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

尘埃被认为是宇宙最重要的组成部分之一。我们自己的太阳系是由46亿年前的星际尘埃云形成的。尘埃-天文学分析星际尘埃、彗星尘埃和小行星尘埃的性质，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尘埃颗粒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。目前研究的重点是用于分析地球和月球表面尘埃的探测器，以实现悬浮尘埃的精确测量。在内部，尘埃探测器由多个传感器组成，其中基于影响电荷的轨迹探测器是最重要的传感器之一。简化后，该探测器可以被认为是由几个孤立的线电极组成的多个栅格。每个电极连接到电荷灵敏放大器(CSA)。通过计算紫外光带电粒子对电极中的瞬变电荷的影响，可以计算出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。研究潜在的措施以达到CSA中的这两项要求是本提案的主要目标。由于粒子的速度变化很大，建议定义了三个频带，范围从7赫兹到50兆赫。对于更高的频率，从10 kHz开始，打算对系统进行全系统的分析性描述和优化。进一步的研究包括设计可以与不同电容值的探测器匹配的放大器。同时，最高工作频率将从10兆赫增加到50兆赫。特别注意从7赫兹到300千赫的频率范围，它代表了粒子在行星表面上的运动。该提案的主要焦点之一是改善闪烁噪声放大器在这些频率下的体验。虽然传统的改善低频噪声的方法在CSA中不起作用，但通过体开关进行开关偏置似乎是降低CSA中这种噪声的一种潜在措施。因此，计划中的项目旨在将这项技术应用于行星表面的低频尘埃探测器。如果成功，据作者所知，这将是有源闪烁噪声抑制在CSA中的第一次成功应用。

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.