Optimum hypering conditions are found for IIIa-J, IIIa-F, 103a-O, 103a-D, and IIa-O plates using hypersensitization machine in KAO. For every experimental plate we get speed gain, fog increment, signal to noise ratio and relative DQE according to hypering time and temperature. The hypersensitization method is baking with 8% hydrogen mixed gas. For IIIa-J, 103a-O, and 103a-D plates treated 65∘C 65∘C , 3 hours baking, the speed gains arc increased by about 10 times, 2 times, and 2 times compared to untreated plates, respectively. The fogs are increased by 0.08, 0.10, and 0.08, respectively. For IIIa-F, IIa-O plates treated 65∘C 65∘C , 2 hours baking, the speed gains are increased by about 4.7 times and 1.8 times compared to untreated plates, respectively. The fogs are increased by 0.15 and 0.04, respectively.

Astronomical plates have a very large density range (dynamical range). Many exposed astronomical photographic plates do not provide detailed structures for very high densities, and some include hidden images for very low densities. The former can be fixed through 'Unsharp Masking' technique and the latter through 'Image Amplification' technique. Besides, we can find intrinsic colors of celestial bodies through 'Tri Color Composition' technique. Images of several plates which were observed from Sobaek Observatory with 61cm telescope are reproduced by the three kinds of image reproducing techniques. As reproduced image examples, we display an Orion nebula and a waxing crescent moon images through unsharp masking technique and an M81 image through image amplification technique. An Orion nebula and a Dumbbell nebula images are also given as results of tri color composition technique.

우리 은하계내 field RR Lyrae 변광성의 관측자료(GCVS 4th ed. )의 특성과 이들의 공간분포 및 증원소함량 분포를 조사하였다 이들의 공간분포에서 scale height 가 H = 0.6 kpc 인 원반(thick)형과 H = 2.2 kpc 인 헬로형의 두 성분으로 나타난다. 그리고 증원소함량의 은하중심거리와 은하정면거리에 따른 변화율은 각각 d[Fe/H]/dr = −0.013∼−0.020/kpc −0.013∼−0.020/kpc (r≤20kpc r≤20kpc ), d[Fe/H]/d|Z| = -0.034 /kpc (|Z|≤10kpc |Z|≤10kpc ) 이다. 이러한 공간분포와 증원소함량의 기울기 변화는 구상성단의 경우와 비슷하게 이증진화모형을 나타낸다. 그러나 증원소함랑의 빈도분포로 보아 field RR Lyrae 변광성이 모두 구상성단에서 기원되었다고 보기는 어렵다.