We present the C III λ977, O VI λλ1032, 1038 and N IV] λ1486 emission line maps of the Cygnus Loop, obtained with the newly processed data of Spectroscopy of Plasma Evolution from Astrophysical Radiation (SPEAR; also known as FIMS) mission. In addition, the Si IV+O IV] line complexes around 1400Å are resolved into two separate emission lines, whose intensity demonstrates a relatively high Si IV region predicted in the previous study. The morphological similarity between the O VI and X-ray images, as well as a comparison of the O VI intensity with the value expected from the X-ray results, indicates that large portions of the observed O VI emissions could be produced from X-ray emitting gas. Comparisons of the far-ultraviolet (FUV) images with the optical and H I 21 cm images, reveal spatial variations of shock-velocity populations and high FUV extinction in the direction of a previously identified H I cloud. By calculating the FUV line ratios for several subregions of the Cygnus Loop, we investigate the spatial variation of the population of radiative shock velocities; and the effects of resonance scattering, X-ray emitting gas, and non-radiative shocks. The FUV and X-ray luminosity comparisons between the Cygnus Loop and the Vela supernova remnant suggest that the fraction of shocks in the early evolutionary stages is much larger in the Cygnus Loop.

In this paper, we present a catalogue of the spectra of bright stars observed during the sky survey using the Far-Ultraviolet Imaging Spectrograph (FIMS), which was designed primarily to observe diffuse emissions. By carefully eliminating the contamination from the diffuse background, we obtain the spectra of 70 bright stars observed for the first time with a spectral resolution of 2-3Å over the wavelength of 1370-1710Å. The far-ultraviolet spectra of an additional 139 stars are also extracted with a better spectral resolution and/or higher reliability than those of the previous observations. The stellar spectral type of the stars presented in the catalogue spans from O9 to A3. The method of spectral extraction of the bright stars is validated by comparing the spectra of 323 stars with those of the International Ultraviolet Explorer (IUE) observations.

Previously, the pitch angle distribution of monoenergetic and broadband electron precipitation has been investigated mainly by case studies. The main focus of this study is quantitative comparison of pitch angle distributions between monoenergetic and broadband electron precipitations using long-term observations on board one platform. From December 2003 to October 2004, Science and Technology Satellite-I (altitude∼680 km) regularly observed auroral electron flux and cold ambient plasma parameters during quiet and moderately disturbed conditions. Monoenergetic electron precipitation has notable perpendicular anisotropy, while broadband electron precipitation is much more field aligned. As for other features of monoenergetic and broadband electron precipitation, the characteristic energy of precipitating electrons is slightly higher for monoenergetic (around 1 keV) than for broadband electron precipitation (from several hundred eV to 1 keV). For both monoenergetic and broadband types, the characteristic energy and energy flux do not show clear correlation with cold ambient plasma density/temperature.

Precision correction is the process of geometrically aligning images to a reference coordinate system using GCPs(Ground Control Points). Many application of remote sensing data, such as change detection, mapping, and environmental monitoring, rely on the accuracy of precision correction. However it is very time consuming, laborious and expensive process. In this research, we propose a new method for automatic precision correction of satellite images using the GCP chips collected from lower resolution satellite images to reduce or eliminate the number of GCPs required. Different Earth observation satellites provide the satellite images of different resolution, different swath and different position accuracy. In general, the satellite images of lower resolution have wider swath and vice versa. In that sense, if we can utilize the GCP chips collected from lower resolution satellite images to do precision correction of the higher resolution satellite images then the number of GCPs required to have a precisely corrected images of the same area will be reduced. In this experiment, we used GCP chips collected from Landsat-7 panchromatic images of 15m resolutions to perform precision correction of the KOMPSAT-1 EOC images of 6.7m resolutions. In this case, since Landsat-7 images provide higher positional accuracy of less than 250m at the systematically corrected level (L1G) comparing about 2km positional accuracy of KOMPSAT-1, GCPs collected from level 1G of Landsat-7 images can provide enough accuracy in certain applications. To utilize this approach easily, this study will be applied to the automatic precision correction method developed previously, which exploits the normalized cross correlation and the RANSAC(Random Sample Consensus) algorithm to removed the outliers of matching results. The initial result showed the possibility of using GCP chips of lower resolution to carry out precision correction in the frame of the automatic precision correction method utilizing RANSAC algorithm.