A Search for Extraterrestrial Life (SETI), based on the possibility of interstellar communication via laser signals, is being designed to extend the search into the near-infrared spectral region (Wright et al, this conference). The dedicated near-infrared (900 to 1700 nm) instrument takes advantage of a new generation of avalanche photodiodes (APD), based on internal discrete amplification. These discrete APD (DAPD) detectors have a high speed response ($>$ 1 GHz) and gain comparable to photomultiplier tubes, while also achieving significantly lower noise than previous APDs. We are investigating the use of DAPD detectors in this new astronomical instrument for a SETI search and transient source observations. We investigated experimentally the advantages of using a multiple detector device operating in parallel to remove spurious signals. We present the detector characterization and performance of the instrument in terms of false positive detection rates both theoretically and empirically through lab measurements. We discuss the required criteria that will be needed for laser light pulse detection in our experiment. These criteria are defined to optimize the trade between high detection efficiency and low false positive coincident signals, which can be produced by detector dark noise, background light, cosmic rays, and astronomical sources. We investigate experimentally how false coincidence rates depend on the number of detectors in parallel, and on the signal pulse height and width. We also look into the corresponding threshold to each of the signals to optimize the sensitivity while also reducing the false coincidence rates. Lastly, we discuss the analytical solution used to predict the probability of laser pulse detection with multiple detectors.
PANOSETI（Pulsed All-Sky Near-Infrared Optical Search for Extra Terrestrial Intelligence）是一个专门的SETI（Search for Extra Terrestrial Intelligence）天文台，旨在观察4，441平方英尺的空间。°的来寻找纳秒到毫秒的瞬态事件。该实验将有一个双天文台系统，共有90个相同的0.48米光学望远镜，每个都有99平方度的视野。这两个观测站将相隔1公里，以帮助消除误报并记录明确的信号。我们讨论了望远镜模块的整体机械设计，其中包括菲涅耳透镜外壳，快门，三个挡板，32 x32阵列的滨松多光子像素计数（MPPC）探测器，驻留在一个线性阶段的聚焦。每个望远镜模块将被安置在一个三角形的第三镶嵌频率测地线圆顶，有能力有方向调整，以纠正制造公差和天体测量对准第二个天文台网站。每个观测站将有一个围栏来保护实验，以及一个观测室用于操作和电子设备。我们将审查测地圆顶和机械望远镜附件的总体设计，以及总体布线和天文台基础设施布局。
LoFreq-SETI: A Low-Frequency Technosignature Search Pipeline for the LWA Swarm
University of New Mexico（新墨西哥大学）；University of Washington（华盛顿大学）；SETI Institute（SETI研究所）；Berkeley SETI Research Center, University of California, Berkeley（加州大学伯克利分校伯克利SETI研究中心）；National Radio Astronomy Observatory（国家射电天文台）
A deep-learning search for technosignatures of 820 nearby stars
University of Toronto（多伦多大学）；Dunlap Institute for Astronomy & Astrophysics（邓拉普天文与天体物理研究所）；University of California, Berkeley（加州大学伯克利分校）；SETI Institute（搜寻地外文明研究所）；The University of Manchester（曼彻斯特大学）；University of Malta（马耳他大学）
