DETECTION OF THE COSMIC FAR-INFRARED BACKGROUND IN AKARI DEEP FIELD SOUTH
DETECTION OF THE COSMIC FAR-INFRARED BACKGROUND IN AKARI DEEP FIELD SOUTH
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DOI：
10.1088/0004-637x/737/1/2
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发表时间：
2010-02
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通讯作者：
Shuji Matsuura;M. Shirahata;M. Kawada;T. T. Takeuchi-T.;D. Burgarella;D. Clements;W. Jeong;H. Hanami;Sophia A. Khan;H. Matsuhara;Takao Nakagawa;S. Oyabu;C. Pearson;A. Pollo;S. Serjeant;T. Takagi;G. J. White;G. J. White
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作者：
Shuji Matsuura;M. Shirahata;M. Kawada;T. T. Takeuchi-T.;D. Burgarella;D. Clements;W. Jeong;H. Hanami;Sophia A. Khan;H. Matsuhara;Takao Nakagawa;S. Oyabu;C. Pearson;A. Pollo;S. Serjeant;T. Takagi;G. J. White;G. J. White
我们报告的绝对亮度和空间波动的宇宙红外背景（CIB）通过AKARI卫星的新的限制。我们在AKARI Deep Field South进行了65，90，140和160 μm的观测，作为宇宙学调查，这是天空中最低的卷云区域之一。在去除明亮的星系并从测量的天空亮度中减去黄道和银河前景后，我们成功地测量了CIB亮度及其在从角分到度的广泛角度尺度上的波动。测量的CIB亮度与先前报道的COBE数据结果一致，但明显高于通过Spitzer从选定的24 μm源的堆叠分析中获得的70和160 μm的下限。与斯皮策观测结果的差异可能是由于一个新的星系群在高红移时被热尘埃或未知的漫射辐射所掩盖。从90 μm的功率谱分析中，确定了两个分量：CIB波动与散粒噪声，由于个别星系在一个小的角尺度从光束大小到10弧分，和银河卷云发射占主导地位的最大角尺度的几度。在90 μm处的功率谱的整体形状与斯皮策和卫星上的大口径亚毫米望远镜（BLAST）观测到的更长波长处的功率谱非常相似。我们的功率谱，与10-30弧分的中间角尺度，给出了一个坚定的上限星系集群，这是发现斯皮策和BLAST。此外，CIB波动的颜色，这是通过结合我们的数据和以前的结果，是红色的超亮红外星系在高红移。这些星系不太可能提供大部分90 μm的CIB辐射，但对波动负有责任。我们的研究结果提供了新的约束远红外星系的演化和聚类特性和任何扩散发射从早期宇宙。
We report new limits on the absolute brightness and spatial fluctuations of the cosmic infrared background (CIB) via the AKARI satellite. We carried out observations at 65, 90, 140, and 160 μm as a cosmological survey in AKARI Deep Field South, which is one of the lowest cirrus regions with a contiguous area of the sky. After removing bright galaxies and subtracting zodiacal and Galactic foregrounds from the measured sky brightness, we successfully measured the CIB brightness and its fluctuations across a wide range of angular scales, from arcminutes to degrees. The measured CIB brightness is consistent with previous results reported from COBE data, but significantly higher than the lower limits at 70 and 160 μm obtained via Spitzer from the stacking analysis of selected 24 μm sources. The discrepancy with the Spitzer result is possibly due to a new galaxy population at high redshift obscured by hot dust or unknown diffuse emission. From a power spectrum analysis at 90 μm, two components were identified: the CIB fluctuations with shot noise due to individual galaxies in a small angular scale from the beam size up to 10 arcminutes, and Galactic cirrus emission dominating at the largest angular scales of a few degrees. The overall shape of the power spectrum at 90 μm is very similar to that at longer wavelengths, as observed by Spitzer and the Balloon-borne Large-Aperture Submillimeter Telescope (BLAST). Our power spectrum, with an intermediate angular scale of 10–30 arcminutes, gives a firm upper limit for galaxy clustering, which was found by Spitzer and BLAST. Moreover, the color of the CIB fluctuations, which is obtained by combining our data with the previous results, is as red as ultra-luminous infrared galaxies at high redshift. These galaxies are not likely to provide the majority of the CIB emission at 90 μm, but are responsible for the fluctuations. Our results provide new constraints on the evolution and clustering properties of distant infrared galaxies and any diffuse emission from the early universe.