Studies of Faint Radio Galaxies

将对过去五年收集的一套独特的高质量深度调查数据进行系统分析。使用甚大阵列(VLA)和韦斯特博克射电望远镜在银河系高纬度的几个选定地区进行了深入调查。通过使用英国红外望远镜(UKIRT)红外望远镜设施(IRTF)、Palomar和多镜望远镜(MMT)进行的电荷耦合器件(CCD)测光和成像，对这些调查进行了跟踪。将完成光学数据的简化和对这些数据的彻底分析。该项目的目标是：1)根据深部CCD图像上的形态、多色测光和可用的光谱，明确地确定微弱射电星系的性质。2)对构成射电源群体高红移尾部的非常微弱、低表面亮度的射电星系进行系统研究。射电星系的红移已经在z大于1和小于3的范围内被测量到。其中一些是正在形成的(椭圆)星系的很好的候选者。由于这些天体是非常弱的射电源，它们提供了一个独特的机会来研究近正常星系的形成，它们的低水平活动核，以及这些近正常星系中可能的相互关系。3)系统地比较了光学-红外数据与星系光谱演化的详细模型。这将为星系可能的演化模型、其形成时期的范围以及哈勃常数(HO)的值提供重要的约束。这些模型将包括尘埃、银河系风和红色的GB、AGB和碳星。

A systematic analysis of a unique set of high quality deep survey data that has been collected during the last five years will be carried out. Deep surveys were carried out in several Selected Areas at high galactic latitude with the Very Large Array (VLA) and Westerbork radio telescopes. The surveys were followed up through charge-coupled device (CCD) photometry and imaging with the United Kingdom Infrared Telescope (UKIRT) Infrared Telescope Facility (IRTF), Palomar and the Multiple Mirror Telescope (MMT). The optical data reduction and a thorough analysis of these data will be completed. The following items are the project goals: 1) Establish the nature of faint radio galaxies unambiguously from their morphology on the deep CCD images, the multicolor photometry and the available spectroscopy. 2) A systematic study of the very faint, low surface brightness radio galaxies that constitute the high redshift tail of the radio source population. Radio galaxy redshifts have been measured in the range of z greater than 1 and less than 3. Some of these are good candidate for (elliptical) galaxies in the process of formation. Since these objects are very weak radio sources, they offer a unique opportunity to study the formation of nearly normal galaxies, of their low level active nuclei, and possible mutual relationship in these nearly normal galaxies. 3) A systematic comparison of the optical-infrared data with detailed models for the spectral evolution of galaxies. This will provide important constraints to possible evolutionary models for galaxies, the range in their formation epoch, and the value of the Hubble constant (Ho). These models will incorporate the roll of dust, galactic winds, and red GB, AGB, and Carbon stars.