RECORD
Detection of possible glycine precursor molecule methylamine towards the hot molecular core G358.93$-$0.03 MM1
Astrophysics of Galaxies · Submitted 26 Feb 2024
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim After spectral analysis using the local thermodynamic equilibrium (LTE) model, we identified the rotational emission lines of CH$_{3}$NH$_{2}$ towards the hot molecular core G358.93$-$0.03 MM1 using the Atacama Large Millimeter/Submillimeter Array (ALMA).
The compiled record
The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.
Open the compiled record
The abstract, sentence by sentence
The search for the simplest amino acid, glycine (NH$_{2}$CH$_{2}$COOH), in the interstellar medium (ISM), has become a never-ending story for astrochemistry and astrophysics researchers because that molecule plays a possible connection between the Universe and the origin of life. In the last forty years, all searches for NH$_{2}$CH$_{2}$COOH in the ISM at millimeter and submillimeter wavelengths have failed. Since the detection of NH$_{2}$CH$_{2}$COOH in the ISM was extremely difficult, we aimed to search for the possible precursors of NH$_{2}$CH$_{2}$COOH. Earlier, many laboratory experiments have suggested that methylamine (CH$_{3}$NH$_{2}$) plays an important role in the ISM as a possible precursor of NH$_{2}$CH$_{2}$COOH. After spectral analysis using the local thermodynamic equilibrium (LTE) model, we identified the rotational emission lines of CH$_{3}$NH$_{2}$ towards the hot molecular core G358.93$-$0.03 MM1 using the Atacama Large Millimeter/Submillimeter Array (ALMA). The column density of CH$_{3}$NH$_{2}$ towards the G358.93$-$0.03 MM1 was estimated to be (1.10$\pm$0.31)$\times$10$^{17}$ cm$^{-2}$ with an excitation temperature of 180.8$\pm$25.5 K. The fractional abundance of CH$_{3}$NH$_{2}$ with respect to H$_{2}$ towards the G358.93$-$0.03 MM1 was (8.80$\pm$2.60)$\times$10$^{-8}$. The column density ratio of CH$_{3}$NH$_{2}$ and NH$_{2}$CN towards G358.93$-$0.03 MM1 was (1.86$\pm$0.95)$\times$10$^{2}$. The estimated fractional abundance of CH$_{3}$NH$_{2}$ towards the G358.93$-$0.03 MM1 agrees fairly well with the previous three-phase warm-up chemical modelling abundance of CH$_{3}$NH$_{2}$. We also discussed the possible formation mechanism of CH$_{3}$NH$_{2}$, and we find that CH$_{3}$NH$_{2}$ is most probably formed via the reactions of radical CH$_{3}$ and radical NH$_{2}$ on the grain surface of G358.93$-$0.03 MM1.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The search for the simplest amino acid, glycine (NH$_{2}$CH$_{2}$COOH), in the interstellar medium (ISM), has become a never-ending story for astrochemistry and astrophysics researchers because that molecule plays a possible connection between the Universe and the origin of life. | background 1.00 | 0.05 | 0.03 | hedged possibility 0.81 |
| s1 | In the last forty years, all searches for NH$_{2}$CH$_{2}$COOH in the ISM at millimeter and submillimeter wavelengths have failed. | background 0.55 | 0.05 | 0.02 | asserted 1.00 |
| s2 | Since the detection of NH$_{2}$CH$_{2}$COOH in the ISM was extremely difficult, we aimed to search for the possible precursors of NH$_{2}$CH$_{2}$COOH. | contribution 0.59 | 0.42 | 0.03 | asserted 0.97 |
| s3 | Earlier, many laboratory experiments have suggested that methylamine (CH$_{3}$NH$_{2}$) plays an important role in the ISM as a possible precursor of NH$_{2}$CH$_{2}$COOH. | background 1.00 | 0.03 | 0.04 | hedged possibility 0.96 |
| s4 | After spectral analysis using the local thermodynamic equilibrium (LTE) model, we identified the rotational emission lines of CH$_{3}$NH$_{2}$ towards the hot molecular core G358.93$-$0.03 MM1 using the Atacama Large Millimeter/Submillimeter Array (ALMA). | result 0.40 | 0.98 | 0.60 | asserted 1.00 |
| s5 | The column density of CH$_{3}$NH$_{2}$ towards the G358.93$-$0.03 MM1 was estimated to be (1.10$\pm$0.31)$\times$10$^{17}$ cm$^{-2}$ with an excitation temperature of 180.8$\pm$25.5 K. | result 1.00 | 0.96 | 0.14 | asserted 1.00 |
| s6 | The fractional abundance of CH$_{3}$NH$_{2}$ with respect to H$_{2}$ towards the G358.93$-$0.03 MM1 was (8.80$\pm$2.60)$\times$10$^{-8}$. | result 1.00 | 0.95 | 0.09 | asserted 1.00 |
| s7 | The column density ratio of CH$_{3}$NH$_{2}$ and NH$_{2}$CN towards G358.93$-$0.03 MM1 was (1.86$\pm$0.95)$\times$10$^{2}$. | result 1.00 | 0.93 | 0.07 | asserted 1.00 |
| s8 | The estimated fractional abundance of CH$_{3}$NH$_{2}$ towards the G358.93$-$0.03 MM1 agrees fairly well with the previous three-phase warm-up chemical modelling abundance of CH$_{3}$NH$_{2}$. | interpretation 0.63 | 0.84 | 0.10 | hedged possibility 0.55 |
| s9 | We also discussed the possible formation mechanism of CH$_{3}$NH$_{2}$, and we find that CH$_{3}$NH$_{2}$ is most probably formed via the reactions of radical CH$_{3}$ and radical NH$_{2}$ on the grain surface of G358.93$-$0.03 MM1. | interpretation 0.97 | 0.95 | 0.26 | hedged possibility 0.84 |
What was examined, and what was not
- arXiv listing abstract v1
- full text
- figures and tables
- references and citing sentences
- relations to other papers
- P abstract
- S sections
- T body sentences
- C citations
- R cross-paper relations
The paper
Original abstract
The search for the simplest amino acid, glycine (NH$_{2}$CH$_{2}$COOH), in the interstellar medium (ISM), has become a never-ending story for astrochemistry and astrophysics researchers because that molecule plays a possible connection between the Universe and the origin of life. In the last forty years, all searches for NH$_{2}$CH$_{2}$COOH in the ISM at millimeter and submillimeter wavelengths have failed. Since the detection of NH$_{2}$CH$_{2}$COOH in the ISM was extremely difficult, we aimed to search for the possible precursors of NH$_{2}$CH$_{2}$COOH. Earlier, many laboratory experiments have suggested that methylamine (CH$_{3}$NH$_{2}$) plays an important role in the ISM as a possible precursor of NH$_{2}$CH$_{2}$COOH. After spectral analysis using the local thermodynamic equilibrium (LTE) model, we identified the rotational emission lines of CH$_{3}$NH$_{2}$ towards the hot molecular core G358.93$-$0.03 MM1 using the Atacama Large Millimeter/Submillimeter Array (ALMA). The column density of CH$_{3}$NH$_{2}$ towards the G358.93$-$0.03 MM1 was estimated to be (1.10$\pm$0.31)$\times$10$^{17}$ cm$^{-2}$ with an excitation temperature of 180.8$\pm$25.5 K. The fractional abundance of CH$_{3}$NH$_{2}$ with respect to H$_{2}$ towards the G358.93$-$0.03 MM1 was (8.80$\pm$2.60)$\times$10$^{-8}$. The column density ratio of CH$_{3}$NH$_{2}$ and NH$_{2}$CN towards G358.93$-$0.03 MM1 was (1.86$\pm$0.95)$\times$10$^{2}$. The estimated fractional abundance of CH$_{3}$NH$_{2}$ towards the G358.93$-$0.03 MM1 agrees fairly well with the previous three-phase warm-up chemical modelling abundance of CH$_{3}$NH$_{2}$. We also discussed the possible formation mechanism of CH$_{3}$NH$_{2}$, and we find that CH$_{3}$NH$_{2}$ is most probably formed via the reactions of radical CH$_{3}$ and radical NH$_{2}$ on the grain surface of G358.93$-$0.03 MM1.
Human review
How the literature uses it
What this paper does with the arXiv papers it cites
What it cites · 1 sentence without a confident label
Cites as background 1 paper
-
The initial chemical development leading to the formation of life is believed to have formed in molecular clouds, proceeded inside the protoplanetary disk, and transported into the planetary atmosphere with the help of comets and asteroids [ref] .
Survey Observation of CH$_3$NH$_2$ and Its Formation Process · Introduction · 0.98
Discussion
Know something about this paper? Leave a comment, or highlight any passage above to comment on it.