Search for methylamine in high mass hot cores

Ligterink, N. F. W.; Tenenbaum, E. D.; Dishoeck, E. F. van

doi:10.1051/0004-6361/201424845

Cited by 17 publications

(17 citation statements)

References 39 publications

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“…Previously, Di Francesco et al (2001) reported a similar kind of inverse P-Cygni profile and found that H 2 CO traces infall in IRAS 4A and they also detected the outflow from both 4A and 4B position by observing bright wing emission of H 2 CO. Formaldehyde, along with its deuterated counterpart, has also been observed in outflows toward other sources (e.g., Sahu et al 2018). The presence of H 2 CS in G31 has previously been reported by Ligterink et al (2015).…”

Section: Formaldehyde H2cosupporting

confidence: 54%

Identification of Methyl Isocyanate and Other Complex Organic Molecules in a Hot Molecular Core, G31.41+0.31

Gorai,

Das,

Shimonishi

et al. 2020

Preprint

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G31.41+0.31 is a well known chemically rich hot molecular core (HMC). Using Band 3 observations of Atacama Large Millimeter Array (ALMA), we have analyzed the chemical and physical properties of the source. We have identified methyl isocyanate (CH 3 NCO), a precursor of prebiotic molecules, towards the source. In addition to this, we have reported complex organic molecules (COMs) like methanol (CH 3 OH), methanethiol (CH 3 SH), and methyl formate (CH 3 OCHO). Additionally, we have used transitions from molecules like HCN, HCO + , SiO to trace the presence of infall and outflow signatures around the star-forming region. For the COMs, we have estimated the column densities and kinetic temperatures, assuming molecular excitation under local thermodynamic equilibrium (LTE) conditions. From the estimated kinetic temperatures of certain COMs, we found that multiple temperature components may be present in the HMC environment. Comparing the obtained molecular column densities between the existing observational results toward other HMCs, it seems that the COMs are favourably produced in the hot-core environment (∼ 100 K or higher). Though the spectral emissions towards G31.41+0.31 are not fully resolved, we find that CH 3 NCO and other COMs are possibly formed on grain/ice phase and populate the gas environment similar to other hot cores like Sgr B2, Orion KL, and G10.47+0.03, etc.

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Section: Formaldehyde H2cosupporting

confidence: 54%

Identification of Methyl Isocyanate and Other Complex Organic Molecules in a Hot Molecular Core, G31.41+0.31

Gorai,

Das,

Shimonishi

et al. 2020

Preprint

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“…A tentative detection was done in Orion Kl by Pagani et al 194 . Non-detections led to upper limit in a number of highmass young stellar objects (YSOs) 195 or in the low-mass Sun-like protostar IRAS 16293-2422B where the abundance of methylamine was determined to be two orders of magnitude lower than in Sgr B2 196 .…”

Section: An Important Prebiotic Speciesmentioning

confidence: 99%

Spectroscopy of Interstellar Internal Rotors: An Important Tool for Investigating Interstellar Chemistry

Kleiner

2019

ACS Earth Space Chem.

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This paper is a review of molecules with internal rotors detected or tentatively detected with upper limits in the interstellar medium. Internal rotor molecules containing one or two methyl groups are present at each of the different phases leading to stellar and planetary formation, from the molecular clouds to the star and its planets. They are also found in comets and asteroids. They represent a ubiquitous hydrogen-rich substituent in many complex organic molecules. This paper shows how high resolution spectra (mainly in the microwave, millimeter and sub-millimeter wave range) are analyzed in the laboratory and what theoretical methods can be used to properly reproduce the spectra. We also present a range of examples of important methyl rotors studied and how they can be used as tools to study the chemistry of interstellar medium.

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“…There are significant non-detections in some regions: for example, species such as methylamine, CH3NH2, and hydroxylamine, NH2OH, have been sought due to their potential roles as precursors for amino acids. However, so far only CH3NH2 has been detected in the ISM and only toward a few select regions such as Sgr B2(N) (Kaifu et al 1974), Orion KL (Pagani et al 2017), G10.47+0.03 (Ohishi et al 2019), and NGC 6334 (Bøgelund et al 2019b), but not in general toward high-mass star forming regions or low-mass protostars (Ligterink, Tenenbaum & van Dishoeck 2015;Ligterink et al 2018a). No secure detection of NH2OH has been reported so far despite dedicated searches toward high- (Pulliam, McGuire & Remijan 2012) and low-mass star forming regions (McGuire et al 2015;Ligterink et al 2018a).…”

Section: Detections In the Warm Gas Of Hot Cores And Corinosmentioning

confidence: 99%

Astrochemistry During the Formation of Stars

Jorgensen,

Belloche,

Garrod

2020

Preprint

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Star-forming regions show a rich and varied chemistry, including the presence of complex organic molecules -both in the cold gas distributed on large scales, and in the hot regions close to young stars where protoplanetary disks arise. Recent advances in observational techniques have opened new possibilities for studying this chemistry. In particular, the Atacama Large Millimeter/submillimeter Array (ALMA) has made it possible to study astrochemistry down to Solar System size scales, while also revealing molecules of increasing variety and complexity. In this review, we discuss recent observations of the chemistry of star-forming environments, with a particular focus on complex organic molecules, taking context from the laboratory experiments and chemical models that they have stimulated. The key takeaway points are:• The physical evolution of individual sources plays a crucial role in their inferred chemical signatures, and remains an important area for observations and models to elucidate. • Comparisons of the abundances measured toward different starforming environments (high-mass versus low-mass, Galactic center versus Galactic disk) reveal a remarkable similarity, an indication that the underlying chemistry is relatively independent of variations in their physical conditions. • Studies of molecular isotopologs in star-forming regions provide a link with measurements in our own Solar System, and thus may shed light on the chemical similarities and differences expected in other planetary systems.

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Search for methylamine in high mass hot cores

Cited by 17 publications

References 39 publications

Identification of Methyl Isocyanate and Other Complex Organic Molecules in a Hot Molecular Core, G31.41+0.31

Identification of Methyl Isocyanate and Other Complex Organic Molecules in a Hot Molecular Core, G31.41+0.31

Spectroscopy of Interstellar Internal Rotors: An Important Tool for Investigating Interstellar Chemistry

Astrochemistry During the Formation of Stars

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