The Short and Mid Wave InfraRed (S-MWIR) rugged active detection system has been designed to be operated in the worst conditions with very low Size Weight and Power (SWaP) factor. The detection system is based on a single uncooled detector device implementing a Lead Sulphide (PbS) (SWIR) and Lead Selenide (PbSe) (MWIR) plate cells on the same package and an emitter based on a combination of standard silicon materials with Nano Amorphous Carbon (NAC) membrane. The data acquisition and processing have been configured to handle very low signal values and important noise in the ambient. The detection system is based on a Lock-In Amplification tuned on 10Hz frequency to reduce the noise effect. The low operation frequency reduces the requirements on IR source and sampling electronics. The IR detectors and source has been instrumented with thermistors and the responsivity of the system has been characterized for non-thermal controlled operation. The characterized responsivity and the instantaneous temperature shall be considered on the data retrieval. The detection system has been qualified for very tough environment as very low temperature (-135°C) and relatively high temperatures (70°C) for a year continuous operation, high vacuum (10-6 mbar), high mechanical vibration and shock and high radiation levels. The S-MWIR detection system has been implemented on the Dust Sensor for the ExoMars’20 mission for operation from 10°C to -90°C with two detector systems forward and backward for calculation the in-situ dust concentration on Mars surface.
Y. Inome, G. Ambrosi, Y. Awane, H. Baba, A. Bamba, M. Barceló, U. Barres de Almeida, J. Barrio, O. Blanch Bigas, J. Boix, L. Brunetti, E. Carmona, E. Chabanne, M. Chikawa, N. Cho, P. Colin, J. Contreras, J. Cortina, F. Dazzi, A. Deangelis, G. Deleglise, C. Delgado, C. Díaz, F. Dubois, A. Fiasson, D. Fink, N. Fouque, L. Freixas, C. Fruck, A. Gadola, R. García, D. Gascón, N. Geffroy, N. Giglietto, F. Giordano, F. Grañena, S. Gunji, R. Hagiwara, N. Hamer, Y. Hanabata, T. Hassan, K. Hatanaka, T. Haubold, M. Hayashida, R. Hermel, D. Herranz, K. Hirotani, J. Hose, D. Hugh, S. Inoue, Y. Inoue, K. Ioka, C. Jablonski, M. Kagaya, H. Katagiri, J. Kataoka, H. Kellermann, T. Kishimoto, M. Knoetig, K. Kodani, K. Kohri, T. Kojima, Y. Konno, S. Koyama, H. Kubo, J. Kushida, G. Lamanna, T. Le Flour, M. López-Moya, R. López, E. Lorenz, P. Majumdar, A. Manalaysay, M. Mariotti, G. Martínez, M. Martinez, S. Masuda, S. Matsuoka, D. Mazin, U. Menzel, J. Miranda , R. Mirzoyan, I. Monteiro, A. Moralejo, K. Murase, S. Nagataki, T. Nagayoshi, D. Nakajima, T. Nakamori, K. Nishijima, K. Noda, A. Nozato, M. Ogino, Y. Ohira, M. Ohishi, H. Ohoka, A. Okumura, S. Ono, R. Orito, J. Panazol, D. Paneque, R. Paoletti, J. Paredes, G. Pauletta, S. Podkladkin, J. Prast, R. Rando, O. Reimann, M. Ribó, S. Rosier-Lees, K. Saito, T. Saito, Y. Saito, N. Sakaki, R. Sakonaka, A. Sanuy, M. Sawada, V. Scalzotto, S. Schultz, T. Schweizer, T. Shibata, S. Shu, J. Sieiro, V. Stamatescu, S. Steiner, U. Straumann, R. Sugawara, H. Tajima, H. Takami, M. Takahashi, S. Tanaka, M. Tanaka, L. Tejedor, Y. Terada, M. Teshima, Y. Tomono, T. Totani, T. Toyama, Y. Tsubone, Y. Tsuchiya, S. Tsujimoto, H. Ueno, K. Umehara, Y. Umetsu, A. Vollhardt, R. Wagner, H. Wetteskind, T. Yamamoto, R. Yamazaki, A. Yoshida, T. Yoshida, T. Yoshikoshi
The Large Size Telescopes, LSTs, located at the center of the Cherenkov Telescope Array, CTA, will be sensitive
for low energy gamma-rays. The camera on the LST focal plane is optimized to detect low energy events based
on a high photon detection efficiency and high speed electronics. Also the trigger system is designed to detect
low energy showers as much as possible. In addition, the camera is required to work stably without maintenance
in a few tens of years. In this contribution we present the design of the camera for the first LST and the status
of its development and production.
G. Ambrosi, Y. Awane, H. Baba, A. Bamba, M. Barceló, U. Barres de Almeida, J. Barrio, O. Blanch Bigas, J. Boix, L. Brunetti, E. Carmona, E. Chabanne, M. Chikawa, R. Colin, J. Cortina, J. Contreras, F. Dazzi, A. De Angelis, G. Deleglise, C. Delgado, C. Díaz, A. Fiasson, D. Fink, N. Fouque, L. Freixas, C. Fruck, A. Gadola, R. García, D. Gascon, N. Geffroy, N. Giglietto, F. Giordano, F. Grañena, S. Gunji, R. Hagiwara, N. Hamer, Y. Hanabata, T. Hassan, K. Hatanaka, K. Hirotani, S. Inoue, Y. Inoue, K. Ioka, C. Jablonski, M. Kagaya, H. Katagiri, T. Kishimoto, K. Kodani, K. Kohri, Y. Konno, S. Koyama, H. Kubo, J. Kushida, G. Lamanna, T. Le Flour, E. Lorenz, R. López, M. López-Moya, P. Majumdar, A. Manalaysay, M. Mariotti, G. Martínez, M. Martínez, D. Mazin, J. Miranda , R. Mirzoyan, I. Monteiro, A. Moralejo, K. Murase, S. Nagataki, D. Nakajima, T. Nakamori, K. Nishijima, K. Noda, A. Nozato, Y. Ohira, M. Ohishi, H. Ohoka, A. Okumura, R. Orito, J. Panazol, D. Paneque, R. Paoletti, J. Paredes, G. Pauletta, S. Podkladkin, J. Prast, R. Rando, O. Reimann, M. Ribó, S. Rosier-Lees, K. Saito, T. Saito, Y. Saito, N. Sakaki, R. Sakonaka, A. Sanuy, H. Sasaki, M. Sawada, V. Scalzotto, S. Schultz, T. Schweizer, T. Shibata, S. Shu, J. Sieiro, V. Stamatescu, S. Steiner, U. Straumann, R. Sugawara, H. Tajima, H. Takami, S. Tanaka, M. Tanaka, L. Tejedor, Y. Terada, M. Teshima, T. Totani, H. Ueno, K. Umehara, A. Vollhardt, R. Wagner, H. Wetteskind, T. Yamamoto, R. Yamazaki, A. Yoshida, T. Yoshida, T. Yoshikoshi
The Cherenkov Telescope Array (CTA) project aims to implement the world’s largest next generation of Very High Energy gamma-ray Imaging Atmospheric Cherenkov Telescopes devoted to the observation from a few tens of GeV to more than 100 TeV. To view the whole sky, two CTA sites are foreseen, one for each hemisphere. The sensitivity at the lowest energy range will be dominated by four Large Size Telescopes, LSTs, located at the center of each array and designed to achieve observations of high red-shift objects with the threshold energy of 20 GeV. The LST is optimized also for transient low energy sources, such as Gamma Ray Bursts (GRB), which require fast repositioning of the telescope. The overall design and the development status of the first LST telescope will be discussed.
In this work, three strategies for shortening the output pulse of a silicon photomultiplier (SiPM) are reported. The first strategy is passive filtering, where band-pass filtering removes the lowest frequency components in the signal, getting a noticeable reduction in pulse width (a compression ratio of 10∶1 was obtained). In the second place, a reflectometric scheme is proposed where the amplified signal coming from the SiPM is injected into a signal splitter with one of its stubs connected to a short-circuited stub. In the last strategy, the reflectometric part is replaced by an analog subtractor circuit. In this approach, a signal splitter with stubs of different lengths is used. All solutions provide good compression ratios, up to 10∶1. Best pulses obtained are single narrow peaks, with width below 10 ns, preserving the photonic modulation and with good pseudo-Gaussian shape, single polarity and low ringing. The potential of pulse shortening for improving the capability of the detector to resolve single photons is demonstrated by mean of single photon counting patterns. The detection error probability is reduced in one order of magnitude when shortening is used for conditioning the output photosignal.
Photomultipliers have a wide range of applications, from nuclear medicine to nuclear physics. In particular, they are commonly used in high energy physics and astrophysics. The Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescope is an example of their applications. This work presents a test system for the characterization of the transient response of the photomultipliers used as fast light detectors in the telescope. The bias of the photomultiplier is described, taking into account its effects in the response to fast light pulses. Two methods are used to generate these pulses: 1. a specifically designed pulse generator, and 2. a plastic scintillator. For the former case, we also calculate the anode charge we expect in this setup to cross-check it with the actual measurements.
A simple and cost-effective integrated synthesizer of fast light pulses has been designed, analyzed and tested for the characterization of the time response of photo-multipliers (PMT). This synthesizer consists of an integrated pulse generator based on Schmidt Trigger Inverters, a broadband matching network and a high speed LED. It enables the generation of pulses as short as less than 10 ns with variable pulse width, amplitude and repetition frequency. In order to accurately know the shape of the pulses applied to the PMT under test, a circuital model of the LED has been developed and verified at frequencies up to 2 GHz. This model accounts for the nonlinear behavior of the LED capacitance as well as the package parasitics. The influence of the mismatch at the different frequency components of the synthesized pulse has been investigated. The pulse transmitter has been used to test the time response of MAGIC telescope pixels.
In this work we have built an electro-optical system for the transmission of low frequency analogue signals through optical fibre. The main goal was to achieve minimum pulse distortion with maximum dynamic range. The system has been used in the framework of the MAGIC telescope experiment for the transmission of the analogue output from a photo-multiplier dedicated to optical observation of astrophysical objects, in particular pulsars. The received signal polarizes an infrared LED (λ=850 nm), which converts the pulse into an optical analogue pulse. The electro-optical pulse is transmitted by means of a multi-mode optic fibre and finally amplified and filtered by the optical receiver. The whole system has been tested using a pulse generator resembling the type of pulsed signal we expect from pulsars, that is with period of about tens of milli-seconds and few milli-seconds wide. The system was calibrated in order to: a) obtain a fixed relation between the received pulse and the final data and b) enhance the dynamic range and low distortion. In what follows, we show the behaviour of the optical transmitter under different pulse shapes, amplitude and frequencies up to several hundred Hz. The electro-optical system has been mounted on the MAGIC telescope and tested successfully with the observation of the pulsed optical signal from the Crab pulsar.
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