Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation
Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation
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DOI：
10.1051/0004-6361/201322093
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发表时间：
2013-09
影响因子：
6.5
通讯作者：
P. Ade;N. Aghanim;C. Armitage-Caplan;M. Arnaud;M. Ashdown;F. Atrio-Barandela;J. Aumont;C. Baccigalu
中科院分区：
文献类型：
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作者：
P. Ade;N. Aghanim;C. Armitage-Caplan;M. Arnaud;M. Ashdown;F. Atrio-Barandela;J. Aumont;C. Baccigalu
我们提出了新的测量宇宙红外背景（CIB）各向异性使用普朗克。结合HFI数据和IRAS，测量了143 - 3000 GHz的角自频和互频功率谱，以及217 - 545 GHz的自双谱。用于计算CIB功率谱和双谱的总面积分别约为2240和4400度2。在仔细去除污染物（宇宙微波背景各向异性，银河尘埃和Sunyaev-Zeldovich发射），并对系统学进行完整的研究后，CIB功率谱以前所未有的信噪比从角多极子到150到2500进行测量。由于尘埃，恒星形成星系的聚集而产生的双谱测量范围为130到1100，在217，353和545 GHz处的总信噪比分别为6，19和29。两种方法被开发用于建模CIB功率谱各向异性。第一种方法利用了普朗克在大角度尺度上的独特测量，并且仅对功率谱的线性部分进行建模，其中暗物质晕在给定的红移下托管尘埃星系的平均偏差由它们对发射率的贡献加权。第二种方法是基于一个模型，该模型将恒星形成星系与暗物质晕及其亚晕相关联，使用尘埃处理的红外光度和（亚）晕质量之间的参数化关系。这两种方法同时适合所有的自动和交叉功率谱非常好。我们发现，星星的形成历史是很好的约束，红移约2，并同意最近的估计模糊恒星形成密度使用斯皮策和赫歇尔。然而，在较高的红移，星星形成历史测量的准确性是强烈退化的光谱能量分布的CIB星系的不确定性。我们还发现，最有效的主持星星形成的平均晕质量是log（Meff/M�）= 12。6和CIB星系有温暖的温度随着红移的增加。CIB双谱比功率谱预期的要陡，尽管很好地符合幂律;这给出了一些关于大质量晕对CIB双谱的贡献的信息。最后，我们证明了相同的晕占据分布可以同时拟合所有的功率谱。普朗克的精确测量为CIB各向异性的建模提出了新的挑战，表明了使用CIB各向异性来理解星系形成过程的力量。
We present new measurements of cosmic infrared background (CIB) anisotropies using Planck. Combining HFI data with IRAS, the angular auto- and cross-frequency power spectrum is measured from 143 to 3000 GHz, and the auto-bispectrum from 217 to 545 GHz. The total areas used to compute the CIB power spectrum and bispectrum are about 2240 and 4400 deg 2 , respectively. After careful removal of the contaminants (cosmic microwave background anisotropies, Galactic dust, and Sunyaev-Zeldovich emission), and a complete study of systematics, the CIB power spectrum is measured with unprecedented signal to noise ratio from angular multipoles � ∼ 150 to 2500. The bispectrum due to the clustering of dusty, star-forming galaxies is measured from � ∼ 130 to 1100, with a total signal to noise ratio of around 6, 19, and 29 at 217, 353, and 545 GHz, respectively. Two approaches are developed for modelling CIB power spectrum anisotropies. The first approach takes advantage of the unique measurements by Planck at large angular scales, and models only the linear part of the power spectrum, with a mean bias of dark matter haloes hosting dusty galaxies at a given redshift weighted by their contribution to the emissivities. The second approach is based on a model that associates star-forming galaxies with dark matter haloes and their subhaloes, using a parametrized relation between the dust-processed infrared luminosity and (sub-)halo mass. The two approaches simultaneously fit all auto- and cross-power spectra very well. We find that the star formation history is well constrained up to redshifts around 2, and agrees with recent estimates of the obscured star-formation density using Spitzer and Herschel. However, at higher redshift, the accuracy of the star formation history measurement is strongly degraded by the uncertainty in the spectral energy distribution of CIB galaxies. We also find that the mean halo mass which is most efficient at hosting star formation is log (Meff/M� ) = 12. 6a nd that CIB galaxies have warmer temperatures as redshift increases. The CIB bispectrum is steeper than that expected from the power spectrum, although well fitted by a power law; this gives some information about the contribution of massive haloes to the CIB bispectrum. Finally, we show that the same halo occupation distribution can fit all power spectra simultaneously. The precise measurements enabled by Planck pose new challenges for the modelling of CIB anisotropies, indicating the power of using CIB anisotropies to understand the process of galaxy formation.