The atmospheric monitoring system of the JEM-EUSO instrument

Adams, J. H.; Ahmad, S.; Albert, J.; Allard, Denis; Anchordoqui, Luis A.; Andreev, V.; Anzalone, A.; Arai, Y.; Asano, Katsuaki; Pernas, M. Ave; Baragatti, P.; Barrillon, P.; Batsch, T.; Bayer, J.; Bechini, R.; Belenguer, T.; Bellotti, R.; Belov, K.; Berlind, Andreas A.; Bertaina, M.; Biermann, P. L.; Biktemerova, S.; Blaksley, C.; Blanc, Nicolas; Błȩcki, J.; Blin-Bondil, S.; Blümer, J.; Bobík, P.; Bogomilov, M.; Bonamente, Massimiliano; Briggs, M. S.; Briz, S.; Bruno, A.; Cafagna, F.; Campana, D.; Capdevielle, J. N.; Caruso, R.; Casolino, M.; Cassardo, Claudio; Castellinic, G.; Catalano, C.; Catalano, Gelsomina; Cellino, A.; Chikawa, M.; Christl, M. J.; Cline, D.; Connaughton, V.; Conti, L.; Cordero, G.; Crawford, H. J.; Cremonini, R.; Csorna, S. E.; Dagoret-Campagne, S.; Castro, Antonio; Donato, C. De; Taille, C. De La; Santis, C. De; Peral, L. del; Dell’Oro, A.; Simone, N. De; Martino, M. Di; Distratis, G.; Dulucq, F.; Dupieux, M.; Ebersoldt, A.; Ebisuzaki, T.; Engel, R.; Falk, S.; Fang, Ke; Fenu, Francesco; Fernández-Gómez, I.; Ferrarese, S.; Finco, D.; Flamini, Marta; Fornaro, C.; Franceschi, A.; Fujimoto, J.; Fukushima, M.; Galeotti, P.; Garipov, G.; Geary, J.; Gelmini, Graciela B.; Giraudo, G.; Gonchar, M.; Alvarado, C. González; Gorodetzky, P.; Guarino, F.; Guzmán, A.; Hachisu, Y.; Harlov, B.; Haungs, A.; Carretero, J. Hernández; Higashide, K.; Ikeda, D.; Ikeda, Hirokazu; Inoue, N.; Inoue, Susumu; Insolia, A.; Isgrò, Francesco; Itow, Y.; Joven, E.; Judd, E. G.; Jung, A.; Kajino, F.; Kajino, Toshitaka; Kaneko, Ichiro; Karadzhov, Y.; Karczmarczyk, J.; Karus, M.; Katahira, Kazutoshi; Kawai, K.; Kawasaki, Y.; Keilhauer, B.; Khrenov, B. A.; Kim, J. S.; Kim, S. W.; Kleifges, M.; Климов, П. А.; Kolev, D.; Kreykenbohm, I.; Kudela, K.; Kurihara, Y.; Kusenko, Alexander; Kuznetsov, E.; Lacombe, M.; Lachaud, C.; Lee, J.; Licandro, J.; Lim, H.; López, Fernando Martínez; Maccarone, Maria Concetta; Mannheim, K.; Maravilla, D.; Marcelli, L.; Marini, A.; Martinez, O.; Masciantonio, G.; Mase, K.; Matev, R.; Medina‐Tanco, G.; Mernik, T.; Miyamoto, H.; Miyazaki, Y.; Mizumoto, Y.; Modestino, G.; Monaco, A.; Monnier-Ragaigne, D.; Ríos, J. A. Morales de los; Moretto, C.; Morozenko, V. S.; Mot, B.; Murakami, Takeshi; Murakami, Masao; Nagata, M.; Nagataki, Shigehiro; Nakamura, Tôru; Napolitano, T.; Naumov, D.; Nava, Rodrigo; Neronov, A.; Nomoto, Ken’ichi; Nonaka, T.; Ogawa, Tatsuhiko; Ogio, S.; Ohmori, Hitoshi; Olinto, Angela V.; Orleański, P.; Osteria, G.; Panasyuk, M. I.; Parizot, E.; Park, I. H.; Park, H. W.; Pastirčák, B.; Patzak, T.; Paul, T.; Pennypacker, C.; Cano, S. Perez; Peter, Thomas; Picozza, P.; Pierog, T.; Piotrowski, L. W.; Piraino, S.; Plebaniak, Z.; Pollini, A.; Prat, P.; Prévôt, G.; Prieto, H.; Putiš, M.; Reardon, Patrick J.; Reyes, M.; Ricci, M.; Rodríguez, I.; Frías, M. D. Rodríguez; Ronga, F.; Roth, M.; Rothkaehl, Hanna; Roudil, G.; Rusinov, I.; Rybczyński, M.; Sabau, M. D.; Sáez-Cano, G.; Sagawa, H.; Saito, Akinori; Sakaki, N.; Sakata, M.; Salazar, H.; Sánchez, Sergio; Santangelo, A.; Crúz, L. Santiago; Palomino, M. Sanz; Saprykin, O.; Sarazin, F.; Sato, H.; Sato, Mitsuteru; Schanz, T.; Schieler, H.; Scotti, V.; Segreto, A.; Selmane, S.; Semikoz, D.; Serra, M.; Sharakin, S.; Shibata, T.; Shimizu, Hideyuki; Shinozaki, K.; Shirahama, T.; Siemieniec‐Oziȩbło, G.; López, H. H. Silva; Sledd, J.; Słomińska, K.; Sobey, A.; Sugiyama, T.; Supanitsky, D.; Suzuki, M.; Szabelska, B.; Szabelski, J.; Tajima, Fumiko; Tajima, N.; Tajima, T.; Takahashi, Y.; Takami, H.; Takeda, M.; Takizawa, Y.; Tenzer, C.; Tibolla, O.; Ткачев, Л.; Tokuno, H.; Tomida, T.; Tone, N.; Toscano, S.; Trillaud, F.; Tsenov, R.; Tsunesada, Y.; Tsuno, K.; Tymieniecka, T.; Uchihori, Y.; Unger, Michael; Văduvescu, O.; Valdés-Galicia, J. F.; Vallania, P.; Valore, L.; Vankova, G.; Vigorito, C.; Villaseñor, L.; Ballmoos, P. von; Wada, Satoshi; Watanabe, J.; Watanabe, Shigeto; Watts, J. W.; Weber, M.; Weiler, T.; Wibig, T.; Wiencke, L.; Wille, M.; Wilms, J.; Włodarczyk, Z.; Yamamoto, T.; Yamamoto, Y.; Yang, J.; Yano, Hajime; Yashin, I. V.; Yonetoku, Daisuke; Yoshida, Kenji; Yoshida, Shigeru; Young, R.; Zotov, M. Yu.; Marchi, A. Zuccaro

doi:10.1007/s10686-014-9378-1

Cited by 11 publications

(4 citation statements)

References 11 publications

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“…For this reason, in order to increase the statistics, it has been suggested to install the UV telescope on a satellite or on the International Space Station (ISS) to monitor a portion of the Earth's atmosphere much larger than the one currently covered by the ground‐based detectors. The telescope will also perform studies of atmospheric phenomena, observation of meteors, strange quark matter search, and space debris tracking . Sixteen countries, 84 research institutes, and more than 350 researchers are collaborating on the JEM‐EUSO program, with the support of several space agencies, including NASA (USA), ASI (Italy), CNES (France), ROSCOSMOS (Russia), and JAXA (Japan).…”

Section: The Jem‐euso Experimentsmentioning

confidence: 99%

The onboard software of the EUSO‐SPB pathfinder experiment

et al. 2018

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In this paper, the flight software architecture of the EUSO-SPB mission is described. The JEM-EUSO program aims at developing an advanced large space-borne UV telescope designed to detect ultra high energy cosmic rays. In this framework, the EUSO-SPB experiment is the third pathfinder mission of the JEM-EUSO program, the second that has been launched on a stratospheric balloon to test the technological readiness of the detectors and to carry out some preliminary scientific observations. The EUSO-SPB software has a modular structure conceived to control all the instruments and the ancillary subsystems, to acquire data, and to manage data transfer to ground. System programming in C and C++ languages and Bash scripts have been used to implement and run the modules. The software runs on the data processor, an onboard computer that communicates with several payload blocks, the UV sensor, and the synchronization and time tagging board. The control software module controls all the subsystems, provides communication to ground through the NASA telemetry or the Internet, runs the acquisition control and download software, and manages the execution of the acquisition software. The acquisition software module directly operates the subsystems for the data acquisition activity. The acquisition control and download software module runs the acquisition software upon request of the control software and transfers scientific data to ground. The software system performed as expected during the flight on April 2017. KEYWORDS cosmic rays, EUSO, flight software, SPB, stratospheric balloon, UHECR THE JEM-EUSO EXPERIMENTSThe JEM-EUSO * program 1,2 aims at developing a large space-borne UV telescope able to detect the ultra high energy cosmic rays (UHECRs). The very wide field-of-view telescope is conceived to look down from space toward the Earth to detect the fluorescence photons emitted by the cascades of particles produced by the interaction of an UHECR with the *EUSO is the acronym of Extreme Universe Space Observatory, whereas JEM is named after the Japanese Experiment Module, the module of the International Space Station where the UV telescope was initially designed to be installed. 524

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Section: The Jem‐euso Experimentsmentioning

confidence: 99%

The onboard software of the EUSO‐SPB pathfinder experiment

et al. 2018

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“…For this reason, JEM-EUSO will be equipped with an Atmospheric Monitoring System (AMS), see Figure 1, which will include: a) an InfraRed (IR) camera; b) a Lidar device. Moreover it will be supported by global atmospheric models generated from the analysis of all available meteorological data provided by global weather services, such as the European Centre for Medium-range Weather Forecasts (ECMWF) (http://www.ecmwf.int/) [5]. Lidar data provide precise measurements of atmospheric parameters, such as cloud optical depth, cloud height etc., in certain localised points in the FoV (i.e., around the EAS location).…”

Section: Introductionmentioning

confidence: 99%

Methods to Retrieve the Cloud-Top Height in the Frame of the JEM-EUSO Mission

Anzalone

Bertaina

Briz

et al. 2019

IEEE Trans. Geosci. Remote Sensing

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The JEM-EUSO (Japanese Experiment Module-Extreme Universe Space Observatory) telescope will measure Ultra High Energy Cosmic Ray properties by detecting the UV fluorescence light generated in the interaction between cosmic rays and the atmosphere. Therefore, information on the state of clouds in the atmosphere is crucial for a proper interpretation of the data. For a real-time observation of the clouds in the telescope Field of View (FoV), JEM-EUSO will use an atmospheric monitoring system composed of a Lidar (LIght Detection And Ranging) and an Infra-Red Camera. In this article the focus is on the IR camera data. To retrieve the Cloud Top Height (CTH) from IR images, three different methods are considered here. The first one is based on bi-spectral stereo vision algorithms and requires two different views of the same scene in different spectral bands. For the second one, brightness temperatures provided by the IR camera are converted to effective cloud top temperatures, from which the CTH is estimated using the vertical temperature profiles. A third method that uses primary Numerical Weather Prediction (NWP) model output parameters, such as the cloud fraction, has also been considered to retrieve the CTH. This article presents a first analysis, in which the heights retrieved by these three methodologies are compared with the heights given by MODIS (MODerate resolution Imaging Spectroradiometer) sensor installed on the polar satellite Terra. Since all these methods are suitable for the JEM-EUSO mission, they could be used in the future in a complementary way to improve the accuracy of the CTH retrieval.

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“…Since JEM-EUSO will cover a very large observation area in the atmosphere (∼10 5 km 2 ), a properly monitoring of the atmospheric conditions is mandatory. The Atmospheric Monitoring System (AMS) [1,2] of JEM-EUSO will consist of a bispectral and space qualified Infrared Camera and a LIDAR (LIght Detection And Ranging). The bi-spectral IR camera gives the cloud coverage in the FoV of the main telescope.…”

Section: Introductionmentioning

confidence: 99%

Thin and thick cloud top height retrieval algorithm with the Infrared Camera and LIDAR of the JEM-EUSO Space Mission

Sáez-Cano

Ríos

Peral

et al. 2015

EPJ Web of Conferences

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Abstract. The origin of cosmic rays have remained a mistery for more than a century. JEM-EUSO is a pioneer space-based telescope that will be located at the International Space Station (ISS) and its aim is to detect Ultra High Energy Cosmic Rays (UHECR) and Extremely High Energy Cosmic Rays (EHECR) by observing the atmosphere. Unlike ground-based telescopes, JEM-EUSO will observe from upwards, and therefore, for a properly UHECR reconstruction under cloudy conditions, a key element of JEM-EUSO is an Atmospheric Monitoring System (AMS). This AMS consists of a space qualified bi-spectral Infrared Camera, that will provide the cloud coverage and cloud top height in the JEM-EUSO Field of View (FoV) and a LIDAR, that will measure the atmospheric optical depth in the direction it has been shot. In this paper we will explain the effects of clouds for the determination of the UHECR arrival direction. Moreover, since the cloud top height retrieval is crucial to analyze the UHECR and EHECR events under cloudy conditions, the retrieval algorithm that fulfills the technical requierements of the Infrared Camera of JEM-EUSO to reconstruct the cloud top height is presently reported.

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The atmospheric monitoring system of the JEM-EUSO instrument

Cited by 11 publications

References 11 publications

The onboard software of the EUSO‐SPB pathfinder experiment

The onboard software of the EUSO‐SPB pathfinder experiment

Methods to Retrieve the Cloud-Top Height in the Frame of the JEM-EUSO Mission

Thin and thick cloud top height retrieval algorithm with the Infrared Camera and LIDAR of the JEM-EUSO Space Mission

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