Riccardo Rando∗ab, Daniele Cortia, Francesco Dazzic, Alessandro De Angelisd, Antonios Dettlaffc, Daniela Dornere, David Finkc, Nadia Fouque f , Felix Grundnerc, Werner Habererc, Alexander Hahnc, Richard Hermel f , Samo Korparg, Gasper Kukec Mezekh, Ronald Maierc, Christian Maneaa, Mose Mariottiab, Daniel Mazinci, Fatima Mehrez f , Razmik Mirzoyanc, Sergey Podkladkinc, Ignasi Reichardta, Wolfgang Rhode j, Sylvie Rosier f , Cornelia Schultzab, Carlo Stellak, Masahiro Teshimaci, Holger Wetteskindc and Marko Zavrtanikgh for the CTA Consortium† E-mail: riccardo.rando@pd.infn.it a INFN Section of Padova, Italy; b University of Padova, Italy; c Max Planck Institute for Physics, Munich, Germany; d LIP/IST Lisboa, Portugal; e University of Wurzburg, Germany; f LAPP, CNRS-IN2P3, Annecy, France; g Jožef Stefan Institute, Ljubljana, Slovenia; h University of Nova Gorica, Slovenia; i University of Tokyo and ICRR, Tokyo, Japan; j Technische Universitat, Dortmund, Germany; k University of Udine and INFN, Italy. The Cherenkov Telescope Array (CTA) is the the next generation facility of imaging atmospheric Cherenkov telescopes; two sites will cover both hemispheres. CTA will reach unprecedented sensitivity, energy and angular resolution in very-high-energy gamma-ray astronomy. Each CTA array will include four Large Size Telescopes (LSTs), designed to cover the low-energy range of the CTA sensitivity (∼20 GeV to 200 GeV). In the baseline LST design, the focal-plane camera will be instrumented with 265 photodetector clusters; each will include seven photomultiplier tubes (PMTs), with an entrance window of 1.5 inches in diameter. The PMT design is based on mature and reliable technology. Recently, silicon photomultipliers (SiPMs) are emerging as a competitor. Currently, SiPMs have advantages (e.g. lower operating voltage and tolerance to high illumination levels) and disadvantages (e.g. higher capacitance and cross talk rates), but this technology is still young and rapidly evolving. SiPM technology has a strong potential to become superior to the PMT one in terms of photon detection efficiency and price per square mm of detector area. While the advantage of SiPMs has been proven for high-density, small size cameras, it is yet to be demonstrated for large area cameras such as the one of the LST. We are working to develop a SiPM-based module for the LST camera, in view of a possible camera upgrade. We will describe the solutions we are exploring in order to balance a competitive performance with a minimal impact on the overall LST camera design. The 34th International Cosmic Ray Conference, 30 July6 August, 2015 The Hague, The Netherlands

/pdf/silicon-photomultiplier-research-and-development-studies-for-tisaz1br92.pdf

Silicon Photomultiplier Research and Development Studies for the Large Size Telescope of the Cherenkov Telescope Array

The Cherenkov Telescope Array (CTA) is the the next generation facility of imaging atmospheric Cherenkov telescopes; two sites will cover both hemispheres. CTA will reach unprecedented sensitivity, energy and angular resolution in very-high-energy gamma-ray astronomy. Each CTA array will include four Large Size Telescopes (LSTs), designed to cover the low-energy range of the CTA sensitivity ($\sim$20 GeV to 200 GeV). In the baseline LST design, the focal-plane camera will be instrumented with 265 photodetector clusters; each will include seven photomultiplier tubes (PMTs), with an entrance window of 1.5 inches in diameter. The PMT design is based on mature and reliable technology. Recently, silicon photomultipliers (SiPMs) are emerging as a competitor. Currently, SiPMs have advantages (e.g. lower operating voltage and tolerance to high illumination levels) and disadvantages (e.g. higher capacitance and cross talk rates), but this technology is still young and rapidly evolving. SiPM technology has a strong potential to become superior to the PMT one in terms of photon detection efficiency and price per square mm of detector area. While the advantage of SiPMs has been proven for high-density, small size cameras, it is yet to be demonstrated for large area cameras such as the one of the LST. We are working to develop a SiPM-based module for the LST camera, in view of a possible camera upgrade. We will describe the solutions we are exploring in order to balance a competitive performance with a minimal impact on the overall LST camera design.

pdf/silicon-photomultiplier-research-and-development-studies-for-5zkn5bxqa2.pdf

The Cherenkov Telescope Array (CTA) is the next generation ground-based very high energy gamma-ray observatory. The Large-Sized Telescope (LST) of CTA targets 20 GeV -- 1 TeV gamma rays and has 1855 photomultiplier tubes (PMTs) installed in the focal plane camera. With the 23 m mirror dish, the night sky background (NSB) rate amounts to several hundreds MHz per pixel. In order to record clean images of gamma-ray showers with minimal NSB contamination, a fast sampling of the signal waveform is required so that the signal integration time can be as short as the Cherenkov light flash duration (a few ns). We have developed a readout board which samples waveforms of seven PMTs per board at a GHz rate. Since a GHz FADC has a high power consumption, leading to large heat dissipation, we adopted the analog memory ASIC "DRS4". The sampler has 1024 capacitors per channel and can sample the waveform at a GHz rate. Four channels of a chip are cascaded to obtain deeper sampling depth with 4096 capacitors. After a trigger is generated in a mezzanine on the board, the waveform stored in the capacitor array is subsequently digitized with a low speed (33 MHz) ADC and transferred via the FPGA-based Gigabit Ethernet to a data acquisition system. Both a low power consumption (2.64 W per channel) and high speed sampling with a bandwidth of $>$300 MHz have been achieved. In addition, in order to increase the dynamic range of the readout we adopted a two gain system achieving from 0.2 up to 2000 photoelectrons in total. We finalized the board design for the first LST and proceeded to mass production. Performance of produced boards are being checked with a series of quality control (QC) tests. We report the readout board specifications and QC results.

Development of the photomultiplier tube readout system for the first Large-Sized Telescope of the Cherenkov Telescope Array

Telescopes -- far seeing -- have since centuries revealed insights to objects at cosmic distances. Adopted for gamma-ray-astronomy, ground based Cherenkov-telescopes image the faint Cherenkov-light of air-showers induced by cosmic gamma-rays rushing into earth's atmosphere. In the race for the lowest possible energy-threshold for cosmic gamma-rays, these Cherenkov-telescopes have become bigger, and now reached their physical limits. The required structural rigidity for image-quality constrains a cost-effective construction of telescopes with apertures beyond 30 meter in diameter. Moreover, as the aperture increases, the narrower depth-of-field irrecoverably blurs the images what prevents the reconstruction of the cosmic particle's properties. To overcome these limits, we propose plenoptic-perception with light-fields. Our proposed 71 meter Cherenkov-plenoscope requires much less structural rigidity and turns a narrow depth-of-field into three-dimensional reconstruction-power. With an energy-threshold for gamma-rays of one Giga electron Volt, 20 times lower than what is foreseen for the future planned Cherenkov-Telescope-Array (CTA), the Cherenkov-plenoscope could become the portal to enter the sub second time-scale of the highly variable gamma-ray-sky. Also, this doctoral-thesis contains a second part on the prospects of single-photon-perception in Cherenkov-astronomy.

Cherenkov-Plenoscope.

High-speed analog-to-digital converters (ADCs) are key components in a huge variety of systems, including trigger and data acquisition (TDAQ) systems of Nuclear and Sub-nuclear Physics experiments. Over the last decades, the sample rate and dynamic range of high-speed ADCs underwent a continuous growth and it required the development of suitable interface protocols, such as the new JESD204B serial interface protocol. In this work, we present an original JESD204B-compliant architecture we designed, which is able to operate an analog-to-digital converter in a remote fashion. Our design includes a deterministic-latency high-speed serial link, which is the only connection between the local and remote logic of the architecture and which preserves the deterministic timing features of the protocol. By means of our solution it is possible to read data out of several converters, even remote to each other, and keep them operating synchronously. Our link also supports forward error correction (FEC) capabilities, in the view of the operation in radiation areas (e.g. on-detector in TDAQ systems). We discuss an implementation of our concept in a latest generation FPGA (Xilinx Kintex-7 325T), its logic footprint, frequency performance and power consumption. We present measurements of the timing jitter and latency stability of JESD204B timing-critical signals forwarded over the link. We also describe a demo application of our architecture.

A JESD204B-compliant architecture for remote and deterministic-latency operation

The camera of the Large Size Telescopes (LSTs) of the Cherenkov Telescope Array (CTA) consists of 265 photosensor modules, each of them containing 7 photomultiplier tubes (PMTs), a slow control board (SCB), a readout board, and a trigger logic. We have developed the SCB, which is installed between the 7 PMTs and the readout board. The main task for SCBs is the controlling of the high voltages for the PMTs and the monitoring of their anode currents. In addition, the SCB provides the functionality to create test pulses that can be injected at the input of the PMT preamplifier in order to emulate a PMT signal without the need of setting a high voltage, or even without the PMT itself. The test pulses have a very similar width as the PMT pulses (less than 3 ns FWHM) and their amplitude can be adjusted in a wide dynamic range. These features allow us not only to test the functionality of the camera modules but also to fully characterize these. We report on the design and the functions of the SCB together with the results of test measurements.

/pdf/development-of-slow-control-boards-for-the-large-size-2fi8wwgro7.pdf

Development of Slow Control Boards for the Large Size Telescopes of the Cherenkov Telescope Array

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Development of the photomultiplier tube readout system for the first Large-Sized Telescope of the Cherenkov Telescope Array

Development of Slow Control Boards for the Large Size Telescopes of the Cherenkov Telescope Array