Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses
Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 1011 solar masses
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DOI：
10.1038/nature09771
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发表时间：
2011-01
期刊：
影响因子：
64.8
通讯作者：
A. Amblard;A. Cooray;P. Serra;B. Altieri;V. Arumugam;H. Aussel;A. Blain;J. Bock;A. Boselli-
中科院分区：
文献类型：
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作者：
A. Amblard;A. Cooray;P. Serra;B. Altieri;V. Arumugam;H. Aussel;A. Blain;J. Bock;A. Boselli-
远红外波段的河外背景光，来自宇宙中光学上暗淡的、多尘的、正在形成恒星的星系，这些星系的恒星形成速度是每年几百个太阳质量。由于远红外望远镜的空间分辨率相对较差，对这些微弱的亚毫米星系进行单独研究具有挑战性。相反，它们的平均特性可以用统计数据来研究，比如背景强度变化的角功率谱。先前测量该功率谱的尝试结果表明，聚类幅度低于基于晕模型的简单ansatz计算的水平。在250、350和500 μm的亮度波动功率谱中，我们报告了弧分角尺度下线性预测的过度聚类。从这个过量，我们发现亚毫米星系位于质量最小的暗物质晕中，M min，使得log10 [M min/M⊙]= 350 μm，其中M⊙是太阳质量。这个最小的暗物质晕质量对应于宇宙中恒星形成的最有效的质量尺度，比星系形成的半解析模型预测的要低。
The extragalactic background light at far-infrared wavelengths,, comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year. These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes,. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations,,,. A previous attempt at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model. Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 μm. From this excess, we find that submillimetre galaxies are located in dark matter haloes with a minimum mass, M min, such that log10 [M min/M⊙]= at 350 μm, where M⊙ is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe, and is lower than that predicted by semi-analytical models for galaxy formation.