Search

The evolution of galaxies and the history of star formation in the Universe are among the most important topics in today’s astrophysics. Especially, the role of small, irregular galaxies in the star-formation history of the Universe is not yet clear. Using the data from the AKARI IRC survey of the Large Magellanic Cloud at 3.2, 7, 11, 15, and 24 μm wavelengths, i.e., at the mid- and near-infrared, we have constructed a multiwavelength catalog containing data from a cross-correlation with a number of other databases at different wavelengths. We present the separation of different classes of stars in the LMC in color-color, and color-magnitude, diagrams, and analyze their contribution to the total LMC flux, related to point sources at different infrared wavelengths.

In fusion plasma, the behaviour of impurities is important. In order to study the behaviour of impurities spectroscopic measurement is necessary. We are now studying EUV spectra from Large Helical Device (LHD) to study the behaviour of impurities. We present here the three kinds of EUV spectra measured from LHD.In order to analyse the observed spectra, we need atomic data. We use collisional radiative models of different ions to estimate the line intensities. To construct a collisional radiative model we need a lot of atomic data between excited states. Model and atomic data are coupled. To derive correct answers from a model we need reliable atomic data.

Energy levels, radiative transition probabilities and autoionization rates for 1s22s22p63l'nl(n= 3-12, l? n? 1) and 1s22s22p64l'nl(n= 4-7, l? n? 1) states in Mg-like iron (Fe14+) are calculated by the Hartree-Fock-relativistic method (Cowan code) and the relativistic many-body perturbation theory method (RMBPT code). Autoionizing levels above three thresholds 1s22s22p63s, 1s22s22p63p and 1s22s22p63d are considered. It is found that configuration mixings [3sns + 3pnp + 3dnd] and [3snp + 3pns + 3pnd + 3dnp] play an important role for all atomic characteristics. Branching ratios relative to the first threshold and intensity factors are calculated for satellite lines, and dielectronic recombination (DR) rate coefficients are determined for the excited 444 odd-parity and 419 even-parity states. It is shown that the contribution of the highly-excited states is very important for calculation of total DR rates. Contributions from the excited 1s22s22p63l'nlstates with n? 12 and 1s22s22p64l'nlstates with n? 7 to DR rate coefficients are estimated by extrapolation of all atomic parameters. The total DR rate coefficient is derived as a function of electron temperature.

A solid phase approach is presented for the synthesis of azapeptide inhibitors and activity based probes (ABPs) for cysteine proteases. This synthetic method allows the incorporation of diverse reactive warheads linked to different peptide recognition elements. Application of this method to the synthesis of a series of caspase probes is described.

AbstractRecent progress in the Large Helical Device (LHD) experiment during the last 2 yr is reviewed. The LHD has been extending its operational regime toward fusion-relevant conditions while taking advantage of the net-current-free heliotron concept employing a superconducting coil system. Heating capability has exceeded 10 MW, and the central ion and electron temperatures have reached 7 and 10 keV, respectively. The maximum values of beta and pulse length have been extended to 3.2% and 150 s, respectively. Several encouraging physics observations have been obtained, i.e., simultaneous achievement of the mitigation of the magnetohydrodynamic instability criteria and good confinement, and formation of an internal transport barrier. The initial results have been obtained using a local island divertor, which shows the possibility of particle control at the plasma edge.

The Porphyromonas gingivalis fimbria is an important virulence factor involved in the adherence and colonization of the organism in the oral cavity. In this study, we transformed this organism with a gene, fimA381, encoding the fimbrial subunit of P. gingivalis 381 (fimbrillin) by using the host-vector system that we developed previously and examined expression of the cloned fimA381 gene. The recombinant plasmid pYHF2 was constructed by ligating a fragment containing the fimA381 gene into the plasmid vector pYH420 and transformed into the restriction-deficient P. gingivalis host YH522. pYHF2 was autonomously maintained in YH522 cells, and the fimbrillin polypeptide (recombinant fimbrillin) was fully expressed. The molecular mass of the recombinant fimbrillin was evaluated by sodium dodecyl sulfate-polyacrylamide gel electrophoresis as 41 kDa, which was identical to that of the native fimbrillin of strain 381. The amino acid sequences of the 20 amino-terminal residues of the recombinant fimbrillin and the native fimbrillin of the strain 381 were identical. In addition, characteristic long and thin fimbrial structures (recombinant fimbriae) that were distinguishable from the host's native fimbriae when examined by immunogold electron microscopy were observed around the cell surface of the transformants containing the fimA381 gene. These results suggested that transformation of fimA gene from a different strain of P. gingivalis followed by accumulation of the mature fimbrial subunit protein was sufficient for production of fimbrial structures that were observable by electron microscopy.

Not Available

NIFS (National Institute for Fusion Science) Atomic and Molecular Numerical Database is introduced. Atomic and molecular data of various collision processes in plasma are collected and input to the database. The database is accessible via internet and data can be retrieved by querying an element name, an ionic stage, or other conditions. Numerical data are shown as a table and a graph which can be downloaded as a PDF file. Our other data activities on data compilation, evaluation, and production are also introduced.

An enzyme system of Nocardia diaphanozonaria JCM 3208 catalyzes the inversion of the chirality of various α-substituted carboxylic acids, such as 2-phenylpropanoic acid and 2-phenoxypropanoic acid derivatives, via a novel deracemization reaction.

Continuous tuning of the oscillation frequency of a continuous-wave Raman fibre-optic laser has been demonstrated. The device operates over a 3 nm band in the visible range and exhibits low threshold and high conversion efficiency.

Aims. The aim of this study is to understand the chemical conditions of ices around embedded young stellar objects (YSOs) in the metal-poor Large Magellanic Cloud (LMC).

Aims. The aim of this study is to understand the chemical conditions of ices around embedded young stellar objects (YSOs) in the metal-poor Large Magellanic Cloud (LMC).Methods. We performed near-infrared (2.5-5 μm) spectroscopic observations toward 12 massive embedded YSOs and their candidates in the LMC using the infrared camera (IRC) onboard AKARI. We estimated the column densities of the H2O, CO2, and CO ices based on their 3.05, 4.27, and 4.67 μm absorption features, and we investigated the correlation between ice abundances and physical properties of YSOs.Results. The ice absorption features of H2O, CO2, 13CO2, CO, CH3OH, and possibly XCN are detected in the spectra. In addition, hydrogen recombination lines and PAH emission bands are detected toward the majority of the targets. The derived typical CO2/H2O ice ratio of our samples (~0.36 ±0.09) is greater than that of Galactic massive YSOs (~0.17 ±0.03), while the CO/H2O ice ratio is comparable. It is shown that the CO2ice abundance does not correlate with the observed characteristics of YSOs: the strength of hydrogen recombination line and the total luminosity. Likewise, clear correlation is not seen between the CO ice abundance and YSO characteristics, but it is suggested that the CO ice abundance of luminous samples is significantly lower than in other samples.Conclusions. The systematic difference in the CO2 ice abundance around the LMC's massive YSOs, which was suggested by previous studies, is confirmed with the new near-IR data. We suggest that the strong ultraviolet radiation field and/or the high dust temperature in the LMC are responsible for the observed high abundance of the CO2ice. It is suggested that the internal stellar radiation does not play an important role in the evolution of the CO2ice around a massive YSO, while more volatile molecules like CO are susceptible to the effect of the stellar radiation.