Triggers, data flow and the synchronization between the Auger surface detector and the AMIGA underground muon counters

Z. Szadkowski
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引用次数: 7

Abstract

The aim of the AMIGA project (Auger Muons and Infill for the Ground Array) is an investigation of Extensive Air Showers at energies lower than by standard Auger array, where the transition from galactic to extragalactic sources is expected. The Auger array is enlarged by a relatively small dedicated area of surface detectors with nearby buried underground muon counters at half or less the standard 1.5 km grid. Lowering the Auger energy threshold by more than one order of magnitude allows a precise measurement of the cosmic ray spectrum in the very interesting regions of the second knee and the ankle. The paper describes the working principle of the Master/Slave (standard Auger surface detector/the underground muon counters) synchronous data acquisition, general triggering and the extraction of data corresponding to the real events from underground storage buffers applied in two prototypes: A) with 12.5 ns resolution (80 MHz) built from 4 segments: standard Auger Front End Board (FEB) and Surface Single Board Computer (SSBC) (on the surface) and the Digital Board with the FPGA and the Microcontroller Board (underground), B) with 4-times higher: 3.125 ns resolution (320 MHz) built with two segments only: new surface Front End Board supported by the NIOS® processor and CycloneIII™ Starter Kit board underground, working also with NIOS® virtual processor, which replaces the external TI µC, which in meantime became obsolete. The system with the NIOS® processors can remotely modify and update: the AHDL firmware creating the hardware FPGA net structure responsible for the fast DAQ, the internal structure of the NIOS® (resources and peripherals) and the NIOS® firmware (C code) responsible for software data management. With the standard µC, the µC firmware was fixed and could not be updated remotely. The 80 MHz prototype passed laboratory tests with real scintillators. The 320 MHz prototype (still being optimized) is considered as the ultimate AMIGA design.
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触发器,数据流和俄歇表面探测器和AMIGA地下μ子计数器之间的同步
AMIGA项目(俄歇μ子和地面阵列的填充)的目标是在能量低于标准俄歇阵列的情况下对广泛的空气阵雨进行调查,在那里,从银河系到星系外的源的过渡有望实现。俄歇阵列被一个相对较小的地面探测器专用区域扩大,附近埋在地下的μ子计数器在标准1.5公里网格的一半或更少。将俄歇能量阈值降低一个数量级以上,可以精确测量第二个膝盖和脚踝非常有趣的区域的宇宙射线光谱。本文介绍了主/从(标准俄采表面探测器/地下μ子计数器)同步数据采集、一般触发和从地下存储缓冲区中提取与真实事件相对应的数据的工作原理,应用于两种样机:A) 12.5 ns分辨率(80 MHz),由4段组成:标准的Auger前端板(FEB)和Surface单板计算机(SSBC)(在表面上)以及带有FPGA和微控制器板(地下)的数字板(B),具有4倍高:3.125 ns分辨率(320 MHz),仅由两个部分构建:新的表面前端板由NIOS®处理器和CycloneIII™地下Starter Kit板支持,还与NIOS®虚拟处理器一起工作,取代了外部TIµC,同时也过时了。采用NIOS®处理器的系统可以远程修改和更新:创建硬件FPGA网络结构的AHDL固件负责快速DAQ, NIOS®的内部结构(资源和外设)和NIOS®固件(C代码)负责软件数据管理。使用标准的µC,µC固件是固定的,无法远程更新。80兆赫的原型机通过了真实闪烁体的实验室测试。320mhz的原型(仍在优化中)被认为是最终的AMIGA设计。
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