본 연구는 동아시아 영역에 속해있는 5개 SKYNET 관측소(서울, 지바, 엣추 지마, 후쿠에 지마, 헤도 미사키)에서 6년 간 관측한 AOT 자료를 활용하여 MODIS에서 산출된 AOT를 검증하였고, 아울러 에어로솔 기후장 분석도 함께 수행하였다. 검증연구를 위해 관측소 25 km 이내의 MODIS AOT를 평균하였고, MODIS 관측시각 30분 전후 SKYNET AOT를 평균하여 시공간 일치 자료를 생산하였다. 시공간 일치 자료의 비교 결과 MODIS AOT의 정확도는 에어로솔 종류에 크게 영향을 받지 않았으나, MODIS AOT 산출과정 중 거대 입자 모형의 사용비율이 높아질수록 SKYNET AOT에 비해서 비교적 큰 값을 산출하는 경향을 보였다. 또한 AOT가 낮은 대기에서 MODIS AOT는 과대 추정하는 경향을 보였고 그 경향성은 AOT가 높아질수록 줄어들었다. MODIS-SKYNET AOT간의 회귀분석 결과 기울기는 0.86, Y절편은 0.16으로 나타났고 결정계수(R2)는 0.61로 나타났다. 이러한 통계적 결과로 미루어 볼 때 동아시아 영역에서 산출된 MODIS AOT는 지상 관측에 견줄 만큼 정확하다고 볼 수 있다.

We carried out high-resolution(FWHM=3' .3) HI 21 cm observations of the supernova remnant(SNR) PKS0607+17 and HII region S261 using Arecibo 305-m telescope. The observation was to investigate whether the high-velocity(HV) gas detected in the southern area of PKS0607+17 by Koo & Heiles(1991) is physically associated with the SNR or not. The velocity of the HV gas ranges from +64 km/s to +87 km/s, which is difficult to result from the Galactic rotation. The HV gas could be the gas accelerated by supernova blast wave. However, because the observation of Koo and Heiles(1991) was carried out using Hat Creek radio telescope(FWHM ≃ ≃ 36'), the association of the HV gas with the SNR could not be investigated. Using the Arecibo HI 21cm data, we have found that the HV gas appears m the southern part of the SNR and its velocity ranges from +61 km/s to +77 km/s. But the HV gas is scattered m the whole field, not only toward PKS0607+17 but also outside the SNR Accordingly the HV gas is probably not associated with the SNR, but is accidentally aligned along the same line of sight toward the SNR. Instead we have found that HI clouds at low velocities could be possibly associated with the SNR. In Arecibo HI 21cm channel maps the HI gas seems to surround the southern boundary of the SNR at VLSR VLSR = +19.6 ~ +40.2 km/s. But because the region of the Arecibo HI 21cm observation is not wide enough to examine the HI gas distribution, we investigated this area using the Berkely low-latitude HI survey data(Weaver & Williams 1974) too. There we found HI gas surrounding the radio continuum boundary of PKS0607+17 at VLSR VLSR = +21.6 ~ +258 km/s. It is possible that this HI gas is associated with the SNR, in which case, the velocity of the SNR Vo Vo ≃ ≃ +26 km/s, its distance d ≃ ≃ 12.5 kpc and its radius R ≃ ≃ 145 pc. If we assume that the expansion velocity is ~10 km/s, then the age of the SNR is ∼4.4×106 ∼4.4×106 years. PKS0607+17 could be one of the oldest SNRs in the Galaxy. We also studied HI propertities of the HII region S261, which is ∼1∘ ∼1∘ away from PKS0607+17. There has been no high-resolution m 21 cm observational study on S261. We discovered HI cloud located at the north-eastern part of S261 at VLSR VLSR = +5 km/s ~ +10 km/s, which is possibly associated with the HII region. The central velocity of the HI cloud VLSR VLSR = +7.2 km/s and the corresponding distance d = 1.5 kpc. This velocity is comparable to the radio recombination line velocities.