Keigo Enya

THE TYPE IC HYPERNOVA SN 2002AP

Photometric and spectroscopic data of the energetic Type Ic supernova (SN) 2002ap are presented, and the properties of the SN are investigated through models of its spectral evolution and its light curve. The SN is spectroscopically similar to the hypernova SN 1997ef. However, its kinetic energy [~(4-10) ? 1051 ergs] and the mass ejected (2.5-5 M?) are smaller, resulting in a faster evolving light curve. The SN synthesized ~0.07 M? of 56Ni, and its peak luminosity was similar to that of normal SNe. Brightness alone should not be used to define a hypernova, whose defining character, namely very broad spectral features, is the result of high kinetic energy. The likely main-sequence mass of the progenitor star was 20-25 M?, which is also lower than that of both hypernovae SN 1997ef and SN 1998bw. SN 2002ap appears to lie at the low-energy and low-mass end of the hypernova sequence as it is known so far. Observations of the nebular spectrum, which is expected to dominate by the summer of 2002, are necessary to confirm these values.

Automated observatory for multicolor active galactic nuclei monitoring (MAGNUM)

We present the outline and the current status of the MAGNUM automated observation system. The operational objective of the MAGNUM Project is to carry out long-term multi-color monitoring observations of active galactic nuclei in the visible and near-infrared wavelength regions. In order to obtain these observations, we built a new 2 m optical-infrared telescope, and sited it at the University of Hawaiis Haleakala Observatory on the Hawaiian Island of Maui. Preliminary observations were started early in 2001. We are working toward the final form of the MAGNUM observation system, which is an unmanned, automated observatory. This system requirement was set by considering that the observation procedures are relatively simple, and the targets must be observed consistently over many years.

The mid-infrared imager, spectrometer, coronagraph (MISC) for the Origins Space telescope (OST)

The Mid-infrared Imager, Spectrometer, Coronagraph (MISC) is one of the instruments studied both for the Origins Space Telescope (OST) Mission Concept 1 and 2. The MISC for OST Mission Concept 1 consists of the MISC imager and spectrometer module (MISC I and S), the MISC coronagraph module (MISC COR) and the MISC transit spectrometer module (MISC TRA). The MISC I and S offers (1) a wide field (3 arcminx3 arcmin) imaging and low-resolution spectroscopic capability with filters and grisms for 6-38 μm, (2) a medium-resolution (R~1,000) Integral Field Unit (IFU) spectroscopic capability for 5- 38 μm and (3) a high-resolution (R~25,000) slit spectroscopic capability for 12-18 μm and 25-36 μm. The MISC COR module employs PIAACMC coronagraphy method and covers 6-38 μm achieving 10-7 contrast at 0.5 arcsec from the central star. The MISC TRA module employs a densified pupil spectroscopic design to achieve 3-5 ppm of spectro-photometric stability and covers 5-26 μm with R=100-300. The MISC for OST Mission Concept 2 consists of the MISC wide field imager module (MISC WFI) and the MISC transit Spectrometer module (MISC TRA). The MISC WFI offers a wide field (3 arcmin ×3 arcmin) imaging and low-resolution spectroscopic capabilities with filters and grisms for 6-28μm. The MISC TRA module in the OST Mission Concept 2 also employs the densified pupil spectroscopic design to achieve <5 ppm of spectro-photometric stability and covers 4-22 μm with R=100-300. The highest ever spectrophotometric stability achieved by MISC TRA enables to detect bio-signatures (e.g., ozone, water, and methane) in habitable worlds in both primary and secondary transits of exoplanets and makes the OST a powerful tool to bring an revolutionary progress in exoplanet sciences. Combined with the spectroscopic capability in the FIR provided by other OST instruments, the MISC widens the wavelength coverage of OST down to 5μm, which makes the OST a powerful tool to diagnose the physical and chemical condition of the ISM using dust features, molecules lines and atomic and ionic lines. The MISC also provides the OST with a focal plane guiding function for the other OST science instruments as well as its own use.

Optical/mechanical design of the focal plane receiver of the Ganymede Laser Altimeter (GALA) for the Jupiter Icy Moons Explorer (JUICE) mission

The Jupiter Icy Moons Explorer (JUICE) mission of the European Space Agency to be launched in 2022 will provide an opportunity for a dedicated exploration of the Jovian system including its icy moons. The Ganymede Laser Altimeter (GALA) has been selected as one of the ten payloads of JUICE. GALA will enable unique studies of the topography and shape, tidal and rotational state, and geology of primarily Ganymede but also Europa and Callisto. The GALA project is an ongoing international collaboration led by Germany, together with Switzerland, Spain, and Japan. This paper presents the optical and mechanical design of the focal plane receiver, the Japanese part of GALA.

A lightweight mirror made of a magnesium alloy for space-borne telescopes and instruments

We present a lightweight mirror made of a magnesium alloy for applications to space-borne telescopes and optics in instruments. A non-flammable magnesium alloy was recently developed. We consider this alloy to be a promising material for a lightweight mirror due to its high stiffness, high fracture toughness, low density, and suitability for machining. First, small flat mirrors were fabricated to obtain and improve the fabrication conditions. Then, a 175-mm magnesium-alloy mirror, with a spherical mirror surface and a backside hexagonal cutout structure to reduce the mass of the mirror, was designed and fabricated. The spherical mirror surface was fabricated using a diamond-turning process. The evaluated residual of the surface figure of the 175-mm mirror from the design is 0.90 μm rms. The deformation caused by the jig used for the fabrication was one of the major factors that increased the residual of the surface figure. The surface roughness of the 175-mm mirror was evaluated, and values of Sa = 9.6 nm and Sq = 12.6 nm were obtained by averaging the data of four measurements with a 167 μm × 167 μm field of view. Methods to improve the mirror surface are discussed. We also discuss space-borne telescopes and instruments for which this magnesium alloy is one of promising materials.

High-contrast apodization baffle for instruments onboard solar system exploration missions

We present concept and laboratory demonstration of high-contrast apodization baffle for instruments to be carried on exploration missions of the solar system. The primary science objective of the high-contrast baffle is to reveal escape of atmosphere on Mars, while other faint objects around blight sources are potential targets. We diverted heritages studied for exoplanet science and instrumentation to this work. The apodization in this work is realized by edge with microscopic Gaussian shaped structure. A simulation to confirm the concept and design of the high-contrast apodization baffle was carried out. Then, a baffle which was consisting of transparent flat substrate and thin film of aluminum on it was manufactured. The experiment was executed with He-Ne laser with wavelength of 633 nm. As the result, it was demonstrated that the apodization by the Gaussian edge is significantly working to improve the contrast. Achieved contrast is better than 10-6.5 and 10-8 in θ > 0.5 degree and θ > 1 degree, respectively. These results satisfy the requirement for remote sensing of the atmospheric less on Mars.

PIAA coronagraph for Origins Space telescope (OST) mid-infrared imager, spectrometer, coronagraph (MISC) instrument

The Mid-infrared Imager, Spectrometer Coronagraph (MISC) instrument studied for the Origins Space Telescope (OST) Mission Concept 1 is designed to observe at mid-infrared (MIR) wavelengths ranging from 5 to 38 microns for OST. In the OST Mission Concept 1 study, MISC consists of three separate optical modules providing imaging, spectroscopy, and coronagraph capabilities. The MISC Coronagraph module (MISC COR) employs Phase-Induced Amplitude Apodization (PIAA) coronagraph (Guyon et al. 2014) in which pupil apodization is modified by reflection on mirrors and central starlight is blocked by focal plane mask and Lyot mask. The performance target of MISC COR is to achieve 10-7 contrast at 0.5” from the central star with covering wavelength of 6-38 microns using 2 optical channels. MISC COR will be a powerful tool to bring a revolutionary progress in exoplanet sciences. In this paper, we present detailed design of its optics and optomechanics, and discuss expected performances for a variety of combination of focal plane mask and Lyot mask.