原恒星中的复杂有机分子与ALMA光谱巡天（COMPASS）：I. ALMA大型项目概述
Complex Organic Molecules in Protostars with ALMA Spectral Surveys (COMPASS): I. Overview of the ALMA Large Program
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中文总结 AI 辅助
本文概述了ALMA大型项目COMPASS，通过高分辨率无偏光谱巡天11个原恒星源，旨在表征复杂有机分子库存，初步定性比较显示源间化学差异小于一个数量级。
中文摘要 AI 辅助
在恒星形成早期阶段形成的复杂有机分子的库存特征描述，仍然是天体化学中的一个基本研究问题，这可能影响原行星盘乃至潜在行星的最终化学成分。阿塔卡马大型毫米/亚毫米波阵列（ALMA）提供了角分辨率和灵敏度，能够聚焦于嵌入的太阳型原恒星周围的热（T > 100 K）气体，并高精度地绘制其分子库存。ALMA大型项目“原恒星中的复杂有机分子与ALMA光谱巡天”（COMPASS）旨在提供一系列原恒星源的分子内容综合库存，以理解其环境和演化阶段的化学影响。COMPASS是一项无偏光谱巡天，覆盖11个富含谱线的Class 0和I原恒星源，光谱范围为279.0至311.7 GHz，角分辨率为0.15-0.5角秒，对应于目标源周围约100天文单位（半径）的内部区域。本文提供了COMPASS项目的概述，以及观测设置和目标源选择所采用的策略。我们还对选定分子的空间分布和选定复杂有机物的谱线通量相对强度进行了定性比较。定性比较表明，源之间可能存在化学差异，例如在含氧和含氮物种群的丰度之间，但这种变化发生在小于一个数量级的水平。在这些水平上的丰度定量比较需要巡天的大带宽，以及对巡天中每个源检测到的数千条谱线的激发和强度进行仔细分析，这将在后续论文中探讨。
英文摘要
It remains a fundamental research question in astrochemistry to characterize the inventory of complex organic molecules formed during the early stages of star formation, which may affect the eventual chemical composition of protoplanetary disks and potentially planets. The Atacama Large Millimeter/submillimeter Array (ALMA) provides the angular resolution and sensitivity to zoom in on the hot (T > 100 K) gas surrounding embedded solar-type protostars and chart their molecular inventories with high accuracy. The ALMA Large Program Complex Organic Molecules in Protostars with ALMA Spectral Surveys (COMPASS) aims to provide comprehensive inventories of the molecular content of a sample of protostellar sources to understand the chemical impact of their environments and evolutionary stages. COMPASS is an unbiased spectral survey of 11 line-rich Class 0 and I protostellar sources in the spectral range from 279.0 to 311.7 GHz at 0.15-0.5" angular resolution with ALMA, corresponding to the inner ~100 au (radius) around the targeted sources. This paper provides an overview of the COMPASS program and the adopted strategy in terms of observational setups and targeted sources. We also present a qualitative comparison of the spatial distributions of selected molecules and the relative strengths of the line fluxes of selected complex organics. The qualitative comparisons suggest that chemical differences between sources may be present, for example, between the abundances of groups of oxygen- and nitrogen-bearing species, but also that such variations occur at levels smaller than an order of magnitude. Quantitative comparisons of abundances at these levels require the large bandwidth of the survey, as well as a careful analysis of the excitation and strengths of the several thousands of lines detected toward each source in the survey, as will be explored in forthcoming papers.
发表机构
- Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse（图卢兹大学天体物理与行星学研究所以）
- Physikalisch-Meteorologisches Observatorium Davos und Weltstrahlungszentrum (PMOD/WRC)（达沃斯物理气象观测站和世界辐射中心）
- Department of Chemistry, Biochemistry and Pharmaceutical Sciences (DCBP), Universität Bern（伯尔尼大学化学、生物化学和药学系）
- Department of Physics and Astronomy, Seoul National University（首尔大学物理与天文学系）
- National Radio Astronomy Observatory（美国国家射电天文台）
- Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学）
- Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）
- Institute of Astronomy, Department of Physics, National Tsinghua University（国立清华大学物理系天文学研究所）
- Department of Astronomy, University of Virginia（弗吉尼亚大学天文学系）
- Purdue University（普渡大学）
- Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Scienc（孔科利天文台，匈牙利研究与教育网络天文学与地球科学研究中心）
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