Japanese Experiment Module Research Articles

The JEM-EUSO mission to explore the extreme Universe

Accommodated on the Japanese Experiment Module (JEM) of the International Space Station (ISS), the Extreme Universe Space Observatory JEM-EUSO will utilize the Earth’s atmosphere as a giant detector of the extreme energy cosmic rays; the most energetic particles coming from the Universe. Looking downward the Earth from Space, JEM-EUSO will detect such particles by observing the fluorescence and Cherenkov photons produced during their pass in the atmosphere. The main objective of JEM-EUSO is doing astronomy and astrophysics through the particle channel with extreme energies above several times 1019eV with a significant statistics beyond the Greisen–Zatsepin–Kuzmin (GZK) cut-off. Moreover, JEM-EUSO could observe extremely high energy neutrinos. JEM-EUSO has been designed to operate for more than 3 years onboard the ISS orbiting around the Earth every 90min at an altitude of about 400km. JAXA has selected JEM-EUSO as one of the mission candidates of the second phase utilization of JEM/EF for the launch in mid 2010s.

Space based studies of UHE neutrinos

The Universe at Ultra-High Energies (UHE) above E > 6 × 10 19 eV is largely unexplored. In this paper we focus on the search for UHE neutrinos. After briefly summarizing the science rationale for neutrino studies at UHE, we describe the Extreme Universe Space Observatory (EUSO) onboard the Japanese Experiment Module (JEM) of the International Space Station.

Development of a Tether Based Space Walking Robot to Be Tested on ISS/KIBO

A unique space robot is proposed to support astronauts in space. The robot moves around the surface of a space facility, e.g. a space station using its handrails and tethers that the robot has. This unique mechanism of the proposed robot makes it possible to realize the robot in a small volume while the robot can move around the wide area. In order to demonstrate usefulness of this unique robot, an onboard experiment on the exposed facility of the International Space Station Japanese Experiment Module, “KIBO” will be conducted in the year 2012. Development of the experiment system is progressing now.

Review of the Development of Robotic Manipulator for International Space Station

In extreme environment of the space,most of Extra-Vehicular Activity(EVA) has to depend on the aid of robotic manipulator.As a main part of International Space Station(ISS), robotic manipulator is playing a crucial role in the on-orbit assembly,external maintenance and the operations of ISS,and it therefore allays the working time and frequency of astronauts EVA.This paper reviews the development of the robotic manipulator based on ISS member countries' research, including shuttle remote manipulator,space station remote manipulator,European robotic arm, Japanese experiment module remote manipulator and German manipulator.It is expected that the concerning research will provide some references for the design of Chinese robotic manipulator.

Space Environment Data Acquisition with the Kibo Exposed Facility on the International Space Station (ISS)

The Space Environment Data Acquisition equipment (SEDA), which was mounted on the Exposed Facility (EF) of the Japanese Experiment Module (JEM, also known as Kibo) on the International Space Station (ISS), was developed to measure the space environment along the orbit of the ISS. This payload module, called the SEDA-Attached Payload (AP), began to measure the space environment in August 2009. This paper reports the mission objectives, instrumentation, and current status of the SEDA-AP.

Overview of the Natural Space Environment and ESA, JAXA, and NASA Materials Flight Experiments

AbstractSpace environmental effects on materials are very severe and complex because of the synergistic interaction of orbital environments such as high-energy radiation particles, atomic oxygen, micrometeoroids, orbital debris, and ultraviolet irradiation interacting synergistically, along with thermal exposure. In addition, surface degradation associated with contamination can negatively impact optics performance. Materials flight experiments are critical to understanding the engineering performance of materials exposed to specific space environments. Likewise, the spacecraft designer must have an understanding of the specific environment in which a spacecraft will operate, enabling appropriate selection of materials to maximize engineering performance, increase mission lifetimes, and reduce risk. This article will present a methodology for assessing the engineering performance of materials baselined for a specific spacecraft or mission. In addition, an overview of the space environment, from low Earth orbit to interplanetary space, will be provided along with an overview on the effects of the space environment on materials performance. The majority of this article is devoted to materials flight experiments from the European Space Agency (ESA), the Japan Aerospace Exploration Agency (JAXA), and from the National Aeronautics and Space Administration (NASA). Some of the experiments reviewed include ESA's Materials Exposure and Degradation Experiment on the International Space Station (ISS), JAXA's Micro-Particles Capturer and Space Environment Exposure Device experiments on the ISS Service Module and on the ISS Japanese Experiment Module Exposed Facility, and NASA's Long Duration Exposure Facility satellite and the Materials International Space Station Experiment series flown on the exterior of ISS.

Measurement of the pressure broadening coefficient of the 625GHz transition of in the sub-millimeter-wave region

The hydrogen peroxide ( H 2 O 2 ) molecule plays an important role in stratospheric ozone chemistry as a reservoir molecule in the HO X cycle. The Superconducting Sub-Millimeter-Wave Limb Emission Sounder (SMILES) instrument in the Japanese Experiment Module (JEM) on the International Space Station monitors H 2 O 2 using the pure rotational J Ka , Kc = 20 1 , 19 – 19 2 , 17 transition at 625.044 GHz in the ground vibronic state. Accurate retrievals of H 2 O 2 abundances rely on a knowledge of pressure broadening effects for this transition, and the required nitrogen ( N 2 ) and oxygen ( O 2 ) broadening coefficients are measured here for the first time. Values of the pressure broadening coefficients, γ ( N 2 ) = 4.03 ± 0.06 MHz / Torr and γ ( O 2 ) = 2.49 ± 0.04 MHz / Torr are obtained at room temperature, with statistical 3 σ uncertainties given. The value for air broadening is then derived to be γ ( air ) = 3.71 ± 0.09 MHz / Torr , where the uncertainty includes possible systematic errors.

JEM-EUSO mission on the ISS with the aim of performing particle astronomy

The Extreme Universe Space Observatory (EUSO) is a science mission to investigate the nature and origin of Extremely-High-Energy Cosmic Rays (EHECRs) with primary energy(E 0 ) > 7 × 10 19 eV . It will be installed in the Japanese Experiment Module (JEM) on the International Space Station (ISS). This mission is aimed to perform charged-particle astronomy in this energy region with large statistics of EHECRs (>1000 events above 7 × 10 19 eV ) in 5 years observation. The JEM-EUSO telescope has a Field of View(FoV) of 60 ° × 48 ° and a cumulative exposure of > 4 × 10 5 km 2 ⋅ sr ⋅ yr . It consists of high-transmittance Fresnel lenses (a side-cut shape with a 2.65 m major axis), a cluster of multi-anode photomultipliers(MAPMT) as a photo-sensitive detector at the focal surface and suitable electronics. JEM-EUSO has been selected as one of the mission candidates of the second phase utilization of JEM expected in early 2010s, by the Japan Aerospace eXploration Agency(JAXA).

Simulated performance of the calorimetric electron telescope (CALET) experiment

CALET is a detector planned to be on-board the Japanese Experiment Module Exposed Facility (JEM-EF) of the International Space Station. The CALET mission aims at revealing unsolved problems in high energy phenomena of the Universe by carrying out a precise measurement of the high energy electrons in 1 GeV–20 TeV, the gamma-rays in 20 MeV to a few TeV and the nuclei in a few 10 GeV–1000 TeV. The main detector is composed of imaging calorimeter (IMC), total absorption calorimeter (TASC), silicon pixel array (SIA) and anti-coincidence detector (ACD) to detect various kinds of particles in very wide energy range. The total absorber thickness is 31 radiation lengths for electromagnetic particles and 1.4 interaction mean free paths for protons. Monte Carlo simulation study has been carried out for optimization of the detector performance in observing each kind of particles. We obtained following performance about the observation of very high energy (>100 GeV) electrons, which is a main target of the CALET experiment: (1) Effective geometrical factor is about 7000 cm 2 sr. (2) Energy resolution is better than a few %. (3) Angular resolution is better than 0.1°. (4) Proton rejection power is ∼10 5 with the electron detection efficiency better than 95%. We also present the simulated performance of the CALET experiment in observing other particles.

The MAXI Mission on the ISS: Science and Instruments for Monitoring All-Sky X-Ray Images

Abstract The Monitor of All-sky X-ray Image (MAXI) mission is the first astronomical payload to be installed on the Japanese Experiment Module — Exposed Facility (JEM-EF or Kibo-EF) on the International Space Station. It has two types of X-ray slit cameras with wide FOVs and two kinds of X-ray detectors consisting of gas proportional counters covering the energy range of 2 to 30 keV and X-ray CCDs covering the energy range of 0.5 to 12 keV. MAXI will be more powerful than any previous X-ray All Sky Monitor payloads, being able to monitor hundreds of Active Galactic Nuclei. A realistic simulation under optimal observation conditions suggests that MAXI will provide all-sky images of X-ray sources of $\sim $20 mCrab ($\sim $7 $\times$ 10$^{-10} $erg cm$^{-2} $s$^{-1}$ in the energy band of 2–30 keV) from observations during one ISS orbit (90 min), $\sim $4.5 mCrab for one day, and $\sim $2 mCrab for one week. The final detectability of MAXI could be $\sim $0.2 mCrab for two years, which is comparable to the source confusion limit of the MAXI field of view (FOV). The MAXI objectives are: (1) to alert the community to X-ray novae and transient X-ray sources, (2) to monitor long-term variabilities of X-ray sources, (3) to stimulate multi-wavelength observations of variable objects, (4) to create unbiased X-ray source cataloges, and (5) to observe diffuse cosmic X-ray emissions, especially with better energy resolution for soft X-rays down to 0.5 keV.

Operational retrieval algorithms for JEM/SMILES level 2 data processing system

To measure the thermal emission from stratospheric minor species with high sensitivity, the Superconducting Submillimeter-wave Limb-Emission Sounder (SMILES) aboard the Japanese Experiment Module (JEM) of the International Space Station (ISS) carries 4 K cooled Superconductor–Insulator–Superconductor (SIS) mixers. The major feature of the SMILES is its high-sensitive measurement ability with low system noise temperature less than 700 K. As a part of the ground system for the SMILES, a level 2 data processing system (DPS-L2) has been developed. It retrieves the density distributions of the target species from calibrated spectra in near-real-time. The retrieval process consists of two parts: the forward model, which computes radiative transfer, and the inverse model, which deduces atmospheric states. Since the forward model must provide the most accurate basis for results and be implemented under limited computing resources, the forward model algorithm for an operational system has to be accurate and fast. Hence, the algorithm is improved (1) by designing accurate instrument functions such as the instrumental field of view (FOV), sideband rejection ratio of sideband separator, and spectral responses of acousto-optic spectrometer (AOS) and (2) by optimizing radiative transfer calculation. This paper presents the development of the DPS-L2 along with the details on its algorithm and the algorithm performance. The accuracy of this algorithm is better than 1%, and the processing time for single-scan spectra is less than 1 min with eight parallel processings using a 3.16-GHz Quad-Core Intel Xeon processor. Thus, this algorithm is suitable for the SMILES measurement.

The JEM-EUSO mission

JEM-EUSO is a space science mission to explore the extreme energies and physics of the Universe. Its instrument will watch the darkside of the earth and will detect UV photons emitted from the extensive air shower caused by an ultra-high energy cosmic ray (UHECR above 1018 eV), or an extremely high energy cosmic ray (EHECR) particle (e.g. above about 1020 eV). Such a high-rigidity particle as the latter arrives almost in a straight line from its origin through the magnetic fields of our Milky Way Galaxy and is expected to allow us to trace the source location by its arrival direction. This can open the door to new astronomy with charged particles. In its 5 years of operation including the tilted mode, Extreme Universe Space Observatory an Japanese Experiment Module (JEM-EUSO) will detect at least 1000 events with E>7×1019 eV with the Greisen–Zatsepin–Ku'zmin (GZK) suppression spectrum. It can determine the energy spectrum and source locations of GZK to super-GZK regions with a statistical accuracy of several percent. JEM-EUSO is planned to be deployed by H2 transfer vehicle (HTV) and will be attached to the Japanese Experiment Module/ Exposure Facility (JEM/EF) of International Space Station. JAXA has selected JEM-EUSO as one of the mission candidates of the second phase utilization of JEM/EF for launch in the early-to-mid 2010s.

The JEM-EUSO Mission

The Extreme Universe Space Observatory (EUSO) on Japanese Experiment Module (JEM) is a science mission on the International Space Station (ISS) led by the Japan Aerospace eXploration Agency (JAXA) to investigate the nature and origin of Extreme Energy Cosmic Rays (EECR) beyond energy E 0 > 7 × 10 19 eV . The main objective of the mission is to perform charged-particle astronomy in this energy region by collecting a large sample of events (∼1000 events above E 0 ) in 3-5 years of operation, measure their energy, arrival direction and composition with sufficient accuracy ( Δ E 30 % , Δ ang 2 ° , hadron/photon/neutrino separation Δ X max 120 g / cm 2 ). With the above statistics, dozen of events per source are expected, which are enough to infer their energy spectrum. JEM-EUSO is a wide-angle telescope (field of view ±30°, integrated aperture > 4 × 10 5 km 2 ⋅ sr ⋅ yr ) and consists of high-transmittance Fresnel lenses with a 2.5 m diameter, an advanced photo-sensitive detector at the focal surface and a suitable electronics. An infrared camera and a LIDAR system will be also used to monitor the earth's atmosphere. JEM-EUSO has been selected by JAXA as one of the mission candidates of the second phase utilization of JEM / Exposed Facility (JEM/EF) with launch expected in early 2010s and it is right now undertaking the Phase-A (concept study and technical feasibility). The scientific motivations of the mission, its objectives and expected performance are here summarized together with its links with other space-based projects such as Super-EUSO.

"Myo Lab": A JAXA Cell Biology Experiment in "Kibo (JEM)" of the International Space Station

Skeletal muscle atrophy is an often-unavoidable response to a prolonged lack of muscle use or spaceflight (referred to as unloading), and presents a particular challenge for astronauts during spaceflight. An increased understanding of the molecular mechanisms of muscle atrophy may lead to the development of effective therapies to combat this widespread condition. In this project, we aim to elucidate the molecular mechanisms of microgravity-induced skeletal muscle atrophy, especially physiological relevance of Cbl-b ubiquitin ligase. Japanese experimental module (JEM), Kibo, in International Space Station has been constructed until June, 2009. This enables us to perform cell culture experiment, which is an easy system to observe direct effects of microgravity on the cell, in space for a long term. This project is called Myo Lab, which means Laboratory for Skeletal Muscle. This decal images our dream (space shuttle) that flight beyond Earth forward to Kibo. In addition, the flame from shuttle means skeletal muscle.

CALET Measurements of Cosmic Ray Electrons in the Heliosphere

The CALorimetric Electron Telescope (CALET) mission has been proposed to measure electrons and gamma rays in a wide energy range on the Japanese Experiment Module (JEM)/International Space Station (ISS) and approved for the phase A study by the Japan Aerospace Exploration Agency (JAXA). In this paper we present the purposes of the CALET mission pertaining to solar physics and expected results from measurements of electrons in the 1–100 GeV energy range. Cosmic rays in this energy region are largely modulated by solar activity and their intensity has both long-term and short-term variations. Measuring such variations precisely will give new information about the transport of cosmic rays in the heliosphere. We estimate the energy dependence of the diffusion of cosmic rays through the solar magnetic field and verify some transport models. Electrons in this energy range are mostly negative though CALET does not distinguish the sign of charges directly. We therefore investigate the charge sign dependence of va...

C. elegans RNAi space experiment (CERISE) in Japanese Experiment Module KIBO

We have started a space experiment using an experimental organism, the nematode Caenorhabditis elegans, in the Japanese Experiment Module, KIBO, of the International Space Station (ISS). The specimens were boarded by space shuttle Atlantis on mission STS-129 which launched from NASA Kennedy Space Center on November 16, 2009. The purpose of the experiment was several-fold: (i) to verify the efficacy of RNA interference (RNAi) in space, (ii) to monitor transcriptional and post-translational alterations in the entire genome in space, and (iii) to investigate mechanisms regulating and countermeasures for muscle alterations in response to the space environment. In particular, this will be the first study to utilize RNAi in space.

On-board and Ground Data Processing System of MAXI

MAXI (Monitor of All sky X-ray Image) is the first X-ray observation payload to be installed to EF (Exposed Facility) of Kibo (JEM: Japanese Experiment Module) on ISS (International Space Station). One of the important missions of MAXI is to quickly release novae or transient information of X-ray sources through its alert system to the worldwide astronomers. For this purpose, MAXI is equipped with a unique data transfer system both for the ground and on-board handling, which fully utilizes the communication system of ISS. The uniqueness of the data transfer system of MAXI comes from the fact that it is a payload of ISS, and is not seen in the ordinary payloads on free flyers (satellites). MAXI analyzes the observation data automatically in real time, and an alert for the novae or transient sources can be distributed widely through internet based on the analysis result. Various restrictions are imposed to keep tight security even on the ground system of ISS payloads. This paper describes the data transmission process in each stage, namely that in MAXI, the ISS communication links between the ISS and ground, and the process in the MAXI ground system.

CALET Mission for the Observation of Cosmic Rays on the International Space Station

We have proposed CALET (CALorimetric Electron Telescope) mission to make observations of high energy cosmic rays, electrons, gamma-rays, and nuclei, on the International Space Station (ISS). CALET mission has been approved as one of candidates for the next mission utilizing the Japanese Experiment Module (JEM). The detector of CALET consists of an imaging calorimeter (IMC) and a total absorption calorimeter (TASC). Main objective of cosmic-ray observation with CALET is to determine precise energy spectrum of electrons up to 20 TeV. As the super nova remnants (SNR) are taken to be sources of electrons, some structure caused by nearby electron sources is expected to appear in the energy spectrum over 1 TeV. Gamma-rays from 20 MeV to a few TeV can be also observed by CALET. Because a thick TASC of CALET gives high energy resolution, annihilation line of SUSY particle, which is a candidate of the dark matter, can be detected. Observation of nuclei is also possible up to 1000 TeV owing to the thick TASC. We have been going on conceptual design of CALET to clear a next judgment in one or two years to proceed to practical development for launching in 2013.

On-Orbit Verification of Space Inflatable Structures

This paper gives an overview of the currently planned on-orbit space verification experimental device complex composed of multiple inflatable demonstration units, proposed by the authors' group. The compact device named SIMPLE is designed to be suitable for one of the shared experimental installations that constitute a single experimental block attached to the Exposed Facility of Kibo Japanese Experimental Module (JEM) of ISS. The SIMPLE mission was accepted by JAXA as the candidate of the secondary application of the Exposed Facility of JEM at the end of last year.

Proposal of a Tethered Space Walking Robot - REX-J: Robot Experiment on JEM -

A unique space robot is proposed to support astronauts' EVA work. The robot moves around the surface of a space facility, e.g. a space station. Usefulness of the proposed robot system will be tested in 2012 on the International Space Station Japanese Experiment Module.