Experimental and computational study of ethanolamine ices at astrochemical conditions
R Ramachandran, Milan Sil, Prasanta Gorai, J K Meka, S Pavithraa, J -I Lo, S -L Chou, Y -J Wu, P Janardhan, B -M Cheng, Anil Bhardwaj, Vıctor M. Rivilla, N J Ma… 展开作者
R Ramachandran, Milan Sil, Prasanta Gorai, J K Meka, S Pavithraa, J -I Lo, S -L Chou, Y -J Wu, P Janardhan, B -M Cheng, Anil Bhardwaj, Vıctor M. Rivilla, N J Mason, B Sivaraman, Ankan Das
Ethanolamine (NH2CH2CH2OH) has recently been identified in the molecular cloud G+0.693-0.027, situated in the SgrB2 complex in the Galactic center. However, its presence in other regions, and in particular in star-forming sites, is still elusive. Given its likely role as a precursor to simple amino acids, understanding its presence in the star-forming region is required. Here, we present the experimentally obtained temperature-dependent spectral features and morphological behavior of pure ethanolamine ices under astrochemical conditions in the 2 - 12 micro meter (MIR) and 120 - 230 nm (VUV) regions for the first time. These features would help in understanding its photochemical behavior. In addition, we present the first chemical models specifically dedicated to ethanolamine. These models include all the discussed chemical routes from the literature, along with the estimated binding energies and activation energies from quantum chemical calculations reported in this work. We have found that surface reactions: CH2OH + NH2CH2 --> NH2CH2CH2OH and NH2 + C2H4OH --> NH2CH2CH2OH in warmer regions (60-90 K) could play a significant role in the formation of ethanolamine. Our modeled abundance of ethanolamine complements the upper limit of ethanolamine column density estimated in earlier observations in hot core/corino regions. Furthermore, we provide a theoretical estimation of the rotational and distortional constants for various species (such as HNCCO, NH2CHCO, and NH2CH2CO) related to ethanolamine that have not been studied in existing literature. This study could be valuable for identifying these species in the future.
Electron irradiation and temperature-programmed desorption of layered ethanolamine-water-methanol ices
Zernike Institute for Advanced Materials, University of Groningen（格罗宁根大学泽尔尼克高级材料研究所）；Center for Astrochemical Studies, Max-Planck-Institut für Extraterrestrische Physik（马克斯·普朗克地外物理研究所天体化学研究中心）；Department of Bioscience, Technical University of Munich（慕尼黑工业大学生物科学系）；Síntesis y Mecanismos de Reacción en Química Orgánica, Departamento de Química, Universidad del Valle（瓦尔莱大学化学系有机化学反应合成与机理）；Semillero de investigación en Astroquímica y Astrobiología (AstroLUCA), Departamento de Química, Universidad del Valle（瓦尔莱大学化学系天体化学与天体生物学研究种子团队（AstroLUCA））；Faculty of Health Sciences, Universidad Libre（自由大学健康科学学院）；HUN-REN Institute for Nuclear Research（匈牙利研究与创新网络核子研究所）；Institute of Chemistry, University of Debrecen（德布勒森大学化学研究所）；Astronomical Institute, Slovak Academy of Sciences（斯洛伐克科学院天文研究所）
Modeling the UV-photon irradiation of CS$_2$-bearing ices in the laboratory with the pyRate gas-grain astrochemical code. New insights into the missing sulfur problem
Max-Planck-Institut für Extraterrestrische Physik (MPE)（马克斯·普朗克地外物理研究所）；Centro de Astrobiología (CSIC-INTA)（天体生物学中心（西班牙国家科学技术研究委员会-国家航空航天技术研究所））
The Galactic centre G+0.633-0.0604 molecular cloud: A new astrochemical gold mine: II. Chemical richness
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；Universidad Complutense de Madrid（马德里康普顿斯大学）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）；European Southern Observatory（欧洲南方天文台）；Joint ALMA Observatory（ALMA联合天文台）；RIKEN（理化学研究所）
Isotopomer-Specific Carbon Isotope Ratio of Complex Organic Molecules in Star-Forming Cores
National Astronomical Observatory of Japan（日本国立天文台）；The Graduate University for Advanced Studies, SOKENDAI（综合研究大学院大学）；RIKEN Cluster for Pioneering Research（理化学研究所前沿研究集群）；The University of Tokyo（东京大学）；Queen’s University Belfast（贝尔法斯特女王大学）
Influence of galactic arm scale dynamics on the molecular composition of the cold and dense ISM II. Molecular oxygen abundance
分子氧一直是许多观测研究的主题，因为化学模型预测它是氧气的储存库。虽然它已经在星际介质的两个区域被探测到，但它的稀有性对天体化学模型来说是一个挑战。在本文中，我们结合了计算的物理条件与光滑粒子流体动力学（SPH）模拟与我们的全气体颗粒化学模型鹦鹉螺，研究预测的O2丰度在星际物质形成冷芯。因此，我们遵循的气体和冰的化学演化的物质包裹从弥漫的星际条件冷致密的核心。我们的大多数预测的O2丰度低于1 e-8（相对于总质子密度）和预测的柱密度在模拟冷芯是在最大的几个1 e 14 cm-2，在协议的非检测限。这种低的O2丰度可以通过以下事实来解释，即在大部分星际材料中，在O2可以在气相中形成并且免受UV光解离之前，原子氧被耗尽到晶粒表面上（并且被氢化以形成H2O）。我们之所以能得到这个结果，是因为我们考虑了从弥散介质到冷核的物理条件演化的全部历史。
The role of the pre-exponential factor on temperature programmed desorption spectra: A computational study of frozen species on interstellar icy grain mantles
Mapping Interstellar Ice Inventory toward Class 0 Protostars in Star-forming Region Orion A with JWST Data
Ural Federal University（乌拉尔联邦大学）；Institute of Astronomy of the Russian Academy of Sciences（俄罗斯科学院天文研究所）；Institute of Natural Sciences and Mathematics, Ural Federal University（乌拉尔联邦大学自然科学与数学研究所）；Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）
