A rare case of a patient with a large type IV aortico–left ventricular tunnel who underwent successful repair at 1 day after birth was described. To the best of our knowledge, no such cases that aortic opening was over 10 mm have been reported in the English literature. Our case demonstrated no leak or significant aortic regurgitation by a two-patch repair.

Studying a multi-dimensional structure of supernovae (SNe) gives important constraints on the mechanism of the SN explosion. Polarization measurement is one of the most powerful methods to study the explosion geometry of extragalactic SNe. Especially, Type Ib/c SNe are the ideal targets because the core of the explosion is bare. We have performed spectropolarimetric observations of Type Ib/c SNe with the Subaru telescope. We detect a rotation of the polarization angle across the line, which is seen as a loop in the Q - U plane. This indicates that axisymmetry is broken in the SN ejecta. Adding our new data to the sample of stripped-envelope SNe with high-quality spectropolarimetric data, five SNe out of six show a loop in the Q - U plane. This implies that the SN explosion commonly has a non-axisymmetric, three-dimensional geometry.

We serendipitiously found that the iron-rich low-ionization broad absorption-line (FeLoBAL) quasar SDSS J 163255.46+420407.7 showed a dramatic change in its spectrum over 3.4 years in the rest frame of the quasar. A simple photoionization model suggests the increase in the nuclear radiation caused these changes. Given the recombination coefficient of Fe+, the relaxation time of the absorbing gas suggests ne > 104 cm−3.

A parallel resistance model (PRM), in which the total resistance, Rtotal, is given by a parallel connection of resistance of a filament, Rfila, and that of a film excluding a filament, Rexcl, was proposed to understand DC electric properties of resistive RAM (ReRAM). Here, the relationship of 1/Rtotal = 1/Rfila + 1/Rexcl is satisfied. To prove the validity of this model, the dependence of the relationship between resistance and temperature, R(T), of Pt/NiO/Pt on an area of a top electrode, S, was investigated. It was clarified that R(T) depended on S, which is the result definitely expected by the PRM. It was also clarified that smaller S is crucial to observe intrinsic properties of a filament of ReRAM.

We discuss the implications for the cosmic re-ionization from the optical afterglow spectrum of GRB050904 at z = 6.3

Recently, a number of possible young globular clusters (GCs) have been found in some merging/interacting galaxies or starburst galaxies. On the other hand, it is well known that GCs are numerous in giant elliptical galaxies many of which are thought to be formed via major merger of galaxies. These facts lead us to a thought that the formation process of GCs could accompany galaxy – galaxy interaction followed by starburst. The archetypical starburst galaxy M82 is an ideal target to study the relation between galaxy interaction, starburst, and GC formation.

NGC 7319 is a member of the compact group of galaxies known as Stephan’s Quintet. The systemic velocity 6740 km s−1 gives a distance of 90Mpc (H0= 75 kms−1 Mpc−1) for NGC 7319. This galaxy has a tail and/or ring which suggests interaction with a neighboring pair of galaxies, NGC 7318A and B (e.g., Arp 1973). Durret & Warrin (1990) and Durret (1994) performed optical long-slit spectroscopy and found an extended emission-line region (EELR) in NGC 7319. They detected highly excited gas over along PA = 61° and 10″ along PA – 151°. Apart from these works, there have not been any studies on the velocity field and excitation of the gas in the EELR of NGC 7319. More details were published by Aoki et al. (1996).