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翻訳と辞書　辞書検索 [ 開発暫定版 ] スポンサード リンク NGC 3114 ： ウィキペディア英語版 NGC 3114 NGC 3114 is a sparse open cluster which is projected onto the outskirts of the Carina complex.〔G. Carraro, F. Patat, "Star clusters in the Carina complex: UBVRI photometry of NGC 3114, Colliner 228 and vdB-Hage 99 *, A&A, Volume 379, Number 1, November 2001, pp. 136-146〕 Because of the high number of field stars from the disc of the Milky Way, it is very difficult object to study〔 as this contamination makes its size ambiguous. ==Studies of NGC 3114== NGC 3114 has first been subject of studies in 1963, when Jankowitz and McCosh obtained photographic UBV photometry for 171 of its stars and photoelectric UBV photometry of 52 stars. They estimated the cluster to be 910 parsecs from the Sun, its mean visual extinction $E(B-V)\; =\; 0.27$ and its age to range from $6\backslash times\; 10^$ and $2\backslash times\; 10^$ years.〔 In 1988, Schneider and Weiss obtained photometry data for 122 stars, revising the cluster reddening to be $E(B-V)\; =\; 0.03$.〔 Three years later, Sagar and Sharpless made the largest data recording of the cluster to date, obtaining BV CCD photometry of around 350 stars from seven 3.6'×5.4' regions. Because these regions were rather far from the cluster centre, a substantial contamination was expected. Nevertheless, by assuming the cluster reddening value obtained by Schneider and Weiss, they found the cluster to be $940\; \backslash pm\; 60$ pc, which agreed with the measurements taken 28 years previously by Jankowitz and McCosh. They also found the age of the cluster to be $1-2\; \backslash times\; 10^$ years.〔 Finally, in 1989 Claria' et al. estimated the cluster chemical abundance, finding that NGC 3114 has basically the same metal richness as the Sun, for which $()\; =\; -0.04\backslash pm0.04$〔 (Fe - Iron, H - Hydrogen). 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「NGC 3114」の詳細全文を読む スポンサード リンク 翻訳と辞書 : 翻訳のためのインターネットリソース Copyright(C) kotoba.ne.jp 1997-2016. All Rights Reserved.