arXiv subjects

JEM-EUSO Collaboration

Publications and source records attributed to JEM-EUSO Collaboration.

7 recordsLinked to original sources

arXiv2024

The Fluorescence Camera of the POEMMA-Balloon with Radio (PBR): Design and Scientific goals

The POEMMA-Balloon with Radio (PBR) is a proposed payload to fly on a NASA Super Pressure Balloon (SPB). It will act as a pathfinder of the Probe Of Extreme Multi-Messenger Astrophysics (POEMMA) detector. PBR will consist of an innovative hybrid focal surface featuring a Fluorescence Camera (FC, based on Multi-Anode Photomultiplier Tubes [MAPMTs], 1.05 $μ$s time resolution) and a Cherenkov Camera (based on SiPMs, 10 ns time resolution), both mounted on the same tiltable frame that can point from nadir up to 13$^\circ$ above the horizon. The FC's main scientific goal is to observe, for the first time, the fluorescence emission of Extensive Air Showers produced by Ultra-High Energy Cosmic Rays from sub-orbital altitudes. This measurement will validate the detection strategy for future space-based missions, such as POEMMA. As a secondary goal, the FC will perform a search for macroscopic dark matter through slowly evolving showers that will leave a signal similar to (but distinct from) a meteor. PBR targets a launch in 2027 as a payload of an ultra-long duration balloon flight with a duration of up to 100 days.

astro-ph.IM↗

arXiv2019

Weather Research and Forecasting) model and radiative methods for cloud top height retrieval along the EUSO-SPB1 trajectory

The Extreme Universe Space Observatory-Super Pressure Balloon (EUSO-SPB1) is a pathfinder of the JEM-EUSO program, which aims to observe Ultra High Energy Cosmic Rays (UHECRs) from near-space. It was launched from Wanaka (New Zealand) on April 25, 2017 UTC and was terminated after twelve days of flight in the South Pacific Ocean. A good knowledge of the atmospheric conditions and cloud properties, such as the Cloud Top Height (CTH), is fundamental to correctly reconstruct the energy and geometry of air showers produced by cosmic rays passing through the atmosphere. One of the methods used to retrieve the CTH is based on Numerical Weather Prediction models. In this work, we consider in particular the Weather Research and Forecasting (WRF) model. A first model test is made on the WRF parametrizations for elementary processes, applying a top-bottom directed algorithm based on two quantities: cloud fraction and optical depth. The validated procedure is then applied to the SPB1 trajectory, retrieving the CTH every ten minutes for the days of the flight. A comparison is made with the analyzed data taken from MODerate resolution Imaging Spectroradiometer (MODIS) satellite images, once per day, to understand the reliability of the method. Another way to retrieve the CTH is the so-called radiative method, that allows to calculate the Cloud Top Temperature (CTT). A vertical temperature profile is needed to transform the CTT into CTH. When radiosoundings are not available, WRF can provide vertical temperature profiles. The conversion from the CTT to the CTH is then made.

physics.ao-ph↗

arXiv2019

Laser test with Mini-EUSO

Mini-EUSO (Extreme Universe Space Observatory) is a small-scale prototype cosmic-ray detector that will measure Earth`s UV emission and other atmospheric phenomena from space. It will be placed in the International Space Station (ISS) behind a UV-transparent window looking to the nadir. The launch is planned this year (2019). Consisting of a multi-anode photomultiplier (MAPMT) camera and a $25$ cm diameter Fresnel lens system, Mini-EUSO has a \ang{44} field of view (FoV), a $6.5$ km$^2$ spatial resolution on the ground and a $2.5\ μ$s temporal resolution. In principle, Mini-EUSO will be sensitive to extensive air shower (EAS) from cosmic-rays with energies above $10^{21}$ eV. A mobile, steerable UV laser system will be used to test the expected energy threshold and performance of Mini-EUSO. The laser system will be driven to remote locations in the Western US and aimed across the field of view of Mini-EUSO when the ISS passes overhead during dark nights. It will emit pulsed $355$ nm UV laser light to produce a short speed-of-light track in the detector. The brightness of this track will be similar to the track from an EAS resulting from a cosmic-ray of up to $10^{21}$ eV. The laser energy is selectable with a maximum of around $90$ mJ per pulse. The energy calibration factor is stable within $5\ \% $. The characteristics of the laser system and Mini-EUSO have been implemented inside the JEM-EUSO OffLine software framework, and laser simulation studies are ongoing to determine the best way to perform a field measurement.

astro-ph.IM↗

arXiv2019

Search for Ultra High Energy Cosmic Rays from Space -- The JEM-EUSO Program

The origin and nature of Ultra-High Energy Cosmic Rays (UHECRs) remain unsolved in contemporary astroparticle physics. To give an answer to these questions is rather challenging because of the extremely low flux of a few per km$^2$ per century at extreme energies (i.e. E $>$ 5$\times$10$^{19}$ eV). The central objective of the JEM-EUSO program, Joint Experiment Missions for Extreme Universe Space Observatory, is the realisation of an ambitious space-based mission devoted to UHECR science. A super-wide-field telescope will look down from space onto the night sky to detect UV photons emitted from air showers generated by UHECRs in the atmosphere. The JEM-EUSO program includes several missions from ground (EUSO-TA), from stratospheric balloons (EUSO-Balloon, EUSO-SPB1, EUSO-SPB2), and from space (TUS, Mini-EUSO) employing fluorescence detectors to demonstrate the UHECR observation from space and prepare the large size missions K-EUSO and POEMMA. We review the scientifical objectives associated with the developing projects of the JEM-EUSO program and the technological achievements allowing them.

astro-ph.IM↗

arXiv2019

Silicon Photomultipliers for Orbital Ultra High Energy Cosmic Ray Observation

Development of the Silicon photomultiplier Elementary Cell Add-on camera (SiECA) has provided extensive information regarding the use of SiPMs for future cosmic ray detection systems. We present the technical aspects of sensor readout development utilizing Citiroc ASIC chips from Weeroc controlled by a Xilinx FPGA to process and package events from four 64 channel Hamamatsu MPPC S13361 arrays generating 128 frame events with an integration time of 2.5ms (parameters are based on JEM-EUSO geometry but can be easily adjusted). With single photon counting capability, SiECA proves SiPM are viable sensors to replace Multi-Anode PhotoMultiplier Tubes in future devices, especially when high luminosity exposure is possible potentially damaging MAPMT based systems. Complementary to the technical aspects, computational and analysis methods for sensor array characterization and in depth device flat-fielding are presented. Provided channel by channel biasing, in comparison to uniform biasing with MAPMTs, fine tuning of operating parameters with MPPC arrays allows for substantial improvements in detector and signal uniformity.

astro-ph.IM↗

arXiv2015

Physics Goals and Status of JEM-EUSO and its Test Experiments

The JEM-EUSO mission aims to explore the origin of the extreme energy cosmic rays (EECRs) through the observation of air-shower fluorescence light from space. The superwide-field telescope looks down from the International Space Station onto the night sky to detect UV photons (fluorescence and Cherenkov photons) emitted from air showers. Such a space detector offers the remarkable opportunity to observe a huge volume of atmosphere at once and will achieve an unprecedented statistics within a few years of operation. Several test experiments are currently in operation: e.g., one to observe the fluorescence background from the edge of the Atmosphere (EUSO-Balloon), or another to demonstrate on ground the capability of detecting air showers with a EUSO-type telescope (EUSO-TA). In this contribution a short review on the scientific objectives of the mission and an update of the instrument definition, performances and status, as well as status of the test experiments will be given.

astro-ph.IM↗

arXiv2015

Multi Anode Photomultiplier Tube Reliability Assessment for the JEM-EUSO Space Mission

Reliability assessment in concerned with the analysis of devices and systems whose individual components are prone to fail. This reliability analysis documents the process and results of reliability determination of the JEM-EUSO photomultiplier tube component using the methods 217 Plus. Quantum efficiency degradation and radiation hardness assurance. In conclussion, the levels of damage suffered by the PMTs which comprise the focal surface of JEM-EUSO Space Telescope, are acceptable. The results show as well the greatest contribution to the failure is due to radiation SET. The guaranteed performance of this equipment is a 99.45 per cent, an accepted value of reliability thus fulfilling the objectives and technological challenges of JEM-EUSO.

physics.ins-det↗