Open AccessThe readout system based on the ultra-fast waveform sampler DRS4 for the Large-Sized Telescope of the Cherenkov Telescope Array
Author(s) -
Seiya Nozaki,
O. Blanch,
C. Delgado Mendez,
Paweł Gliwny,
D. Hadasch,
Yusuke Inome,
H. Katagiri,
H. Kubo,
Yasuaki Kobayashi,
D. Mazin,
A. Moralejo,
Y. Nogami,
R. Paoletti,
Takayuki Saito,
Shunsuke Sakurai,
J. Sitarek,
Mitsunari Takahashi,
M. Teshima,
Tokonatsu Yamamoto
Publication year - 2020
Publication title -
journal of physics. conference series
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.21
H-Index - 85
eISSN - 1742-6596
pISSN - 1742-6588
DOI - 10.1088/1742-6596/1468/1/012104
Subject(s) - physics , telescope , cherenkov telescope array , observatory , cherenkov radiation , calibration , optics , detector , sampling (signal processing) , dynamic range , remote sensing , astronomy , quantum mechanics , geology
The Cherenkov Telescope Array (CTA) is the next-generation ground-based very-high-energy gamma-ray observatory. By using three types of telescopes CTA can cover a wide energy range (20 GeV–300 TeV) with an order of magnitude higher sensitivity than the current telescopes. The Large-Sized Telescope (LST) is designed to detect 20 GeV–1 TeV gamma rays thanks to the large light collection area, sensitive photosensors, a fast trigger system, and readout electronics. The camera readout system must have a high signal-to-noise ratio and a linear signal sampling with a large dynamic range in order to efficiently detect dim and low-energy atmospheric showers. To meet this requirement we use the Domino Ring Sampler version 4 (DRS4), which also enables ultra-fast sampling with low power consumption. Some of the intrinsic characteristics of DRS4 chips require software corrections. These procedures lower the effect of non-Gaussian noise contribution and improve the timing resolution of the system. In this contribution we discuss the calibration algorithms and the resulting performance.