Detection and Chemical Modeling of Complex Prebiotic Molecule Cyanamide in the Hot Molecular Core G31.41 + 0.31

Manna, Arijit; Pal, Sabyasachi

doi:10.1021/acsearthspacechem.3c00245

Cited by 4 publications

(3 citation statements)

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“…UV radiation photodissociates these surface ices, and when the cloud core heats up during the protostellar phase, the fragments become mobile. Consequently, complex molecules are formed during the subsequent recombination of the photofragments and evaporate when the grain temperature increases above the ice sublimation temperature of 100 K (Garrod & Herbst 2006;Garrod et al 2008;Manna & Pal 2024). For example, CH 3 OCH 3 , CH 3 OCHO, and C 2 H 5 OH are formed by UV processing of CH 3 OH ice (Öberg et al 2009).…”

Section: Introductionmentioning

confidence: 99%

Study of Complex Nitrogen and Oxygen-bearing Molecules toward the High-mass Protostar IRAS 18089–1732

Manna,

Pal,

Baug

et al. 2024

Res. Astron. Astrophys.

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The observation of oxygen (O)- and nitrogen (N)-bearing molecules gives an idea about the complex prebiotic chemistry in the interstellar medium (ISM). Recent millimeter and submillimeter wavelength observations have shown the presence of complex O- and N-bearing molecules in the star-formation regions. So, the investigation of those molecules is crucial to understanding the chemical complexity in the star-forming regions. In this article, we present the identification of the rotational emission lines of N-bearing molecules ethyl cyanide (C2H5CN), cyanoacetylene (HC3N), and O-bearing molecules methyl formate (CH3OCHO) towards high-mass protostar IRAS 18089–1732 using the Atacama Compact Array (ACA). We also detected the emission lines of both N- and O-bearing molecule formamide (NH2CHO) in the envelope of IRAS 18089–1732. We have detected the v = 0 and 1 states rotational emission lines of CH3OCHO. We also detected the two vibrationally excited states of HC3N (v7 = 1 and v7 = 2). The estimated fractional abundances of C2H5CN, HC3N (v7 = 1), HC3N (v7 = 2), and NH2CHO towards the IRAS 18089–1732 are (1.40±0.5)×10^{−10}, (7.5±0.7)×10^{−11}, (3.1±0.4)×10^{−11}, and (6.25±0.82)×10^{−11}. Similarly, the estimated fractional abundances of CH3OCHO (v = 0) and CH 3 OCHO (v = 1) are (1.90±0.9)×10^{−9} and (8.90±0.8)×10^{−10}, respectively. We also created the integrated emission maps of the detected molecules, and the observed molecules may have originated from the extended envelope of the protostar. We show that C2H5CN and HC3N are most probably formed via the subsequential hydrogenation of the CH2CHCN and the reaction between C2H2 and CN on the grain surface of IRAS 18089–1732. We found that NH2CHO is probably produced due to the reaction between NH2 and H2CO in the gas phase. Similarly, CH3OCHO is possibly created via the reaction between radical CH3O and radical HCO on the grain surface of IRAS 18089–1732.

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Section: Introductionmentioning

confidence: 99%

Study of Complex Nitrogen and Oxygen-bearing Molecules toward the High-mass Protostar IRAS 18089–1732

Manna,

Pal,

Baug

et al. 2024

Res. Astron. Astrophys.

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“…Most chemical models of protostellar sources and hot molecular cores utilize grain surface chemistry to produce different types of complex organic compounds (Tielens & Charnley 1997;Garrod 2013;Manna & Pal 2024). The hydrogenation of solid oxygen (O), carbon (C), nitrogen (N), and carbon monoxide (CO) in the cold (≤20 K) prestellar phase produces CH 3 OH and other hydrogenated species such as H 2 O, NH 3 , and CH 4 (Tielens & Hagen 1982).…”

mentioning

confidence: 99%

“…Ultraviolet radiation photodissociates these surface ices, and when the cloud core heats up during the protostellar phase, the fragments become mobile. Consequently, complex molecules are formed during the subsequent recombination of the photofragments and evaporate when the grain temperature increases above the ice sublimation temperature of ≥100 K (Garrod & Herbst 2006;Garrod et al 2008;Manna & Pal 2024). For example, CH 3 OCH 3 , CH 3 OCHO, and C 2 H 5 OH are formed by UV processing of CH 3 OH ice ( Öberg et al 2009).…”

mentioning

confidence: 99%

Survey of Monocot ethno-medicinal plants in Purba Medinipur, Paschim Medinipur and Jhargram districts of West Bengal, India

Samanta¹,

Maity²,

Panda³

2023

Flora and Fauna

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Present study is on ethno-medicinal uses of 59 monocotyledonous plants in Purba Medinipur, Paschim Medinipur and Jhargram districts of West Bengal in India. Herbal uses against many common diseases such as epilepsy, rheumatism, kidney disorder, heart ailments, leprosy, jaundice, dysentery, toothache, diarrhoea, diabetes, alopecia, snakebite, piles, leucoderma, bronchitis, arthritis, menstrual disorder, tuberculosis, ulcers, dyspepsia, boils, indigestion, etc. have been recorded. Relevant uses of 59 flowering plant species along with family, local name (s), habit and parts used are discussed in this paper.

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Detection and prebiotic chemistry of possible glycine precursor molecule methylenimine towards the hot molecular core G10.47+0.03

Manna,

Pal

2024

International Journal of Astrobiology

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Amino acids are essential for the synthesis of protein. Amino acids contain both amine (R–NH2) and carboxylic acid (R–COOH) functional groups, which help to understand the possible formation mechanism of life in the universe. Among the 20 types of amino acids, glycine (NH2CH2COOH) is known as the simplest non-essential amino acid. In the last 40 years, all surveys of NH2CH2COOH in the interstellar medium, especially in the star-formation regions, have failed at the millimetre and sub-millimetre wavelengths. We aimed to identify the possible precursors of NH2CH2COOH, because it is highly challenging to identify NH2CH2COOH in the interstellar medium. Many laboratory experiments have suggested that methylenimine (CH2NH) plays a key role as a possible precursor of NH2CH2COOH in the star-formation regions via the Strecker synthesis reaction. After spectral analysis using the local thermodynamic equilibrium (LTE) model, we successfully identified the rotational emission lines of CH2NH towards the hot molecular core G10.47+0.03 using the Atacama Compact Array (ACA). The estimated column density of CH2NH towards G10.47+0.03 is (3.40 ± 0.2) × 1015 cm−2 with a rotational temperature of 218.70 ± 20 K, which is estimated from the rotational diagram. The fractional abundance of CH2NH with respect to H2 towards G10.47+0.03 is 2.61 × 10−8. We found that the derived abundance of CH2NH agree fairly well with the existing two-phase warm-up chemical modelling abundance value of CH2NH. We discuss the possible formation pathways of CH2NH within the context of hot molecular cores, and we find that CH2NH is likely mainly formed via neutral–neutral gas-phase reactions of CH3 and NH radicals towards G10.47+0.03.

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Detection and Chemical Modeling of Complex Prebiotic Molecule Cyanamide in the Hot Molecular Core G31.41 + 0.31

Cited by 4 publications

References 42 publications

Study of Complex Nitrogen and Oxygen-bearing Molecules toward the High-mass Protostar IRAS 18089–1732

Study of Complex Nitrogen and Oxygen-bearing Molecules toward the High-mass Protostar IRAS 18089–1732

Survey of Monocot ethno-medicinal plants in Purba Medinipur, Paschim Medinipur and Jhargram districts of West Bengal, India

Detection and prebiotic chemistry of possible glycine precursor molecule methylenimine towards the hot molecular core G10.47+0.03

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