猎户座KL的线混淆限制毫米巡天。II：含硅物质

Sulfur-bearing molecules in Orion KL

We present an observational study of the sulfur (S)-bearing species towards Orion KL at 1.3 mm by combining ALMA and IRAM-30\,m single-dish data. At a linear resolution of $\sim$800 au and a velocity resolution of 1 $\mathrm{km\, s^{-1}\, }$, we have identified 79 molecular lines from 6 S-bearing species. In these S-bearing species, we found a clear dichotomy between carbon-sulfur compounds and carbon-free S-bearing species in various characteristics, e.g., line profiles, spatial morphology, and molecular abundances with respect to $\rm H_2$. Lines from the carbon-sulfur compounds (i.e., OCS, …

Orion-KL =3 mm连续谱的高空间分辨率研究

A High Spatial Resolution Study of the λ=3 mm Continuum of Orion-KL

最近的干涉观测对猎户座KL区域的传统观点提出了质疑，该区域显示了恒星形成区域中化学分化的最明确的情况之一。之前，猎户座KL的低分辨率图像显示了朝向猎户座致密岭的含氧有机分子的发射特征，以及朝向猎户座热核的含氮有机分子的发射特征。然而，最近在更高的空间分辨率下的观测表明，大部分的分子发射是由许多较小的，紧凑的团块，空间上不同于传统的热核和紧凑岭源。正是这种类型的观测信息对于指导天体化学模型至关重要，因为分子的空间分布及其与能量源的关系将决定恒星形成区域中起作用的化学机制。我们已经进行了毫米成像研究的猎户座-KL与各种光束尺寸使用CARMA，以调查的连续结构。这些λ i = 3 mm的观测结果具有约0.5”-5.0”的合成射束尺寸。这些观测结果揭示了该地区复杂的连续结构，这与以前基于较低空间分辨率图像为Orion-KL假设的结构模型形成鲜明对比。新的结果表明，以前用于确定该地区的分子丰度的空间尺度需要完全修订。在这里，我们提出了连续观测的结果，讨论了检测到的源的大小和结构，并提出了一个观测策略，用于确定适当的空间尺度，以准确地确定在猎户座KL地区的分子丰度。

LMT 2毫米接收机系统（B4R）. II. 面向Orion-KL/OMC-1的科学演示观测

The LMT 2 millimeter receiver system (B4R). II. Science demonstration observations toward Orion-KL/OMC-1

B4R在Orion-KL/OMC-1的科学演示观测中展示了其在星际化学研究中的强大能力，通过高分辨率光谱分析识别出多种分子。

CARMA $λ$ = 1 cm Spectral Line Survey of Orion-KL

Orion-KL is a well known high mass star forming region that has long been the target of spectral line surveys and searches for complex molecules. One spectral window where the region had never been surveyed is around wavelengths of $λ$=1 cm. This is an important window to observe due to the fundamental and low energy transitions of numerous complex molecules that indicate the maximum spatial extent of the molecular species; knowing the spatial distribution of a molecule aids in determining the formation mechanism(s) of that molecule. Additionally, there are fewer transitions in this window, re…

Angular Momentum of the N2H+ Cores in the Orion A Cloud

We have analyzed the angular momentum of the molecular cloud cores in the Orion A giant molecular cloud observed in the N2H+ J = 1-0 line with the Nobeyama 45 m radio telescope. We have measured the velocity gradient using position velocity diagrams passing through core centers, and made sinusoidal fitting against the position angle. 27 out of 34 N2H+ cores allowed us to measure the velocity gradient without serious confusion. The derived velocity gradient ranges from 0.5 to 7.8 km/s/pc. We marginally found that the specific angular momentum J/M (against the core radius R) of the Orion N2H+ co…

Orion KL中反式乙基甲基醚的寻找

Searching for Trans Ethyl Methyl Ether in Orion KL

我们报告的$trans$乙基甲基醚（tEME），$t-CH_3CH_2OCH_3$，通过识别大量的旋转线，从每一个自旋状态的分子对猎户座KL的试探性检测。我们还搜索了$gauche$ - $trans$ -正丙醇，$Gt-n-CH_3CH_2CH_2OH$，一种相同来源的tEME异构体。我们在IRAM 30米测线调查和ALMA科学验证数据中确定了这两个物种的线。我们已经获得了ALMA地图，以建立这些物种的空间分布。而tEME主要来自猎户座的紧凑的脊组件，Gt-n-丙醇出现在乙醇的发射峰（南热芯）。对于tEME和Gt-n-丙醇，这些物质在其发射峰位置处的衍生柱密度分别为$\leq(4.0\pm0.8)\times10^{15} cm^{-2}$和$\leq(1.0\pm0.2)\times10^{15} cm^{-2}$。两种分子的旋转温度均为$\sim100 K$。我们还提供了$CH_3OCOH$，$CH_3CH_2OCOH$，$CH_3OCH_3$，$CH_3OH$和$CH_3CH_2OH$的地图，比较这些有机饱和含氧物种在这一地区的分布。提供了相关物种的丰度比和未检测到的醚的丰度上限。我们推导出猎户座致密脊中$N(CH_3OCH_3)/N(tEME)\geq150$的丰度比$N(CH_3OCH_3)/N(tEME)\geq150$。

The Difference in Abundances between N-bearing and O-bearing Species in High-Mass Star-Forming Regions

The different spatial distributions of N-bearing and O-bearing species, as is well known towards Orion~KL, is one of the long-lasting mysteries. We conducted a survey observation and chemical modeling study to investigate if the different distributions of O- and N-bearing species are widely recognized in general star-forming regions. First, we report our observational results of complex organic molecules (COMs) with the 45~m radio telescope at the Nobeyama Radio Observatory towards eight star-forming regions. Through our spectral survey ranging from 80 to 108~GHz, we detected CH$_3$OH, HCOOCH$…

分子云中的含硫物质

Sulfur-bearing species in molecular clouds

我们研究了几种分子，这些分子可以帮助解决稠密云层和星周区域中缺少硫的问题，以及澄清彗星中的硫化学。这些硫分子是：三聚体（CH 2S）3和四聚体（CH 2S）4，它们是硫代甲醛、五硫杂环庚烷S5 CH 2、六硫杂环庚烷S6 CH 2、硫杂环丙烷C2 H4 S、三硫烷HSSSH和硫代丙酮（CH 3）2CS。用密度泛函理论计算了这些化合物的红外光谱。大多数计算的波段属于中红外，其中一些发生在近红外和远红外区域。我们认为红外空间天文台在几个活动星系核和星暴星系中观测到的一些未识别的光谱特征可能是由1，3，5-三硫杂环己烷（（CH_2S）_3），1，3，5，7-四硫杂环己烷（（CH_2S）_4）和硫杂环丙烷（C_2H_4S）引起的。与计算波段比较的未识别红外特征的天体是：NGC 253，M82，NGC 1068，Circinus，Arp 220，30 Doradus，Orion KL和Sgr B2。

ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): I. Detection of New Hot Corinos with ACA

We report the detection of four new hot corino sources, G211.47-19.27S, G208.68-19.20N1, G210.49-19.79W and G192.12-11.10 from a survey study of Planck Galactic Cold Clumps in the Orion Molecular Cloud Complex with the Atacama Compact Array (ACA). Three sources had been identified as low mass Class 0 protostars in the Herschel Orion Protostar Survey (HOPS). One source in the lambda Orionis region is firstly reported as a protostellar core. We have observed abundant complex organic molecules (COMs), primarily methanol but also other oxygen-bearing COMs (in G211.47-19.27S and G208.68-19.20N1) an…

猎户座棒状结构中的亚角秒HCN和CN成像：致密环境中紫外驱动的暖氮化学

Sub-arcsecond imaging of HCN and CN in the Orion Bar. UV-driven warm Nitrogen chemistry in dense environments

利用ALMA亚角秒成像观测猎户座棒状结构中的HCN和CN发射，发现其峰值靠近离解前沿，揭示紫外驱动化学在致密环境中形成暖氮气体并示踪密度梯度。

ALMA对猎户座普朗克银河冷团块的观测巡天(ALMASOP)：SiO和CO辐射揭示的流出流的嵌套形态与运动学结构

ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Nested Morphological and Kinematic Structures of Outflows Revealed in SiO and CO Emission

ALMASOP巡天通过CO和SiO辐射揭示了猎户座分子流出流的复杂嵌套形态与运动学特征，并在喷流、风和环境介质统一模型框架下解释了这些由磁相互作用诱导的结构。

使用ALMA在3毫米波段对IRAS16293-2422 B进行大质量复杂有机分子的深度搜寻

A deep search for large complex organic species toward IRAS16293-2422 B at 3 mm with ALMA

本研究使用ALMA在3mm波段对IRAS 16293-2422 B进行深度搜寻，识别了31种分子，发现Band 3与Band 7的柱密度结果相似，但未探测到甘油等更大复杂分子，表明需更低频的深度巡天。

年轻大质量原恒星NGC 2264 CMM3在4 mm、3 mm和0.8 mm波段的谱线测量

Spectral Line Survey toward Young Massive Protostar NGC 2264 CMM3 in the 4 mm, 3 mm, and 0.8 mm Bands

利用野边山45 m望远镜和阿塔卡玛亚毫米望远镜实验（ASTE）10 m望远镜，在4 mm、3 mm和0.8 mm波段对大质量原恒星候选者NGC 2264 CMM 3进行了谱线巡天观测。在4 mm和3 mm波段总共检测到265条发射线，在0.8mm波段检测到74条发射线。结果，鉴定出36种分子物种和30种同位素体。除了基本的分子种类，许多碳链分子的发射线，如HC 5 N，C4 H，CCS和C3 S的检测在4毫米和3毫米波段。氘代分子物种也检测到相对较强的强度。另一方面，发现复杂有机分子如HCOOCH 3和CH 3 OCH 3的发射线较弱。对于检测到多重跃迁的分子，除了CH_3OH之外，旋转温度被导出为7-33 K。CH 3OH的发射谱线具有较高的上能级能量（Eu > 150 K），表明存在一个热核。与猎户座KL的化学组成相比，发现NGC 2264 CMM 3中碳链分子和氘化分子丰富，而含硫物种和复杂有机分子缺乏。这些特征表明NGC 2264 CMM 3的化学年轻，尽管它位于星系团形成核心NGC 2264 C的中心。