MULTI-WAVELENGTH EXTRAGALACTIC ASTRONOMY AND COSMOLOGY

我们计划在微波、亚毫米、远红外、近红外、光学和x射线波长上进行一系列星系外天体物理学和宇宙学的综合研究。我们将利用现有空间天文任务SPITZER， CHANDRA和GALEX的数据，将于2006年1月发射的日本ASTRO-F任务，将于2007年8月发射的欧空局HERSCHEL和PLANCK任务，以及主要的地面设施，如VLT， Gemini， UKIRT UKIDSS巡天，JCMT上的SCUBA和SCUBA2以及MAMBO。我们的科学目标包括在红外和x射线波长下研究宇宙的恒星形成历史，使用x射线光谱学研究黑洞附近的相对论效应，发现和理解非常明亮的尘埃红外星系，寻找引力透镜系统，非常高的红移类星体，以及高度模糊的活动星系核，提高我们对微波背景辐射的前景污染物的理解，以及利用该背景的极化来探测早期宇宙。通过结合不同波长的观测结果，我们将研究大质量黑洞的吸积与星系形成早期阶段之间的相互作用，尘埃在决定星系和类星体的x射线、紫外线、光学和红外发射之间的平衡中的作用，宇宙被电离时黑暗时代的结束，结构的起源是早期宇宙中非常小的波动它们在微波背景和星系分布上留下的印记。

We plan an integrated series of studies of extragalactic astrophysics and cosmology at microwave, submillimetre, far infrared, near infrared, optical and X-ray wavelengths. We will exploit the data from the current space astronomy missions SPITZER, CHANDRA and GALEX, the Japanese ASTRO-F mission due to be launched in January 2006, and the ESA missions HERSCHEL and PLANCK, due to be launched in August 2007, as well as major ground-based facilities such as the VLT, Gemini, the UKIRT UKIDSS survey, SCUBA and SCUBA2 on JCMT, and MAMBO. Our science goals include studying the star formation history of the universe at infrared and X-ray wavelengths, using X-ray spectroscopy to study relativistic effects in the vicinity of black holes, discovering and understanding very luminous dusty infrared galaxies, searching for gravitational lensed systems, very high redshift quasars, and heavily obscured active galactic nuclei, improving our understanding of foreground contaminants of the microwave background radiation as well as using the the polarization of that background to probe the early universe. By combining the result from surveys at different wavelengths we will study the interaction between accretion onto massive black holes and the early stages of galaxy formation, the role of dust in deciding the balance between X-ray, ultraviolet, optical and infrared emission from galaxies and quasars, the end of the dark ages when the universe becomes ionized, and the origin of structure in very small fluctuations in the early universe from the imprint they leave on the microwave background and in the galaxy distribution.