Exploring the formation pathways of formamide

Allen, V.; Tak, F. F. S. van der; López-Sepulcre, A.; Sánchez-Monge, Á.; Rivilla, V. M.; Cesaroni, R.

doi:10.1051/0004-6361/201935791

Cited by 9 publications

(5 citation statements)

References 33 publications

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“…Mendoza et al (2014) and López-Sepulcre et al ( 2015) reported a correlation between the abundance of NH 2 CHO and HNCO based on their survey observations toward various star-forming regions from low-mass to high-mass ones. The abundance relationship was also reported with the ALMA observations (Coutens et al 2016;Allen et al 2020) and was supported by theoretical calculation (Quénard et al 2018). These works suggest some chemical relations between the two species.…”

Section: Nh 2 Chosupporting

confidence: 80%

Molecular Distributions of the Disk/Envelope System of L483: Principal Component Analysis for the Image Cube Data

Okoda,

Oya,

Abe

et al. 2021

Preprint

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Unbiased understandings of molecular distributions in a disk/envelope system of a low-mass protostellar source are crucial for investigating physical and chemical evolution processes. We have observed 23 molecular lines toward the Class 0 protostellar source L483 with ALMA and have performed principal component analysis (PCA) for their cube data (PCA-3D) to characterize their distributions and velocity structures in the vicinity of the protostar. The sum of the contributions of the first three components is 63.1%. Most oxygen-bearing complex-organic-molecule lines have a large correlation with the first principal component (PC1), representing the overall structure of the disk/envelope system around the protostar. Contrary, the C 18 O and SiO emissions show small and negative correlations with PC1. The NH 2 CHO lines stand out conspicuously at the second principal component (PC2), revealing more compact distribution. The HNCO lines and the high excitation line of CH 3 OH have a similar trend for PC2 to NH 2 CHO. On the other hand, C 18 O is well correlated with the third principal component (PC3). Thus, PCA-3D enables us to elucidate the similarities and the differences of the distributions and the velocity structures among molecular lines simultaneously, so that the chemical differentiation between the oxygen-bearing complex organic molecules and the nitrogen-bearing ones is revealed in this source. We have also conducted PCA for the moment 0 maps (PCA-2D) and that for the spectral line profiles (PCA-1D). While they can extract part of characteristics of the molecular-line data, PCA-3D is essential for comprehensive understandings. Characteristic features of the molecular-line distributions are discussed on NH 2 CHO.

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Section: Nh 2 Chosupporting

confidence: 80%

Molecular Distributions of the Disk/Envelope System of L483: Principal Component Analysis for the Image Cube Data

Okoda,

Oya,

Abe

et al. 2021

Preprint

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“…Single dish observations, which found a constant abundance HNCO/NH 2 CHO ratio in a range of source luminosities and masses (Bisschop et al 2007;López-Sepulcre et al 2015), suggested that these molecules were chemically-related. Evidence of co-spatial emission in the low-mass protobinary system IRAS 16293 (Coutens et al 2016), two high-mass cores in G35.20 (Allen et al 2017), and six cores across three massive star-forming regions (Allen et al 2020) further indicated a link between the two species.…”

Section: Hnco and Nh2chomentioning

confidence: 99%

“…Trot values in italics are those adopted from similar species, as described in the text. Column density upper limits are derived using 3σ line intensity upper limits and by assuming the median line FWHM from a chemically-related or observationally-linked species (e.g., CH3CH2CN/CH2CHCN, HNCO/NH2CHO; Caselli et al 1993;Allen et al 2020) the same. CH 3 OCH 3 , despite its unique column density distribution, remains strongly correlated with CH 3 OH irrespective of the inclusion or exclusion of HC1.…”

Section: 047mentioning

confidence: 99%

Sub-arcsecond Imaging of the Complex Organic Chemistry in Massive Star-forming Region G10.6-0.4

Law,

Zhang,

Öberg

et al. 2021

Preprint

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Massive star-forming regions exhibit an extremely rich and diverse chemistry, which in principle provides a wealth of molecular probes, as well as laboratories for interstellar prebiotic chemistry. Since the chemical structure of these sources displays substantial spatial variation among species on small scales ( 10 4 au), high angular resolution observations are needed to connect chemical structures to local environments and inform astrochemical models of massive star formation. To address this, we present ALMA 1.3 mm observations toward OB cluster-forming region G10.6-0.4 (hereafter "G10.6") at a resolution of 0.14 (700 au). We find highly-structured emission from complex organic molecules (COMs) throughout the central 20,000 au, including two hot molecular cores and several shells or filaments. We present spatially-resolved rotational temperature and column density maps for a large sample of COMs and warm gas tracers. These maps reveal a range of gas substructure in both O-and N-bearing species. We identify several spatial correlations that can be explained by existing models of COM formation, including NH 2 CHO/HNCO and CH 3 OCHO/CH 3 OCH 3 , but also observe unexpected distributions and correlations which suggest that our current understanding of COM formation is far from complete. Importantly, complex chemistry is observed throughout G10.6, rather than being confined to hot cores. The COM composition appears to be different in the cores compared to the more extended structures, which illustrates the importance of high spatial resolution observations of molecular gas in elucidating the physical and chemical processes associated with massive star formation.

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“…cosmic diatomic molecule, to deoxyribonucleic acid (DNA), which can have order of 10 8 carbon atoms, the search and detection of organic molecules in space contribute to our understanding of the emergence of life. Research on molecules such as HNCO, H 2 CO, and NH 2 CHO has shed light on the interstellar chemistry of pre-biotic molecules and species carrying various biogenic elements (e.g., Saladino et al, 2006;Bisschop et al, 2007;Mendoza et al, 2014;López-Sepulcre et al, 2015;Allen et al, 2020;Jørgensen et al, 2020).…”

Section: The Organic Side Of the Galaxymentioning

confidence: 99%

Interrelations Between Astrochemistry and Galactic Dynamics

Mendoza

Duronea

Ronsó

et al. 2021

Front. Astron. Space Sci.

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This paper presents a review of ideas that interconnect astrochemistry and galactic dynamics. Since these two areas are vast and not recent, each one has already been covered separately by several reviews. After a general historical introduction, and a needed quick review of processes such as stellar nucleosynthesis that gives the base to understand the interstellar formation of simple chemical compounds (e.g., H2, CO, NH3, and H2O), we focus on a number of topics that are at the crossing of the two big areas, dynamics and astrochemistry. Astrochemistry is a flourishing field that intends to study the presence and formation of molecules as well as the influence of them on the structure, evolution, and dynamics of astronomical objects. The progress in the knowledge on the existence of new complex molecules and of their process of formation originates from the observational, experimental, and theoretical areas that compose the field. The interfacing areas include star formation, protoplanetary disks, the role of the spiral arms, and the chemical abundance gradients in the galactic disk. It often happens that the physical conditions in some regions of the interstellar medium are only revealed by means of molecular observations. To organize a rough classification of chemical evolution processes, we discuss about how astrochemistry can act in three different contexts, namely, the chemistry of the early universe, including external galaxies, star-forming regions, and asymptotic giant branch (AGB) stars and circumstellar envelopes. We mention that our research is stimulated by plans for instruments and projects, such as the ongoing Large Latin American Millimeter Array (LLAMA), which consists in the construction of a 12 m sub-mm radio telescope in the Andes. Thus, modern and new facilities can play a key role in new discoveries not only in astrochemistry but also in radio astronomy and related areas. Furthermore, the research on the origin of life is also a stimulating perspective.

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Exploring the formation pathways of formamide

Cited by 9 publications

References 33 publications

Molecular Distributions of the Disk/Envelope System of L483: Principal Component Analysis for the Image Cube Data

Molecular Distributions of the Disk/Envelope System of L483: Principal Component Analysis for the Image Cube Data

Sub-arcsecond Imaging of the Complex Organic Chemistry in Massive Star-forming Region G10.6-0.4

Interrelations Between Astrochemistry and Galactic Dynamics

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