论文标题
宇宙红外背景的逆孔子散射
Inverse-Compton Scattering of the Cosmic Infrared Background
论文作者
论文摘要
Thermal Sunyaev-Zel'Dovich（TSZ）效应是通过CMB光子的反compton散射在宇宙微波背景（CMB）频谱中产生的失真，主要位于自由，能量电子电子，主要位于内部内部培养基（ICM）中。预计在星系星系中，来自热灰尘发射的宇宙红外背景（CIB）光子预计将经历相同的过程。在这项工作中，我们对CIB中产生的TSZ样失真进行了第一个计算。为了关注CIB单极，我们使用Halo模型方法来计算产生失真的CIB信号和Compton-y $ y $场。我们自言自语地说明了CIB和Compton- $ y $字段的红移共同进化：它们（部分）由相同的暗物质Halos来源，与CMB案例相比，这引入了计算的新方面。我们发现，在2260 GHz（940 GHz）上，对CIB单极光谱的逆变形对CIB单极光谱的峰值幅度为$ \ 4 $ JY/sr（$ \约-5 $ jy/sr）。与通常的TSZ效应相反，对CIB频谱的失真为两个无效频率，约为196 GHz和1490 GHz。我们执行Fisher矩阵计算，以预测未来实验的新变形信号的可检测性。 $ \ textIt {pixie} $具有足够的仪器灵敏度，可以以$4σ$检测信号，但是前景污染可将投影信号到噪声降低$ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ \ hightiage的$ \约70美元。即使在前景上边缘化后，即使在$ \5σ$中，未来的ESA航行2050光谱仪也可能在$ \5σ$中检测到CIB失真。该信号的测量将提供有关宇宙恒星形成历史的新信息，并且可以通过近距离地面实验来访问失真各向异性。
The thermal Sunyaev-Zel'dovich (tSZ) effect is the distortion generated in the cosmic microwave background (CMB) spectrum by the inverse-Compton scattering of CMB photons off free, energetic electrons, primarily located in the intracluster medium (ICM). Cosmic infrared background (CIB) photons from thermal dust emission in star-forming galaxies are expected to undergo the same process. In this work, we perform the first calculation of the resulting tSZ-like distortion in the CIB. Focusing on the CIB monopole, we use a halo model approach to calculate both the CIB signal and the Compton-$y$ field that generates the distortion. We self-consistently account for the redshift co-evolution of the CIB and Compton-$y$ fields: they are (partially) sourced by the same dark matter halos, which introduces new aspects to the calculation as compared to the CMB case. We find that the inverse-Compton distortion to the CIB monopole spectrum has a positive (negative) peak amplitude of $\approx 4$ Jy/sr ($\approx -5$ Jy/sr) at 2260 GHz (940 GHz). In contrast to the usual tSZ effect, the distortion to the CIB spectrum has two null frequencies, at approximately 196 GHz and 1490 GHz. We perform a Fisher matrix calculation to forecast the detectability of this new distortion signal by future experiments. $\textit{PIXIE}$ would have sufficient instrumental sensitivity to detect the signal at $4σ$, but foreground contamination reduces the projected signal-to-noise by a factor of $\approx 70$. A future ESA Voyage 2050 spectrometer could detect the CIB distortion at $\approx 5σ$ significance, even after marginalizing over foregrounds. A measurement of this signal would provide new information on the star formation history of the Universe, and the distortion anisotropies may be accessible by near-future ground-based experiments.
