E. Mendoza, B. Lefloch, C. Ceccarelli, C. Kahane, A. A. Jaber, L. Podio, M. Benedettini, C. Codella, S. Viti, I. Jimenez-Serra, J. Lepine, H. M. Boechat-Roberty, R. Bachiller
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13 pages, 12 figures. Accepted for publication in Monthly Notices of the Royal Astronomical Society Main Journal
We present here a systematic search for cyanopolyynes in the shock region L1157-B1 and its associated protostar L1157-mm in the framework of the Large Program "Astrochemical Surveys At IRAM" (ASAI), dedicated to chemical surveys of solar-type star forming regions with the IRAM 30m telescope. Observations of the millimeter windows between 72 and 272 GHz permitted the detection of HC$_3$N and its $^{13}$C isotopologues, and HC$_5$N (for the first time in a protostellar shock region). In the shock, analysis of the line profiles shows that the emission arises from the outflow cavities associated with L1157-B1 and L1157-B2. Molecular abundances and excitation conditions were obtained from analysis of the Spectral Line Energy Distributions under the assumption of Local Thermodynamical Equilibrium or using a radiative transfer code in the Large Velocity Gradient approximation. Towards L1157mm, the HC$_3$N emission arises from the cold envelope ($T_{rot}=10$ K) and a higher-excitation region ($T_{rot}$= $31$ K) of smaller extent around the protostar. We did not find any evidence of $^{13}$C or D fractionation enrichment towards L1157-B1. We obtain a relative abundance ratio HC$_3$N/HC$_5$N of 3.3 in the shocked gas. We find an increase by a factor of 30 of the HC$_3$N abundance between the envelope of L1157-mm and the shock region itself. Altogether, these results are consistent with a scenario in which the bulk of HC$_3$N was produced by means of gas phase reactions in the passage of the shock. This scenario is supported by the predictions of a parametric shock code coupled with the chemical model UCL_CHEM.
Perihelion observations of interstellar comet 3I/ATLAS with the IRAM 30-m telescope
LIRA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université, Université de Paris（巴黎天文台）；IRAM（红外毫米波天文台）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Department of Physics, Catholic University of America（美利坚天主教大学物理系）；Department of Physics, American University（美利坚大学物理系）
Plateau de Bure High-z Blue-Sequence Survey 2 (PHIBSS2): Search for Secondary Sources, CO Luminosity Functions in the Field, and the Evolution of Molecular Gas Density through Cosmic Time
我们报告了在第二次Plateau de Bure高z蓝色序列巡天（PHIBSS 2）中，以z ~ 1-2处的CO（2-1）、CO（3-2）和CO（6-5）为目标，在110个立方体中寻找CO排放偶然源的结果。PHIBSS 2观测是IRAM Plateau de Bure干涉仪为期4年的遗留计划的一部分，旨在从分子气体库的角度研究早期星系演化。我们提出了一个目录的67个候选人从这次搜索的次要来源，与45的110个数据立方体显示的来源，除了主要目标，似乎是外地检测，无关的中央来源。这个星表包括红移、线宽、通量，以及基于它们的假阳性概率对它们的可靠性的估计。我们在3D-HST/CANDELS目录中搜索二次CO探测，并初步发现其中约64%具有光学对应物，我们使用它们来限制它们的红移。最后，我们使用我们的候选CO检测目录，以获得CO（2-1），CO（3-2），CO（4-3），CO（5-4）和CO（6-5）的光度函数在一个范围内的红移，以及分子气体的质量密度演化。尽管不同的方法，这些结果是在非常好的协议与以前的观测约束来自盲搜索深领域。它们提供了一个可以通过有针对性的观测进行的“深场”科学类型的例子。
The quest for complex molecules in space: Laboratory spectroscopy of n-butyl cyanide, n-C4H9CN, in the millimeter wave region and its astronomical search in Sagittarius B2(N)
CHEMOUT: CHEMical complexity in star-forming regions of the OUTer Galaxy. V. Chemical composition gradients as a function of the galactocentric radius
INAF - Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切里天文台）；Dipartimento di Fisica e Astronomia, Università di Firenze（佛罗伦萨大学物理与天文学系）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）；LUX, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université（巴黎天文台卢梭实验室（隶属于巴黎文理研究大学、法国国家科学研究中心、索邦大学））；Centro de Astrobiología (CAB), CSIC-INTA（西班牙国家航空航天技术研究所/西班牙国家科学研究委员会天体生物学中心）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Transdisciplinary Research Area (TRA) ‘Matter’/Argelander-Institut für Astronomie, University of Bonn（波恩大学阿尔兰德天体物理研究所跨学科研究领域‘物质’）；Department of Physics and Astronomy, University College London（伦敦大学学院物理与天文学系）；Institut de Ciències de l’Espai (ICE), CSIC（西班牙国家科学研究委员会空间科学研究所）
