AMiBA: scaling relations between the integrated Compton-y and X-ray derived temperature, mass, and luminosity
Chih-Wei Locutus Huang, Jiun-Huei Proty Wu, Paul T. P. Ho, Patrick M. Koch, Yu-Wei Liao, Kai-Yang Lin, Guo-Chin Liu, Sandor M. Molnar, Hiroaki Nishioka, Keiichi… 展开作者
Chih-Wei Locutus Huang, Jiun-Huei Proty Wu, Paul T. P. Ho, Patrick M. Koch, Yu-Wei Liao, Kai-Yang Lin, Guo-Chin Liu, Sandor M. Molnar, Hiroaki Nishioka, Keiichi Umetsu, Fu-Cheng Wang, Pablo Altamirano, Mark Birkinshaw, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Chang, Ming-Tang Chen, Tzihong Chiueh, Chih-Chiang Han, Yau-De Huang, Yuh-Jing Hwang, Homin Jiang, Michael Kesteven, Derek Kubo, Chao-Te Li, Pierre Martin-Cocher, Peter Oshiro, Philippe Raffin, Tashun Wei, Warwick Wilson
We investigate the scaling relations between the X-ray and the thermal Sunyaev-Zel'dovich Effect (SZE) properties of clusters of galaxies, using data taken during 2007 by the Y.T. Lee Array for Microwave Background Anisotropy (AMiBA) at 94 GHz for the six clusters A1689, A1995, A2142, A2163, A2261, and A2390. The scaling relations relate the integrated Compton-y parameter Y_{2500} to the X-ray derived gas temperature T_{e}, total mass M_{2500}, and bolometric luminosity L_X within r_{2500}. Our results for the power-law index and normalization are both consistent with the self-similar model and other studies in the literature except for the Y_{2500}-L_X relation, for which a physical explanation is given though further investigation may be still needed. Our results not only provide confidence for the AMiBA project but also support our understanding of galaxy clusters.
AMiBA: Sunyaev-Zel'dovich effect derived properties and scaling relations of massive galaxy clusters
在86-102 GHz波段观测到6个大质量星系团的Sunyaev-Zel'dovich效应（SZE），红移为0.091 \leq z \leq 0.322。T. Lee Array for Microwave Background Anisotropy（AMiBA）微波背景各向异性天线阵本文改进了一种基于等温β模型的迭代方法，从AMiBA SZE数据中导出了电子温度T_e、总质量M_t、气体质量M_g和r_2500内的积分康普顿Y。本文还考虑了非等温通用温度剖面（UTP）β模型。这些结果与其它观测结果符合得很好。我们还研究了由于我们所采用的方法中所作的假设，这些纯SZ推导的T_e，M_t，M_g和Y之间的嵌入标度关系。我们的研究结果表明，集群属性可能是可测量的SZE观测。然而，建立在纯SZE方法的假设偏差的标度关系估计的结果，需要进一步研究。
Toward the Standard Population Synthesis Model of the X-Ray Background: Evolution of X-Ray Luminosity and Absorption Functions of Active Galactic Nuclei Including Compton-Thick Populations
The Cosmological Impact of Luminous TeV Blazars I: Implications of Plasma Instabilities for the Intergalactic Magnetic Field and Extragalactic Gamma-Ray Background
A Chandra observation of the ultraluminous infrared galaxy IRAS 19254--7245 (the Superantennae): X-ray emission from the Compton-thick AGN and the diffuse starburst
我们提出了一个IRAS 19254- 7245的{ \it Chandra}观测，它是一个邻近的ULIRG，也被称为{ \it the Superantennas}。高空间分辨率的{ \it钱德拉}使我们能够解开第一次从嵌入康普顿厚的活动星系核的弥漫星暴辐射。活动星系核的2-10 keV辐射谱符合平坦的幂律（$Γ=1.3$）和类He的Fe K $α$谱线，EW $\sim$ 1.5 keV，与以前的观测结果一致。Fe K $α$谱线轮廓可以被解析为中性6.4 keV谱线和电离6.7 keV（类He）或6.9 keV（类H）谱线的混合。与以前的{ \it XMM-Newton}和{ \it suzaku}观测相比，检测到了变化，证明了铁谱线发射的紧凑尺寸。我们拟合的光谱的星系尺度扩展发射不包括活动星系核和其他亮点源的软热分量与kT~0.8 keV。扩展辐射的亮度比活动星系核的亮度低一个数量级。扩展辐射的基本物理和结构性质与星暴驱动的星系风完全一致（不需要AGN的反馈）。在南核以南8 \arcsec处检测到候选超亮X射线源。如果发射是各向同性的，并且与超天线有关，那么这个离核点源的0.3-10 keV光度为~ $6\times 10^{40}$ erg s $^{-1}$。
Current and Future Constraints on Dark Matter from Prompt and Inverse-Compton Photon Emission in the Isotropic Diffuse Gamma-ray Background
我们进行了详细的检查，从提示和逆康普顿发射光子，包括模型相关和模型无关的边界的湮灭和衰变暗物质模型的电流约束。我们还表明，所观察到的各向同性弥散伽马射线背景（DGRB），这提供了一个最保守的约束模型的湮灭弱尺度暗物质粒子，可能会提高其灵敏度的一个因素~2至3（95% C. L.）。因为费米-LAT实验通过五年的观测解决了DGRB贡献的blazar源。对于我们的预测，我们采用的结果约束的光度依赖的密度演化加上blazar光谱能量分布序列模型，这是由DGRB和blazar源计数分布函数的约束。
