First detection of methyl formate in the hot molecular core IRAS 18566+0408

Manna, Arijit; Pal, Sabyasachi

doi:10.1007/s10509-022-04132-8

Cited by 4 publications

(5 citation statements)

References 27 publications

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“…After the generation of the integrated emission maps of all identified lines of CH 2 NH, we estimated the emitting regions of CH 2 NH towards the G10.47+0.03 by fitting the 2D Gaussian over the integrated emission maps of CH 2 NH using the CASA task IMFIT. The deconvolved beam size of the emitting region of CH 2 NH was estimated by the following equation, where indicates the diameter of the circle whose area ( A ) corresponds to the 50% line peak of CH 2 NH and θ beam is the half-power width of the synthesized beam (Rivilla et al , 2017; Manna and Pal, 2022c, 2023b). The estimated emitting regions of the J = 2(0, 2) − 1(0, 1), J = 6(2, 4) − 7(1, 7), and J = 10(3, 7) − 11(2, 10) transitions of CH 2 NH were 10.520 (0.44 pc), 10.275 (0.430 pc), and 10.781 (0.451 pc).…”

Section: Resultsmentioning

confidence: 99%

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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Section: Resultsmentioning

confidence: 99%

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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“…The subsequential hydrogenation of the CH 2 CHCN form C 2 H 5 CN in the grain surface of the hot molecular cores and high-mass protostars (CH 2 CHCN + 2H → C 2 H 5 CN; Garrod 2013), through barrierless and exothermic radical-radical reactions (Singh et al 2021). This particular chemical reaction is demonstrated to be the most efficient way for the formation of C 2 H 5 CN towards the Sgr B2, G10.47+0.03, G31.41+0.31, and other molecular cores (Belloche et al 2009;Manna & Pal 2023;Mininni et al 2023). This reaction may be most efficient towards IRAS 18089 because HC 3 N acts as a possible precursor of C 2 H 5 CN, and we detected the emission lines of HC 3 N from this source, which we already discussed in this paper.…”

Section: Discussionmentioning

confidence: 99%

“…In the hot molecular cores and high-mass protostars, CH 3 OCHO molecule can efficiently be formed by the reaction of CH 3 O and HCO radicals on the surface of dust grains (CH 3 O + HCO → CH 3 OCHO) (see Garrod et al 2008, and references therein). Earlier, Manna & Pal (2022) showed that the reactions between radical CH 3 O and radical HCO produce CH 3 OCHO towards the hot molecular core IRAS 18566+0408. Garrod (2013) showed the chemical reaction between CH 3 O and HCO is mobile between 30-40 K, and this chemical reaction is the most efficient pathway to the formation of CH 3 OCHO towards the hot molecular cores and high-mass protostars.…”

Section: Methyl Formate (Ch 3 Ocho)mentioning

confidence: 99%

“…Additionally, the Goldreich-Kylafis effect was observed for the CO (J = 3-2) emission line, which revealed a linear polarization fraction of up to 8% (Beuther et al 2010). The H 2 O and CH 3 OH maser emissions were also detected towards the IRAS 18089 (Beuther et al 2002b (Gorai et al 2020;Mondal et al 2021;Manna & Pal 2023;Mondal et al 2023), G31.41+0.31 (Mininni et al 2023), Orion KL (Beuther et al 2005a), Sgr B2 (N) (Belloche et al 2013), and low-mass protostar IRAS 16293-2422 (Jørgensen et al 2016;Calcutt et al 2018). The paper is organized in the following manner.…”

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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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“…In the hot molecular cores and high-mass protostars, the CH 3 OCHO molecule can efficiently be formed by the reaction of CH 3 O and HCO radicals on the surface of dust grains Garrod et al 2008, and references therein). Earlier, Manna & Pal (2022) showed that the reactions between radical CH 3 O and radical HCO produce CH 3 OCHO toward the hot molecular core IRAS 18566+0408. Garrod (2013) showed the chemical reaction between CH 3 O and HCO is mobile between 30 and 40 K, and this chemical reaction is the most efficient pathway to the formation of CH 3 OCHO toward the hot molecular cores and high-mass protostars.…”

Section: Methyl Formate (Ch 3 Ocho)mentioning

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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First detection of methyl formate in the hot molecular core IRAS 18566+0408

Cited by 4 publications

References 27 publications

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

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

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

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

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