标题： ALMA-QUARKS巡天调查：-- I. 巡天描述与数据处理 显示英文标题

标题： The ALMA-QUARKS survey: -- I. Survey description and data reduction

摘要： 本文综述了QUARKS巡天的概况，QUARKS是“利用ALMA解析的气体运动学和结构研究大质量恒星形成机制”的缩写。QUARKS巡天正在观测阿尔玛6波段（$\lambda\sim$1.3毫米）覆盖的139个大质量团块，共156个指向点。结合来自ALMA-ATOMS 3波段巡天的数据（$\lambda\sim$3毫米），QUARKS旨在对原星团中的大质量恒星形成过程进行无偏统计学研究，尺度可达1000天文单位。这篇综述文章描述了QUARKS巡天的观测和数据处理，并首次展示了代表性源——人马座B2(M)小星爆的例子。QUARKS巡天的宽带（7.5 GHz）和高角分辨率（~0.3弧秒）观测能够分辨出比ATOMS巡天更多的致密核心，并检测到之前未揭示的更微弱的丝状结构。光谱窗口覆盖了包括CO、SO、N$_2$D$^+$、SiO、H$_{30}\alpha$、H$_2$CO、CH$_3$CN以及许多其他复杂有机分子的跃迁，用于追踪具有不同温度和空间范围的气体组分。QUARKS的目标是深化我们对大质量恒星形成几个科学课题的理解，如原星团内的质量传输通过（枢纽）丝状结构、大质量恒星初始核心的存在、原星团内密集核心的物理和化学性质，以及已经形成的高大质量年轻原恒星的反馈效应。 显示英文摘要

摘要： This paper presents an overview of the QUARKS survey, which stands for `Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures'. The QUARKS survey is observing 139 massive clumps covered by 156 pointings at ALMA Band 6 ($\lambda\sim$ 1.3 mm). In conjunction with data obtained from the ALMA-ATOMS survey at Band 3 ($\lambda\sim$ 3 mm), QUARKS aims to carry out an unbiased statistical investigation of massive star formation process within protoclusters down to a scale of 1000 au. This overview paper describes the observations and data reduction of the QUARKS survey, and gives a first look at an exemplar source, the mini-starburst Sgr B2(M). The wide-bandwidth (7.5 GHz) and high-angular-resolution (~0.3 arcsec) observations of the QUARKS survey allow to resolve much more compact cores than could be done by the ATOMS survey, and to detect previously unrevealed fainter filamentary structures. The spectral windows cover transitions of species including CO, SO, N$_2$D$^+$, SiO, H$_{30}\alpha$, H$_2$CO, CH$_3$CN and many other complex organic molecules, tracing gas components with different temperatures and spatial extents. QUARKS aims to deepen our understanding of several scientific topics of massive star formation, such as the mass transport within protoclusters by (hub-)filamentary structures, the existence of massive starless cores, the physical and chemical properties of dense cores within protoclusters, and the feedback from already formed high-mass young protostars.