Characterisation of low power readout electronics for a UV microchannel plate detector with cross-strip readout

Pfeifer, M.; Barnstedt, J.; Diebold, S.; Hermanutz, S.; Kalkuhl, C.; Kappelmann, N.; Schanz, T.; Schütze, B.; Werner, K.

doi:10.1117/12.2054742

Cited by 4 publications

(4 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Most parts of our detector electronics have been designed to take advantage of the capabilities of the 128-channel charge amplifying BEETLE chip. Details on its application can be found in previous articles by Pfeiffer et al (2014) 18 and Conti et al (2018) 19 . We use four ADCs to digitize the analog signals from the BEETLE chip and process the data with a centroiding algorithm implemented in an FPGA (s. following Section 5.2).…”

Section: Detector Electronicsmentioning

confidence: 99%

MCP detector development for UV space missions

Conti

Barnstedt

Buntrock

et al. 2020

Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray

View full text Add to dashboard Cite

The Institute for Astronomy and Astrophysics in Tübingen (IAAT) has a long-term experience in developing and building space-qualified imaging and photon counting microchannel-plate (MCP) detectors, which are sensitive in the ultraviolet wavelength range. Our goal is to achieve high quantum efficiency and spatial resolution, while maintaining solar blindness and low-noise characteristics.Our flexible detector design is currently tailored to the specific needs of three missions: For the ESBO DS (European Stratospheric Balloon Observatory -Design Study) we provide a sealed detector to the STUDIO instrument (Stratospheric Ultraviolet Demonstrator of an Imaging Observatory), a 50 cm telescope with a UV imager for operation at an altitude of 37-41 km. In collaboration with the Indian Institute of Astrophysics we plan a space mission with a CubeSat-sized farultraviolet spectroscopic imaging instrument, featuring an open version of our detector. A Chinese mission, led by the Purple Mountain Observatory, comprises a multi-channel imager using open and sealed detector versions.Our MCP detector has a cesium activated p-doped gallium-nitride photocathode. Other photocathode materials like cesium-telluride or potassium-bromide could be used as an alternative. For the sealed version, the photocathode is operated in semi-transparent mode on a MgF2 window with a cut-off wavelength of about 118 nm. For missions requiring sensitivity below this cut-off, we are planning an open version. We employ a coplanar cross-strip anode and advanced low-power readout electronics with a 128-channel charge-amplifier chip. This publication focuses on the progress concerning the main development challenges: the optimization of the photocathode parameters and the sophisticated detector electronics.

show abstract

Section: Detector Electronicsmentioning

confidence: 99%

MCP detector development for UV space missions

Conti

Barnstedt

Buntrock

et al. 2020

Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray

View full text Add to dashboard Cite

show abstract

“…8) is to provide the highly demanding interconnections required to link each of the 128 anode strips to a corresponding input channel of the BEETLE chip. After the signals are preamplified and shaped by the BEETLE chip, the Hybrid Board also provides the outputs to send this data to our front-end electronics as well as the I 2 C Interface to control the BEETLE chip parameters (further details in Pfeifer et al (2014)).…”

Section: Beetle Hybrid Boardmentioning

confidence: 99%

“…Due to the advancements in technology in nearly every part and especially for the readout electronics, our current and next generation detector is a small and lightweight MCP detector with very low power consumption. That means that its mass will be below 3 kg for the detector, its electronics and the high voltage supply at a power consumption of 10-15 Watt (Pfeifer et al 2014). We chose to build an MCP detector as they are solar blind by design (in contrast to a CCD), they provide fast photon counting and a Poissonian noise dominated only by photon statistics (Martin et al 1981).…”

Section: Introductionmentioning

confidence: 99%

MCP detector development for UV space missions

Conti

Barnstedt

Hanke

et al. 2018

Astrophys Space Sci

View full text Add to dashboard Cite

We are developing imaging and photon counting UV-MCP detectors, which are sensitive in the wavelength range from far ultraviolet to near ultraviolet. A good quantum efficiency, solar blindness and high spatial resolution is the aim of our development. The sealed detector has a Cs-activated photoactive layer of GaN (or similarly advanced photocathode), which is operated in semitransparent mode on (001)-MgF 2 . The detector comprises a stack of two long-life MCPs and a coplanar cross strip anode with advanced readout electronics. The main challenge is the flawless growth of the GaN photocathode layer as well as the requirements for the sealing of the detector, to prevent a degradation of the photocathode. We present here the detector concept and the experimental setup, examine in detail the status in the production and describe the current status of the readout electronics development.

show abstract

“…In addition, each channel of the XS anode detector needs a special preamplifier and shaping amplifier, which increases the overall mass and cost. Another scheme is to develop a special multichannel application-specific integrated circuit (ASIC), combining the preamplifier and shaping amplifier [14][15][16][17]. This method can greatly reduce the detector mass and power consumption, but the cost of developing ASIC is high.…”

Section: Introductionmentioning

confidence: 99%

A Photon Imaging Detector Model with High Resolution and High Counting Rate

Jiang

2023

Applied Sciences

View full text Add to dashboard Cite

A cross strip (XS) anode detector is a photon-counting imaging detector with high spatial resolution. However, due to the Poisson distribution characteristics of the photons emitted by the target, photons with a small time interval will cause signal superposition and resolution degradation. This is particularly significant at a high photon count rate. The key link that restricts the counting rate of the XS detector is the electronic system. In this paper, we propose a new electronic signal processing system scheme using a digital trapezoidal shaping filter instead of a traditional Gaussian shaping filter, which enables the detector to maintain a high resolution at high count rates. In order to verify the feasibility of the scheme, the relationship between shaping errors and shaping parameters is studied. Furthermore, the relationship between spatial resolution and photon-counting rate at different noise levels is revealed by numerical simulation. The results show that the detector can achieve a spatial resolution of <50 μm at a photon count rate of >6 MHz for 1000 e RMS noise.

show abstract

Characterisation of low power readout electronics for a UV microchannel plate detector with cross-strip readout

Cited by 4 publications

References 1 publication

MCP detector development for UV space missions

MCP detector development for UV space missions

MCP detector development for UV space missions

A Photon Imaging Detector Model with High Resolution and High Counting Rate

Contact Info

Product

Resources

About