Identification of interstellar amino acetonitrile in the hot molecular core G10.47＋0.03: Possible glycine survey candidate for the future

Manna, Arijit; Pal, Sabyasachi

doi:10.1016/j.lssr.2022.04.002

Cited by 13 publications

(10 citation statements)

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“…Our estimated higher excitation temperature of CH 2 NH using ACA is accurate because the temperature of the hot molecular cores is above 100 K (van Dishoeck and Blake, 1998). The other two precursors of NH 2 CH 2 COOH, such as CH 3 NH 2 (Ohishi et al, 2019) and NH 2 CH 2 CN (Manna and Pal, 2022a) were also detected towards G10.47+0.03 using the NRO and ALMA telescopes. The detection of CH 2 NH towards G10.47+0.03 indicates that three possible precursors of NH 2 CH 2 COOH are present in G10.47+0.03.…”

Section: Discussionmentioning

confidence: 92%

“…Previously, Manna and Pal (2022a) claimed that NH 2 CH 2 CN was the daughter molecule of CH 2 NH (see Fig. 1).…”

Section: Discussionmentioning

confidence: 98%

“…6. In the chemical network, all reactions were obtained from Woon (2002) Searching of NH 2 CH 2 COOH towards the G10.47+0.03 using the ACA After the identification of three possible NH 2 CH 2 COOH precursor molecules like CH 2 NH (present paper), CH 3 NH 2 (Ohishi et al, 2019) and NH 2 CH 2 CN (Manna and Pal, 2022a) towards the G10.47+0.03, we searched the emission lines of NH 2 CH 2 COOH conformers I and II towards the G10.47+0.03. After the careful spectral analysis using the LTE model, we did not detect any evidence of NH 2 CH 2 COOH conformers I and II towards the G10.47+0.03 within the limits of our LTE modelling.…”

Section: Discussionmentioning

confidence: 99%

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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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Section: Discussionmentioning

confidence: 92%

“…Previously, Manna and Pal (2022a) claimed that NH 2 CH 2 CN was the daughter molecule of CH 2 NH (see Fig. 1).…”

Section: Discussionmentioning

confidence: 98%

Section: Discussionmentioning

confidence: 99%

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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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“…Emission lines of interstellar aminoacetonitrile were detected towards molecular clouds, such as Sgr B2(N) 36 and G10.47 + 0.03. 37,38 It has been suggested that aminoacetonitrile may be formed within, or on, interstellar ice mantles. 39,40 According to the pathways described above, Gly, NHCH 40 Second, extra energy sources are needed to overcome the high barriers over 200 kJ mol À1 .…”

Section: Astrochemical Implicationsmentioning

confidence: 99%

Mechanisms of glycine formation from aminoacetonitrile in space

Choe

2023

Phys. Chem. Chem. Phys.

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“…Hot molecular cores are early phases of massive star-formation regions, and most complex molecules, including glycine (NH 2 CH 2 COOH) precursors (NH 2 CH 2 CN, CH 2 NH, CH 3 NH 2 , etc. ), are frequently found in hot molecular cores. − The complex molecules in the hot molecular cores significantly increase the chemical richness of the ISM. Hot molecular cores are suitable candidates for studying individual complex organic molecules because they have a high gas density (≥10 6 cm –3 ), a small and compact source size (≤0.1 pc), and a warm gas temperature (≥100 K). , Most of the complex molecular lines arise mainly from the warm inner region of the envelope of hot cores. ,, The abundance of complex molecules varies from ∼10 –11 to ∼10 –7 .…”

Section: Introductionmentioning

confidence: 99%

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

Manna,

Pal

2024

ACS Earth Space Chem.

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In the interstellar medium (ISM), the complex prebiotic molecule cyanamide (NH 2 CN) plays a key role in producing adenine (C 5 H 5 N 5 ), purines (C 5 H 4 N 4 ), pyrimidines (C 4 H 4 N 2 ), and other biomolecules via a series of reactions. Therefore, studying the emission lines of NH 2 CN is important for understanding the hypothesis of the presolar origin of life in the universe. We present the detection of the rotational emission lines of NH 2 CN with vibrational states v = 0 and 1 toward the hot molecular core G31.41 + 0.31 using the high-resolution 12 meter array of the Atacama Large Millimeter/Submillimeter Array (ALMA) band 3. The estimated column density of NH 2 CN toward G31.41 + 0.31 using the local thermodynamic equilibrium (LTE) model is (7.21 ± 0.25) × 10 15 cm −2 with an excitation temperature of 250 ± 25 K. The abundance of NH 2 CN with respect to H 2 toward G31.41 + 0.31 is (7.21 ± 1.46) × 10 −10 . The NH 2 CN and NH 2 CHO column density ratio toward G31.41 + 0.31 is 0.13 ± 0.02. We compare the estimated abundance of NH 2 CN with that of other hot cores and corinos and observe that the abundance of NH 2 CN toward G31.41 + 0.31 is nearly similar to that of the hot molecular core G358.93 − 0.03 MM1, the hot corinos IRAS 16293-2422 B, and NGC 1333 IRAS4A2. We compute the two-phase warm-up chemical model of NH 2 CN using the gas-grain chemical code UCLCHEM, and after chemical modeling, we notice that the observed and modeled abundances are nearly similar. After chemical modeling, we conclude that the neutral−neutral reaction between NH 2 and CN is responsible for the production of NH 2 CN on the grain surface of G31.41 + 0.31.

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Identification of interstellar amino acetonitrile in the hot molecular core G10.47＋0.03: Possible glycine survey candidate for the future

Cited by 13 publications

References 9 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

Mechanisms of glycine formation from aminoacetonitrile in space

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

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