The Wasilewski Sample of Emission-Line Galaxies: Follow-up CCD Imaging and Spectroscopic and IRAS Observations
The Wasilewski Sample of Emission-Line Galaxies: Follow-up CCD Imaging and Spectroscopic and IRAS Observations
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Wasilewski 发射线星系样本：后续 CCD 成像、光谱和 IRAS 观测
DOI：
10.1086/191341
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发表时间：
1989
影响因子：
8.7
通讯作者：
C. Impey
中科院分区：
文献类型：
--
作者：
G. Bothun;M. Schmitz;J. Halpern;C. Lonsdale;C. Impey
提出了对 Wasilewski (1982) 的客观棱镜选择发射线星系 (ELG) 样本进行广泛成像和光谱跟踪的结果。 12、25、60 和 100 微米的通量也从共同的 IRAS 调查数据中获得。通过客观棱镜巡天发现的 ELG 通常较小且亮度较低，通常具有高于平均光学表面亮度的星系。客观棱镜巡天中的 Seyfert 探测率约为 10%，Seyfert 2 与 Seyfert 1 星系的空间密度之比明显大于 1。客观棱镜巡天选择的大多数星系都是恒星形成的晚期螺旋星系，通常表现出受干扰的形态。巡天探测到的星系中大约有 25% 是微弱的、高激发的贫金属致密 H II 区域。 62 参考文献
The results of an extensive imaging and spectroscopic follow-up of the objective prism-selected emission line galaxy (ELG) sample of Wasilewski (1982) are presented. Fluxes at 12, 25, 60, and 100 microns were also obtained from the coadded IRAS survey data. ELGs found by objective prism surveys are found to be generally small and underluminous galaxies which usually have higher than average optical surface brightness. The Seyfert detection rate in objective prism surveys is roughly 10 percent and the ratio of the space densities of Seyfert 2 to Seyfert 1 galaxies is significantly larger than unity. Most of the galaxies selected by objective prism surveys are star-forming, late-type spirals which often show disturbed morphology. About 25 percent of the galaxies detected by the surveys are faint, high-excitation metal-poor compact H II regions. 62 refs.