在3个DIRBE暗点中使用Spitzer探测3.6微米CIRB
Probing the 3.6 Micron CIRB with Spitzer in 3 DIRBE Dark Spots
摘要：
我们用斯皮策望远镜观测了三个天区，用从黄道光减DIRBE图中减去2 MASS恒星通量的方法确定了3.5微米的宇宙红背景（CIRB）。对于这些区域中的每一个，我们已经获得了270秒的积分时间每像素与IRAC斯皮策在中心平方度。我们目前的星系计数在这些大约1平方度的IRAC调查。随着扩展的格罗斯带和北GOODS的深星系计数，我们能够比较银河系对CIRB的贡献与“DIRBE减去2 MASS”确定的L波段CIRB。使用轮廓拟合测光包GIM 2D，我们发现一个更大的流量贡献的CIRB比确定使用孔径测光。我们还作出了第一次严格的分析，在确定的不确定性，通过星系计数斯皮策图像使用蒙特卡洛马尔可夫链模拟我们的数据分析。用一个简单的破幂律模型计算星系数与星等的函数，我们发现3.6微米处星系对CIRB的贡献最大，为10.8^{+2.1}-1.1} kJy/sr.然而，即使用这个限制模型，我们发现星系数并不能从上面强烈地限制CIRB.我们能够找到解决方案，其中CIRB运行到大强度，而不需要额外的漫射源。
英文摘要：
We observed three regions of the sky with Spitzer in which the Cosmic InfraRed Background (CIRB) has been determined at 3.5 microns using the method of subtracting 2MASS stellar fluxes from zodiacal light subtracted DIRBE maps. For each of these regions we have obtained 270 seconds of integration time per pixel with IRAC on Spitzer over the central square degree. We present galaxy counts in each of these approximately 1 square degree IRAC surveys. Along with deep galaxy counts in the Extended Groth Strip and GOODS North, we are able to compare the galactic contribution to the CIRB with the "DIRBE minus 2MASS'' determined L-band CIRB. Using the profile-fit photometry package GIM2D, we find a substantially larger flux contribution to the CIRB than that determined using aperture photometry. We have also made the first rigorous analysis of the uncertainties in determining the CIRB via galaxy counts in Spitzer images using a Monte Carlo Markov Chain simulation of our data analysis. Using a simple broken power law model for galaxy counts as a function of magnitude we find a most probable contribution to the CIRB from galaxies at 3.6 microns of 10.8^{+2.1}_{-1.1} kJy/sr. Even with this restricted model, however, we find that galaxy counting does not strongly constrain the CIRB from above. We are able to find solutions in which the CIRB runs away to large intensities without the need for an additional diffuse source.
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