摘要
By adopting a recently developed semi empirical methodology for removing the atmospheric diffuse light and an improved technique of individual star subtraction, we have newly reduced the distribution of the visible zodiacal light (ZL) brightness from almucantar scan observations of the night sky brightness at Mt. Haleakala, Hawaii. The resulting two dimensional map of the ZL brightness covers the sky over 40°≤λ-λ ⊙≤320° and -40°≤β≤40° and its angular resolution 2°×2°is fine enough to reveal optical counterparts of the structures in the zodiacal emission first found from the IRAS space observations.
By adopting a recently developed semi empirical methodology for removing the atmospheric diffuse light and an improved technique of individual star subtraction, we have newly reduced the distribution of the visible zodiacal light (ZL) brightness from almucantar scan observations of the night sky brightness at Mt. Haleakala, Hawaii. The resulting two dimensional map of the ZL brightness covers the sky over 40°≤λ-λ ⊙≤320° and -40°≤β≤40° and its angular resolution 2°×2°is fine enough to reveal optical counterparts of the structures in the zodiacal emission first found from the IRAS space observations.
作者
S.M.Kwon 1, S.S.Hong 2, J.L.Weinberg 3 1 ( Dept. of Science Education, Kangwon Nat. Univ., Chunchon 200 701,KOREA ) 2 ( Department of Astronomy, Seoul Nat. Univ., Seoul 151 742,KOREA ) 3 ( Technology Care Givers, Snellville,G A 30039,U.S.A. )
出处
《天文研究与技术》
CSCD
1999年第S1期269-273,共5页
Astronomical Research & Technology
