蜻蜓望远天线阵的发展及其科学应用
The Development and Scientific Application of the Dragonfly Telephoto Array
摘要：
低表面亮度的可见光波长低于29等角秒的宇宙$^{-2}$充满了未被探索的天体物理现象。由于天空相减的系统误差以及大气和望远镜中的散射光，比这个表面亮度更暗的结构极难成像。在第1章中，我将展示蜻蜓长焦阵列（简称蜻蜓）如何通过硬件和软件的组合来解决这些系统学问题，并能够在30 mag arcsec $^{-2}$或更暗的水平上成像。在第2章中，我将介绍Dragonfly Pipeline以及它如何针对低表面亮度成像进行优化，如何自动拒绝有问题的曝光，以及它的云编排。在第3章中，我提出了一个研究的外盘附近的螺旋星系NGC 2841使用蜻蜓以及档案数据在紫外线从星系演化探测器卫星和休息帧21厘米数据使用甚大阵。虽然人们普遍认为气体在星系外盘中占主导地位，但我发现在NGC 2841中，情况并非如此。恒星盘延伸到R25的5倍，在所有半径上，恒星质量都比气体质量多。令人惊讶的是，在30千秒差距以上，恒星与气体质量的比例是恒定的，在那里，圆盘也是弯曲的。我建议最有可能的形成机制，这个外盘是共面卫星吸积。在第四章中，我提出了一个研究的热发射和散射光的尘埃在蜘蛛HI云的光学薄的区域，使用蜻蜓和赫歇尔空间天文台的数据。在结束论文（第5章）时，我期待着蜻蜓管道（Dragonfly Pipeline）的进一步改进，这是一项星系盘形成机制的人口研究，并进行尘埃模型的测试。
英文摘要：
The low surface brightness visible wavelength Universe below 29 mag arcsec$^{-2}$ is teeming with unexplored astrophysical phenomena. Structures fainter than this surface brightness are extremely difficult to image due to systematic errors of sky subtraction and scattered light in the atmosphere and in the telescope. In Chapter 1, I show how The Dragonfly Telephoto Array (Dragonfly for short) addresses these systematics via a combination of hardware and software and is able to image at a level of 30 mag arcsec$^{-2}$ or fainter. In Chapter 2, I describe the Dragonfly Pipeline and how it is optimized for low surface brightness imaging, how it automatically rejects problematic exposures, and its cloud-orchestration. In Chapter 3, I present a study of the outer disk of the nearby spiral galaxy NGC 2841 using Dragonfly as well as archival data in UV from the Galaxy Evolution Explorer Satellite and rest frame 21 cm data using the Very Large Array. While it is commonly accepted that gas dominates over stars in galaxy outer disks, I find that in NGC 2841, this is not the case. The stellar disk extends to five times R25, and there is more stellar than gas mass at all radii. Surprisingly there is a constant ratio of stellar to gas mass beyond 30 kpc, where the disk is also warped. I propose the most likely formation mechanism for this outer disk is co-planar satellite accretion. In Chapter 4, I present a study of thermally emitted and scattered light from dust in the optically thin regions of the Spider HI Cloud, using Dragonfly and Herschel Space Observatory data. In closing the thesis (Chapter 5), I look forward to further improvements in the Dragonfly Pipeline, a population study of the formation mechanisms of galaxy disks and to carrying out tests of dust models.
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