Extremely low noise integrated charge sensitive amplifiers for electrostatic influence based detectors for cosmic and terrestrial dust

尘埃被认为是宇宙中最重要的组成部分之一。我们的太阳系是由46亿年前的星际尘埃云形成的。尘埃天文学分析星际，彗星和小行星尘埃的特性，以更好地了解太阳系形成期间的条件。通过分析尘埃颗粒的化学成分和轨迹，未来的尘埃望远镜将提供有关粒子起源的前所未有的细节，并将有助于在太空中寻找有机分子。目前的研究主要集中在探测器上，用于分析地球和月球表面的尘埃，实现对悬浮尘埃的精确测量，尘埃探测器内部由多个传感器组成，其中基于影响电荷的磁阻探测器是最重要的传感器之一。简单地说，这种探测器可以被认为是由几个隔离的线电极组成的许多网格。每个电极连接到电荷敏感放大器（CSA）。通过评估由紫外光带电粒子在电极中影响的瞬态电荷，可以计算粒子的飞行速度和方向。设计这些探测器的最大挑战是粒子的电荷非常低，未来的尘埃探测器从35个基本电荷开始。此外，新的粉尘探测器项目需要大幅增加带宽。研究在CSA中达到这两项要求的潜在措施是本提案的主要目标。由于粒子的速度变化很大，该提案定义了覆盖7 Hz至50 MHz范围的三个频带。对于更高的频率，从10 kHz开始，系统范围内的分析描述和系统的优化。研究的另一点包括设计放大器，其可以与具有不同电容值的检测器相匹配。与此同时，最大工作频率将从10 MHz增加到50 MHz。特别注意的是，从7赫兹到300千赫的频率范围，代表了行星表面上移动的粒子。该提案的主要焦点之一是改善这些频率下的闪烁噪声放大器体验。虽然经典的方法，以改善低频噪声不工作的CSA，开关偏置通过批量开关似乎是一个潜在的措施，以减少这种噪声的CSA。因此，计划中的项目旨在将该技术应用于行星表面的低频尘埃探测器。如果成功的话，据作者所知，这将是第一次成功的应用主动闪烁噪声抑制CSA。

Dust is considered to be one of the most important components of the Universe. Our own solar system was created from what used to be an interstellar dust cloud 4.6 billion years ago. Dust-astronomy analyzes the properties of interstellar, cometary and asteroidal dust to gain a better understanding of the conditions during the creation of our solar system. By analyzing both the chemical composition and the trajectory of dust grains, future dust telescopes will deliver unprecedented details on the origin of the particles and will aid the search for organic molecules in space. Concurrently research focuses on detectors to analyze dust on Earth and on lunar surfaces, ena-bling the precise measurement of suspended dust.Internally the dust detector consists of multiple sensors, of which the influence-charge based trajectory-detector is one of the most important ones. Simplified, this detector can be considered as a number of grids consisting of several isolated wire-electrodes. Each electrode is connected to a charge sensitive amplifier (CSA). By evaluating the transient charges influenced in the electrodes by UV-light charged particles the speed and the direction of flight of the particle can be calculated. The biggest challenge in designing these detectors is presented by the very low charge of the particles, starting at 35 elementary charges for future dust detectors. Additionally, new dust detector projects demand heavily increased bandwidths. Researching potential measures to reach both of these requirements in CSAs presents the primary goal of this proposal. Due to the large variety of the speed of the particles the proposal defines three frequency bands covering the range form 7 Hz to 50 MHz. For higher frequencies, starting at 10 kHz, a system-wide analytic description and optimization of the system is intended. A further point of research consists of designing amplifiers, which can be matched to detectors with different capacitance values. At the same time the maximum operating frequency is meant to increase from 10 MHz to 50 MHz. Special attention is given to the frequency range that spans from 7 Hz to 300 kHz and represents particles moving on planetary surfaces. One of the main focus points of the proposal consists of improving the flicker noise amplifiers experience at these frequencies. While classic methods to improve the low frequency noise do not work in CSAs, Switched Biasing via bulk switching appears to be a potential measure to reduce this noise in CSAs. Therefore the planned project aims at em-ploying this technique in low frequency dust detectors for planetary surfaces. If successful, accord-ing to the knowledge of the authors, this would be the first successful application of active flicker noise suppression in CSAs.