic Sciences (IASBS)（基础科学高等研究院）；Lehigh University（利哈伊大学）；University of Virginia（弗吉尼亚大学）；Isfahan University of Technology（伊斯法罕理工大学）；University of Delaware（特拉华大学）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森天体物理中心）
A comprehensive simulation framework for multi-modal kilonova observations from all-sky surveys
University of Minnesota（明尼苏达大学）；Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）；Florida State University（佛罗里达州立大学）；University of California, Santa Cruz（加州大学圣克鲁兹分校）；University of Delaware（特拉华大学）；University of Virginia（弗吉尼亚大学）
The Impact of Observing Strategy on Reliable Classification of Standard Candle Stars: Detection of Amplitude, Period, and Phase Modulation (Blazhko Effect) of RR Lyrae Stars with LSST
维拉C。鲁宾天文台将进行其时空遗产巡天（LSST），单次曝光深度为$r{\sim}24.7$，预期基线为10年，不仅可以访问银河系的旧晕更深，而且基线更长，节奏更好，例如PS1 3 $π$（Chambers et al. 2016）。这将使LSST成为研究变星（如RR型天琴座星（RRL））的理想选择。在这里，我们解决了LSST的观察策略优化问题，因为调查足迹定义，单次访问暴露时间以及不同过滤器中重复访问的节奏尚未最终确定。我们提出了用于评估不同观测策略对标准烛光变星的可靠探测性和分类的影响的指标，包括RR天琴座星的振幅周期检测，相位调制效应，所谓的Blazhko效应（Blazhko 1907，Kollath et al. 2011），通过评估模拟潜在巡天设计的指标。到目前为止，由于典型的全天空调查的深度和节奏，几乎不可能在更大的样本上研究这种影响。在中等长度的基线上具有相对较少观测的全天巡天仅允许拟合相位折叠RRL光变曲线，从而在整个巡天长度上积分并隐藏关于巡天期间可能的周期或相位调制的任何信息。另一方面，以节奏探测轻微变化的光变曲线的测量通常具有相对较小的足迹。然而，LSST的调查策略将允许研究变星的方式，使人口研究成为可能。
The Southern-sky MWA Rapid Two-metre (SMART) pulsar survey--IV. Survey update and an atlas of 205 non-recycled southern pulsars
International Centre for Radio Astronomy Research, Curtin University（国际射电天文研究中心，科廷大学）；Australian SKA Regional Centre (AusSRC), Curtin University（澳大利亚SKA区域中心（AusSRC），科廷大学）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；CSIRO Astronomy and Space Science（CSIRO天文学与空间科学）；National Radio Astronomy Observatory（美国国家射电天文台）；Manly Astrophysics（曼利天体物理学）
Uniform Rolling: An LSST Observing Cadence Offering Sufficient Survey Uniformity for Comprehensive Cosmological Analysis
Imperial College London（帝国理工学院）；Argonne National Laboratory（阿贡国家实验室）；Stanford University（斯坦福大学）；SLAC National Accelerator Laboratory（斯坦福直线加速器中心）；Rutgers, the State University of New Jersey（新泽西州立罗格斯大学）；University College London（伦敦大学学院）；University of Toronto（多伦多大学）；Duke University（杜克大学）；University of the Western Cape（西开普敦大学）；Carnegie Mellon University（卡内基梅隆大学）；University of Pittsburgh（匹兹堡大学）；University of Cambridge（剑桥大学）；Stockholm University（斯德哥尔摩大学）；University of Washington（华盛顿大学）
Deep multi-survey classification of variable stars
Pontificia Universidad Católica de Chile（智利天主教大学）；Millennium Institute of Astrophysics（千禧天体物理研究所）；Institute of Applied Computational Science (IACS), Harvard（哈佛大学应用计算科学研究所（IACS））
