CMZoom: Survey Overview and First Data Release
CMZoom: Survey Overview and First Data Release
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DOI：
10.3847/1538-4365/aba18e
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发表时间：
2020-07
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通讯作者：
C. Battersby;E. Keto;D. Walker;A. Barnes;D. Callanan;A. Ginsburg;H. P. Hatchfield;J. Henshaw;J. Kauffmann;J. Kruijssen;S. Longmore;Xing Lu;Elisabeth A. C. Mills;T. Pillai;Qizhou Zhang;J. Bally;N. Butterfield;Yanett Contreras;Luis C. Ho;J. Ott;N. Patel;V. Tolls
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作者：
C. Battersby;E. Keto;D. Walker;A. Barnes;D. Callanan;A. Ginsburg;H. P. Hatchfield;J. Henshaw;J. Kauffmann;J. Kruijssen;S. Longmore;Xing Lu;Elisabeth A. C. Mills;T. Pillai;Qizhou Zhang;J. Bally;N. Butterfield;Yanett Contreras;Luis C. Ho;J. Ott;N. Patel;V. Tolls
我们概述了 CMZoom 调查及其首次数据发布。 CMZoom 是第一个以对大质量恒星前体敏感的波长对中央分子带（CMZ；银河系内部 500 片）进行盲测的高分辨率观测。 CMZoom 是亚毫米阵列上的一个 550 小时大型程序，以 ∼3 英寸（0.1 pc）的分辨率绘制了 1.3 毫米处 CMZ 中氢分子柱密度 1023 cm−2 以上的所有气体和尘埃。在本文中，我们重点关注 1.3 毫米灰尘连续体及其数据发布，同时也描述了将在即将出版的出版物中发布的 CMZoom 谱线数据。虽然 CMZoom 检测到许多具有丰富且复杂的子结构的区域，但其主要结果是 0.1-2 pc 尺度上致密子结构（致密致密气体组分：CDGF）的整体缺陷。与银盘中的云相比，尽管 CMZ 中的平均柱密度要高得多，但 CDGF 却要低得多。具有高 CDGF 的 CMZ 云是众所周知的活跃恒星形成场所。 CMZ 中的大多数气体无法形成致密的亚结构，这可能是 CMZ 中缺乏恒星形成的原因，考虑到其高密度，这一点令人惊讶。造成低 CDGF 的因素尚不清楚，但很可能是由于 CMZ 的极端环境造成的，这对我们理解整个宇宙的恒星形成过程具有深远的影响。
We present an overview of the CMZoom survey and its first data release. CMZoom is the first blind, high-resolution survey of the Central Molecular Zone (CMZ; the inner 500 pc of the Milky Way) at wavelengths sensitive to the pre-cursors of high-mass stars. CMZoom is a 550 hr Large Program on the Submillimeter Array that mapped at 1.3 mm all of the gas and dust in the CMZ above a molecular hydrogen column density of 1023 cm−2 at a resolution of ∼3″ (0.1 pc). In this paper, we focus on the 1.3 mm dust continuum and its data release, but also describe CMZoom spectral line data which will be released in a forthcoming publication. While CMZoom detected many regions with rich and complex substructure, its key result is an overall deficit in compact substructures on 0.1–2 pc scales (the compact dense gas fraction: CDGF). In comparison with clouds in the Galactic disk, the CDGF in the CMZ is substantially lower, despite having much higher average column densities. CMZ clouds with high CDGFs are well-known sites of active star formation. The inability of most gas in the CMZ to form compact substructures is likely responsible for the dearth of star formation in the CMZ, surprising considering its high density. The factors responsible for the low CDGF are not yet understood but are plausibly due to the extreme environment of the CMZ, having far-reaching ramifications for our understanding of the star formation process across the cosmos.