CMZoom III: Spectral line data release
CMZoom III: Spectral line data release
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CMZoom III：谱线数据发布
DOI：
10.1093/mnras/stad388
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发表时间：
2023
影响因子：
4.8
通讯作者：
Kauffmann, Jens
中科院分区：
文献类型：
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作者：
Callanan, Daniel;Longmore, Steven N.;Battersby, Cara;Hatchfield, H. Perry;Walker, Daniel L.;Henshaw, Jonathan;Keto, Eric;Barnes, Ashley;Ginsburg, Adam;Kauffmann, Jens
我们介绍了SMA大型项目CMZoom的谱线部分的概述和数据发布。在中央分子带（CMZ;银河系内部的几百pc）中，在柱密度大于1023 cm − 2的气体中，CMZ放大了12 CO（2 - 1）、13 CO（2-1）和C18 O（2-1）、H2 CO的三次跃迁、CH 3OH的几次跃迁、OCS的两次跃迁以及SiO和SO的单次跃迁。我们提取光谱从所有紧凑的1.3 mmCMZoomcontinuum源和拟合线轮廓的光谱。我们利用H2 CO 3（0，3）-2（0，2）跃迁的拟合结果来确定源的运动学性质。我们发现90%的CMZoom源的总质量有可靠的运动学。只有四个紧凑的连续源形式上是自引力的。其余的是一致的，在流体静力学平衡假设它们是由CMZ的高外部压力的限制。我们只发现了两个令人信服的原恒星流出，排除了以前未被发现的人口非常大，积极吸积YSO与强大的流出。最后，尽管有足够的灵敏度和分辨率来探测高速致密云（HVCC），这被认为是中等质量黑洞与分子气体云相互作用的证据，但我们在大的调查区域内没有发现这样的物体。
We present an overview and data release of the spectral line component of the SMA Large Program,CMZoom. CMZoomobserved12CO (2–1),13CO (2–1), and C18O (2–1), three transitions of H2CO, several transitions of CH3OH, two transitions of OCS, and single transitions of SiO and SO within gas above a column density of N(H2) ≥ 1023cm−2in the Central Molecular Zone (CMZ; inner few hundred pc of the Galaxy). We extract spectra from all compact 1.3 mmCMZoomcontinuum sources and fit line profiles to the spectra. We use the fit results from the H2CO 3(0, 3)–2(0, 2) transition to determine the source kinematic properties. We find ∼90 per cent of the total mass ofCMZoomsources have reliable kinematics. Only four compact continuum sources are formally self-gravitating. The remainder are consistent with being in hydrostatic equilibrium assuming that they are confined by the high external pressure in the CMZ. We find only two convincing proto-stellar outflows, ruling out a previously undetected population of very massive, actively accreting YSOs with strong outflows. Finally, despite having sufficient sensitivity and resolution to detect high-velocity compact clouds (HVCCs), which have been claimed as evidence for intermediate mass black holes interacting with molecular gas clouds, we find no such objects across the large survey area.