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Compter les galaxies infrarouges, raconter leur histoire : propriétés statistiques des galaxies infrarouges à grand redshift et origine du fond extragalactique infrarouge

机译:计算红外星系,并讲述它们的故事:具有大红移的红外星系的统计特性和红外河外背景的起源

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摘要

The extragalactic background light is the relic emission of the process of structure formation in the Universe. About half of this background, called cosmic infrared background, is emitted in the 8-1000 microns interval, peaks near 150 microns, and is essentially due to the star formation processes in the Universe. In fact, the infrared luminosity of a galaxy is linked to the hosted star formation. It is thus necessary to determine the evolution of infrared galaxies to well understand the origin of the cosmic infrared background.A rather simple statistical measurement, enabling to understand the origin of the cosmic infrared background, but also the evolution of the galaxies, consist in counting the sources as a function of their flux. I measured number counts of infrared galaxies using different methods in the data of the Spitzer and Herschel space telescopes, and of the BLAST experiment. The individually detected sources in the 24 microns Spitzer maps are responsible of the main part of the background. But, at larger wavelength, the sensitivity and the angular resolution of the instruments decreases, and the detected sources explain only a small part of the background. The stacking analysis enable to measure the mean far-infrared or sub-millimeter flux of a population detected only in the mid-infrared. This technique provides stringent lower limits on the level of the background, but also enables to count the sources which are too faint to be detected individually. These results are confirmed by the P(D) analysis, which determines the counts from the histogram of the infrared maps.These new measurements constrain the evolution of the infrared galaxies. I built a parametric evolution model to interpret the source counts. This model well reproduces the statistical properties of the infrared galaxies between 15 and 1100 microns. It predicts that the star formation in the young Universe (z>2) mainly happen in ultra-luminous infrared galaxies (LIR> 10^12 Lsun). These galaxies formed stars very quickly (more than 100 Msun/years), and have few equivalents in the local Universe. Nowadays, the star formation rate has decreased by a factor of ten, and the star formation mainly happen in galaxies like ours. This model has been used to interpret the fluctuations of the cosmic infrared background at large wavelength observed by BLAST, Planck, and Herschel.
机译:星系外背景光是宇宙结构形成过程的遗迹。这种背景的大约一半(称为宇宙红外背景)以8-1000微米的间隔发射,在150微米附近达到峰值,这主要归因于宇宙中的恒星形成过程。实际上,星系的红外光度与主恒星的形成有关。因此,有必要确定红外星系的演化,以充分了解宇宙红外背景的起源。相当简单的统计测量,不仅可以了解宇宙红外背景的起源,而且还可以了解星系的演化,包括进行计数源是其通量的函数。我在Spitzer和Herschel太空望远镜的数据以及BLAST实验的数据中使用不同的方法测量了红外星系的数量。在24微米的Spitzer图中单独检测到的辐射源是背景的主要部分。但是,在较大波长下,仪器的灵敏度和角分辨率降低,并且所检测到的源仅能解释背景的一小部分。堆叠分析可以测量仅在中红外中检测到的种群的平均远红外或亚毫米通量。此技术提供了严格的背景水平下限,但也可以对太微弱以致无法单独检测的光源进行计数。这些结果通过P(D)分析得到了证实,该分析从红外图的直方图确定了计数。这些新的测量结果限制了红外星系的演化。我建立了一个参数演化模型来解释源计数。该模型很好地再现了15到1100微米之间的红外星系的统计特性。它预言年轻宇宙(z> 2)中的恒星形成主要发生在超发光红外星系(LIR> 10 ^ 12Lsun)中。这些星系很快就形成了恒星(超过100 Msun /年),而在当地的宇宙中却很少。如今,恒星形成率下降了十倍,恒星形成主要发生在像我们这样的星系中。该模型已用于解释BLAST,Planck和Herschel观测到的大波长宇宙红外背景的波动。

著录项

  • 作者

    Bethermin Matthieu;

  • 作者单位
  • 年度 2011
  • 总页数
  • 原文格式 PDF
  • 正文语种 fr
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