An 870um Heterodyne Array Receiver for the Arizona/MIPfR Submillimeter Telescope

摘要美国亚利桑那大学计划为美国亚利桑那大学/马克斯·普朗克射电天文研究所（MPIfR） 10米海因里希·赫兹望远镜（HHT）建造一个11元SIS外差阵列接收机。该阵列将被设计用于870 pm的大气窗口，其调谐范围从315到380 Ghz，是亚毫米频谱部分最丰富的区域之一。在任何亚毫米波段中，870 pm窗口的大气透射率也是最高的。为这个波长范围设计的阵列将充分利用望远镜和可用的大气传输，并为现在和过去时代的恒星、化学和星系演化提供新的视角。阵列接收器将在一个高效、紧凑的光学系统中使用SIS波导接收器。该阵列被分成两个独立调谐的、正交极化的六边形填充子阵列。子阵列是物理排列的，当它们的波束组合在一个金属网格上时，在天空中看起来是交错的。该阵列的视场是76“x 88”。相邻像素之间的距离最多为~ 19”。阵列接收机的调谐和控制将完全自动化。资金将用于构建阵列接收器“前端”，包括光学器件、混频器、低温恒温器、局部振荡器和冷却I.F.放大器。每个阵列信道将具有500 MHz （435 km/s）到2 GHz （1740 km/s）的可用带宽。相应的光谱分辨率分别为0.053和0.85 km/s。如此大范围的瞬时带宽和光谱分辨率将使该阵列成为一个出色的探测器，可以探测从冷云到边缘的高红移星系等各种天文物体的速度场。

AST 9622569 ABSTRACT The University of Arizona proposes to build an 11- element, SIS heterodyne array receiver for use on the 10 meter University of Arizona/Max Planck Institute for Radioastronomy (MPIfR) Heinrich Hertz Telescope (HHT). The array will be designed for operation in the 870 pm atmospheric window, with a tuning range from 315 to 380 Ghz, one of the richest regions in the submillimeter portion of the spectrum. The 870 pm window also has the highest atmospheric transmission of any submillimeter band. An array designed for this wavelength range will make excellent use of the telescope, the available atmospheric transmission, and provide a new perspective on stellar, chemical, and galaxy evolution in the present as well as past epochs. The array receiver will use SIS waveguide receivers in an efficient, compact optical system. The array is divided into two, independently tuned, hexagonally packed subarrays with orthogonal polarizations. The subarrays are physically arranged so that their beams, when combined on a wire grid, appear interleaved on the sky. The field-of-view of the array is 76" x 88". The separation between adjacent pixels is at most ~ 19". The tuning and control of the array receiver will be completely automated. Funding will be used to build the array receiver "front-end", which includes the optics, mixers, cryostat, local oscillators, and cooled I.F. amplifiers. Each array channel will have from 500 MHz (435 km/s) to 2 GHz (1740 km/s) of available bandwidth. The corresponding spectral resolutions are 0.053 and 0.85 km/s respectively. Such a large range in instantaneous bandwidth and spectral resolution will make the array an excellent probe of velocity fields in a wide range of astronomical objects, from cold clouds to edge-on, high-redshift galaxies.