The Infrared Camera (IRC) is one of two focal-plane instruments on the AKARI 1 satellite. It is designed for wide-field deep imaging and low-resolution spectroscopy in the near-to mid-infrared (1.8-26.5 µm) in the pointed observation mode of AKARI. IRC is also operated in the survey mode to make an all-sky survey at 9 and 18 µm. It comprises three channels. The NIR channel (1.8-5.5 µm) employs a 512 × 412 InSb array, whereas both the MIR-S (4.6-13.4 µm) and MIR-L (12.6-26.5 µm) channels use 256 × 256 Si:As impurity band conduction arrays. Each of the three channels has a field-of-view of about 10 ′ × 10 ′ and are operated simultaneously. The NIR and MIR-S share the same field-of-view by virtue of a beam splitter. The MIR-L observes the sky about 25 ′ away from the NIR/MIR-S field-of-view. IRC gives us deep insights into the formation and evolution of galaxies, the evolution of planetary disks, the process of star-formation, the properties of interstellar matter under various physical conditions, and the nature and evolution of solar system objects. The in-flight performance of IRC has been confirmed to be in agreement with the pre-flight expectation. This paper summarizes the design and the in-flight operation and imaging performance of IRC.

AKARI, the first Japanese satellite dedicated to infrared astronomy, was launched on 2006 February 21, and started observations in May of the same year. AKARI has a 68.5 cm cooled telescope, together with two focal-plane instruments, which survey the sky in six wavelength bands from mid–to far-infrared. The instruments also have a capability for imaging and spectroscopy in the wavelength range 2-180$\mu$m in the pointed observation mode, occasionally inserted into a continuous survey operation. The in-orbit cryogen lifetime is expected to be one and a half years. The All-Sky Survey will cover more than 90% of the whole sky with a higher spatial resolution and a wider wavelength coverage than that of the previous IRAS all-sky survey. Point-source catalogues of the All-Sky Survey will be released to the astronomical community. Pointed observations will be used for deep surveys of selected sky areas and systematic observations of important astronomical targets. These will become an additional future heritage of this mission.

AKARI (formerly ASTRO-F) is an infrared space telescope designed for an all-sky survey at 10-180 µm, and deep pointed surveys of selected areas at 2-180 µm. The deep pointed surveys with AKARI will significantly advance our understanding of galaxy evolution, the structure formation of the Universe, the nature of the buried AGNs, and the cosmic infrared background. Here we describe the important characteristics of the AKARI mission: the orbit, and the attitude control system, and investigate the optimum survey area based on the updated pre-flight sensitivities of 1 AKARI, taking into account the cirrus confusion noise as well as the surface density of bright stars. The North Ecliptic Pole (NEP) is concluded to be the best area for 2-26 µm deep surveys, while the low-cirrus noise regions around the South Ecliptic Pole (SEP) are worth considering for 50-180 µm pointed surveys to high sensitivities limited by the galaxy confusion noise. Current observational plans of these pointed surveys are described in detail. Comparing these surveys with the deep surveys with the Spitzer Space Telescope, the AKARI deep surveys are particularly unique in respect of their continuous wavelength coverage over the 2-26 µm range in broad-band deep imaging, and their slitless spectroscopy mode over the same wavelength range.

The formation and structure of the potassium complex with valinomycin in solution were studied by means of Raman and Raman optical activity (ROA) spectroscopy. The complexation caused significant spectral changes, particularly in the region 1200-1400 cm(-1). The experimental spectra were interpreted using first principles computations. A complete computational conformational search combined with the spectral analysis revealed the arrangement of the isopropyl side chains in the complex. From a total of 6579 unique conformers two predominant ones were confirmed in the solution by ROA. A third one was predicted theoretically, but its population in the experiment could be estimated only roughly. The most populated conformer does not exhibit C(3) symmetry, and is different from that present in the crystal and the NMR-derived structure. Molecular dynamics techniques were used to estimate the molecular flexibility and its effect on the spectra. Density functional computations and Cartesian coordinate transfer (CCT) techniques provided the ROA and Raman spectral shapes and intensities well comparable with the experiment. The polar solvent (methanol) environment modeled with a polarizable continuum model (PCM) leads to rather minor changes in the conformer populations and vibrational properties as compared to vacuum computations, due to the hydrophobic character of the complex. Additional computational experiments suggest that the vibrational interactions determining the ROA spectra are quite local, which contributes to the good spatial resolution of the method. A reduction of the noise in the experimental spectra as well as increased precision of the simulations is desirable for the further exploration of the potential of the ROA spectroscopy for biomolecular studies in the future.

Microemulsion capillary electrophoresis, which employed oil in water microemulsions as the electrophoretic media was demonstrated for the separation of ionic and non-ionic samples.