목적: 비구면 디자인의 소프트 콘택트렌즈 ASCL(aspheric soft contact lens)로 굴절교정을 한 젊은 성인 근시안에서 콘택트렌즈 착용 후 안구의 구면수차와 코마수차 변화를 확인하였다. 방법: 건강한 성인 근시안 50명(평균 연령: 23.15±1.70세, 평균 등가구면굴절력: –2.90±1.75 D)을 대상으로 굴절교정용 ASCL(Biotrue, Bausch+Lomb, USA)을 착용시킨 후 검사실의 조도 100 lx에서 고위수차와 동공크기를 측정하였다. 고위수차는 Wavefront Analyzer를 사용하여 동공크기 4 mm 영역에서 측정하였고, 동공크기는 Pupillometer를 이용하여 3.5 m 거리의 물체를 주시하도록 한 후 암소시(scotopic condition, light off) 상태에서 측정하였다. 결과: 20대 근시안의 구면수차와 코마수차는 0.026±0.031 ㎛, 0.078±0.039 ㎛, ASCL 착용 후에는 0.019±0.026 ㎛ and 0.082±0.038 ㎛로 구면수차는 감소하고 코마수차는 유의하게 증가하였다. 대상안 중 구면수차가 감소한 경우는 전체의 68%로 양의 구면수차를 갖는 대상안에서 감소하였고, 증가한 경우는 11%로 음의 구면수차를 갖는 대상안에서 증가하였다. 코마수차는 대상안의 53%에서 증가하였고 19%에서는 변함이 없었으며 28%에서 감소하였다. 약도 및 중등도 근시안에서 구면수차는 근시도와 상관성이 없었고, 코마수차는 근시도가 높을수록 큰 것으로 나타났다. 결론: 조절자극이 없는 암소시 상태에서 ASCL 착용 후 안구의 구면수차는 양의 값을 갖는 경우에는 감소 하지만 음의 값을 갖는 경우에는 증가하였고, 이는 ASCL 디자인과 동공크기가 영향을 준 것으로 생각된다.

Based on the database of 128 disk galaxies (66 SO, 62 S and Irr) mailnly compiled from Kent and Gunn (1982) and Doi et a1.(1995) which is complete down to m < 15.6 mag within a radius of 3°, the orientation of spin vectors of disk galaxies of the Coma cluster has been analyzed. The results confirm the morphological dependence of the orientation of disk galaxies found from the analsis of the Virgo cluster. Common features of orientation of disk galaxies of both clusters are outlined.

A velocity inhomogeneity, which is defined as a regional preponderence of either radial or tangential orbits, is searched with a new technique for the Coma cluster of galaxies. It is found within ~2h-1 Mpc from the cluster center that the Coma shows conspicuous inhomogeneities in velocity and that the inhomogeneities are real at a 99% level of confidence. Even in the central region (7' - 30' from the center), zones that are dominated by radial and tangential orbits are distinguishable. Defining the cluster's 'equator' as the direction defined by the Coma-A1367 supercluster, tangential orbits dominate the 'polar' zones in the central region. Galaxies that are located in 30'-100' also inhomogeneous in velocity in that the 'polar' zones are mostly radial while the rest is nearly homogeneous. These results indicate that the Coma galaxies are exceedingly more radial in orbit, implying that merging or infalls are either still going on or an earlier virialization is likely to have occurred preferentially near the 'equator'. Incorporating the velocity inhomogeneity into mass estimators, the most appropriate mass is turned out to be 0.4×1015h-1M⊙ (R ≤ 0.6h-1 Mpc),and 1.0\times10×15h-1 M⊙ (R≤ 2.1h-1Mpc). The corresponding mass to blue light ratio on the average is ~300h. These estimates are consistent with Merritt (1987) and Hughes (1989) and the MILE is seemed to favour the mass-follows-light models than the uniform spread of dark matter throughout the cluster.

A velocity inhomogeneity, which is the regional preponderence of either radial or tangential orbits, is searched with the new technique proposed by Kim (1992) for Coma, Hydra I, and Abell 2256 cluster of galaxies. Conspicuous inhomogeneities are found in the Coma and A2256 which X-ray isophotes are indicative for their underlying potentials being ellipitcal in shape, Even in their central regions, zones that are dominated by radial orbits are clearly distinguishable from that of the tangential orbits, and defining the cluster 'equator' as the direction of maximum elongation of the X-ray isophotes, radial orbits dominate along this direction whereas tangential orbits dominate the 'polar' zones. Merger events that are evidenced in X-ray observations occur in the equatorial zones of Coma and A2256, suggesting preponderence of radial orbits in the zones, which is in good agreement with their velocity structures. On the other hand, the inhomogeneity in Hydra I turns out to be insignificant in the central regions and this is just what is expected from a cluster whose X-ray isophotes is nearly circular. The velocity distribution in regions further out, however, shows significant inhomogeneity and this seems to support the previous results that this cluster is likely to have substructures and velocity anisotropy.

In the presence of synchrotron losses, diffusion of an ensembel of relativistic particles in an intraculster medium is investigated. The diffusion coefficient in the medium is found to be constrained by 28.8 ± 0.4 ≤ L o g D ≤ 30.5 ± 0.4 c m 2 s − 1 with the energy dependency of D 0 ε μ of μ = 0.4 ± 0.2 as the previous observations suggested. As an important implication of the result, the brightest head-tail radio source NGC 4869, whose radio tail structure is indicative for its orbit within the cluster core, is considered to be the major contributor of particles for the formation of the Coma radio halo.