A spectral line survey of Orion KL in the bands 486-492 and 541-577 GHz with the Odin satellite II. Data analysis
C. M. Persson, A. O. H. Olofsson, N. Koning, P. Bergman, P. Bernath, J. H. Black, U. Frisk, W. Geppert, T. I. Hasegawa, A. Hjalmarson, S. Kwok, B. Larsson, A. L… 展开作者
C. M. Persson, A. O. H. Olofsson, N. Koning, P. Bergman, P. Bernath, J. H. Black, U. Frisk, W. Geppert, T. I. Hasegawa, A. Hjalmarson, S. Kwok, B. Larsson, A. Lecacheux, A. Nummelin, M. Olberg, Aa. Sandqvist, E. S. Wirstrom
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51 pages, 47 figures, 35 tables, accepted for publication in Astronomy and Astrophysics 17 September 2007
We investigate the physical and chemical conditions in a typical star forming region, including an unbiased search for new molecules in a spectral region previously unobserved. Due to its proximity, the Orion KL region offers a unique laboratory of molecular astrophysics in a chemically rich, massive star forming region. Several ground-based spectral line surveys have been made, but due to the absorption by water and oxygen, the terrestrial atmosphere is completely opaque at frequencies around 487 and 557 GHz. To cover these frequencies we used the Odin satellite to perform a spectral line survey in the frequency ranges 486-492 GHz and 541-577 GHz, filling the gaps between previous spectral scans. Odin's high main beam efficiency and observations performed outside the atmosphere make our intensity scale very well determined. We observed 280 spectral lines from 38 molecules including isotopologues, and, in addition, 64 unidentified lines. The beam-averaged emission is dominated by CO, H2O, SO2, SO, 13CO and CH3OH. Species with the largest number of lines are CH3OH, (CH33)2O, SO2, 13CH3OH, CH3CN and NO. Six water lines are detected including the ground state rotational transition o-H2O, its isotopologues o-H218O and o-H217O, the Hot Core tracing p-H2O transition 6(2,4)-7(1,7), and the 2(0, 2)-1(1,1) transition of HDO. Other lines of special interest are the 1_0-0_0 transition of NH3 and its isotopologue 15NH3. Isotopologue abundance ratios of D/H, 12C/13C, 32S/34S, 34S/33S, and 18O/17O are estimated. The temperatures, column densities and abundances in the various subregions are estimated, and we find very high gas-phase abundances of H2O, NH3, SO2, SO, NO, and CH3OH. A comparison with the ice inventory of ISO sheds new light on the origin of the abundant gas-phase molecules.
Herschel observations of Extra-Ordinary Sources: Methanol as a probe of physical conditions in Orion KL
University of Michigan（密歇根大学）；Jet Propulsion Laboratory, Caltech（加州理工学院喷气推进实验室）；California Institute of Technology（加州理工学院）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Universität zu Köln（科隆大学）
Herschel observations of EXtra-Ordinary Sources: The Terahertz spectrum of Orion KL seen at high spectral resolution
University of Michigan（密歇根大学）；California Institute of Technology（加州理工学院）；Jet Propulsion Laboratory, Caltech（加州理工学院喷气推进实验室）；Observatoire de Paris（巴黎天文台）；Université de Toulouse [UPS]（图卢兹大学）；CNRS/INSU（法国国家科学研究中心）
Analysis of the Herschel/HEXOS Spectral Survey Towards Orion South: A massive protostellar envelope with strong external irradiation
我们目前的结果，从一个全面的亚毫米光谱调查对源猎户座南，获得的数据的基础上与HIFI仪器搭载的\textit{Herschel Space Observatory}，覆盖频率范围480至1900 GHz。我们用S/N $>$ 3 $σ$探测到685条光谱线，来自52种不同的分子和原子种类。我们模拟每个检测到的物种假设条件的局部热力学平衡。该分析提供了猎户座南的物理条件（柱密度，温度，源大小，\& V $_{LSR}$）的估计。我们发现了三种不同的云成分的证据：（T $_{ex} \sim 20-40$ K），空间扩展（$> 60"$）和静止（$ΔV_{FWHM} \sim 4$ km s $^{-1}$）分量;较暖的（T $_{ex} \sim 80-100$ K），空间延伸较小（$\sim 30"$）和动态（$ΔV_{FWHM} \sim 8$ km s $^{-1}$）分量，可能受到嵌入流出的影响;以及运动学上不同的区域（T $_{ex}$ $>$ 100 K; V $_{LSR}$ $\sim$ 8 km s $^{-1}$），主要是来自追踪紫外线辐射的物质的发射，可能在云的表面。我们发现一个化学上不同的“热芯”组件的存在的证据很少，可能是由于小填充因子的热芯或热芯内的\textit{Herschel}光束。我们发现，在较冷的气体的化学成分，猎户座南部的静态组件更接近猎户座K…
Q/W-band Observations toward Starless Cores in Orion (QWOSCO) I. Overview, Isotopologues, Isomers, and Complex Organics
Institute of Astronomy and Astrophysics, Academia Sinica（中央研究院天文及天文物理研究所）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；University of Helsinki（赫尔辛基大学）；Korea Astronomy and Space Science Institute（韩国天文学与空间科学研究所）；University of Science and Technology, Korea (UST)（韩国科学技术院）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）
A VLBA survey of radio stars in the Orion Nebula Cluster: III. Inter-epoch variability analysis
Centre for Astrophysics Research, University of Hertfordshire（赫特福德大学天体物理研究中心）；European Space Agency (ESA), European Space Research and Technology Centre (ESTEC)（欧洲航天局（ESA）欧洲空间研究与技术中心（ESTEC））；Joint ALMA Observatory（ALMA联合观测站）
Survey of Orion Disks with ALMA (SODA) I: Cloud-level demographics of 873 protoplanetary disks
对附近恒星形成区（SFR）的原行星盘的调查提供了有关其人口统计的重要信息，但由于样本量，它们不能用于研究盘的属性如何随环境而变化。我们进行了调查的873个原行星盘的未解决的毫米连续辐射的L1641和L1647地区的猎户座A云斯皮策确定。这是迄今为止最大的一次此类调查，使我们能够确定中等磁盘质量的微弱趋势，作为云和集群成员的位置的函数。还将样品检测率和中值质量与附近（<300 pc）SFR的样品检测率和中值质量进行比较。用ALMA在225 GHz下观察样品，中值rms为0.08 mJy/束（1.5 M $_{\oplus}$）。使用创新的并行数据处理方法对数据进行了简化和成像。我们检测到58%（502/873）的观察磁盘。这包括20个尘埃质量>100 M $_{\oplus}$的圆盘，以及与扩展尘埃排放相关的两个物体。我们推断在$2.2^{+0.2}_{-0.2}$ M $_{\oplus}$的整个样品中的平均盘尘埃质量。在L1641和L1647中，尘埃质量中值分别为$2.1^{+0.2}_{-0.2}$ M $_{\oplus}$和$2.6^{+0.4}_{-0.5}$ M $_{\oplus}$。完整样本的磁盘质量分布是类似的附近的低质量SFR在类似的年龄为1-3百万年。我们发现，只有微弱的趋势盘（尘埃）质量与银河经度和YSO集群之间的样本中确定的，与中位数质量变化$\lesss…
Nascent Embedded-protostar Survey in Taurus (NEST) II: Measuring Dust Mass, Disk Size, and Gas Mass
University of Virginia（弗吉尼亚大学）；National Radio Astronomy Observatory（美国国家射电天文台）；Space Science Institute（空间科学研究所）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；SKA Observatory（平方公里阵列射电望远镜观测站）；University of Arizona（亚利桑那大学）；National Sun Yat-Sen University（国立中山大学）；National Taiwan Normal University（台湾师范大学）
