Detection of Interstellar Methylamine by its 2_{02}-&gt;1_{10} A_{a^{-}} State Transition

Fourikis, N.; Takagi, Kojiro; Morimoto, Manabu

doi:10.1086/181570

Cited by 76 publications

(58 citation statements)

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“…Methylamine was detected early on towards Sgr B2 (Kaifu et al 1974;Fourikis et al 1974). The same papers report its detection in Orion, but Johansson et al (1984) proved these detections to be incorrect 5 .…”

Section: Methylamine Ch 3 Nhmentioning

confidence: 98%

The complexity of Orion: an ALMA view

Pagani

Favre

Goldsmith

et al. 2017

A&A

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Context. We wish to improve our understanding of the Orion central star formation region (Orion-KL) and disentangle its complexity. Aims. We collected data with ALMA during cycle 2 in 16 GHz of total bandwidth spread between 215.1 and 252.0 GHz with a typical sensitivity of 5 mJy/beam (2.3 mJy/beam from 233.4 to 234.4 GHz) and a typical beam size of 1 . 7 × 1 . 0 (average position angle of 89 • ). We produced a continuum map and studied the emission lines in nine remarkable infrared spots in the region including the hot core and the compact ridge, plus the recently discovered ethylene glycol peak. Methods. We present the data, and report the detection of several species not previously seen in Orion, including n-and i-propyl cyanide (C 3 H 7 CN), and the tentative detection of a number of other species including glycolaldehyde (CH 2 (OH)CHO). The first detections of gGg ethylene glycol (gGg (CH 2 OH) 2 ) and of acetic acid (CH 3 COOH) in Orion are presented in a companion paper. We also report the possible detection of several vibrationally excited states of cyanoacetylene (HC 3 N), and of its 13 C isotopologues. We were not able to detect the 16 O 18 O line predicted by our detection of O 2 with Herschel, due to blending with a nearby line of vibrationally excited ethyl cyanide. We do not confirm the tentative detection of hexatriynyl (C 6 H) and cyanohexatriyne (HC 7 N) reported previously, or of hydrogen peroxide (H 2 O 2 ) emission. Results. We report a complex velocity structure only partially revealed before. Components as extreme as −7 and +19 km s −1 are detected inside the hot region. Thanks to different opacities of various velocity components, in some cases we can position these components along the line of sight. We propose that the systematically redshifted and blueshifted wings of several species observed in the northern part of the region are linked to the explosion that occurred ∼500 yr ago. The compact ridge, noticeably farther south displays extremely narrow lines (∼1 km s −1 ) revealing a quiescent region that has not been affected by this explosion. This probably indicates that the compact ridge is either over 10 000 au in front of or behind the rest of the region. Conclusions. Many lines remain unidentified, and only a detailed modeling of all known species, including vibrational states of isotopologues combined with the detailed spatial analysis offered by ALMA enriched with zero-spacing data, will allow new species to be detected.

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Section: Methylamine Ch 3 Nhmentioning

confidence: 98%

The complexity of Orion: an ALMA view

Pagani

Favre

Goldsmith

et al. 2017

A&A

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“…Its formation in ice seems to be well understood and is explained by direct hydrogenation of CO on the grain surface (Hiraoka et al 1994(Hiraoka et al , 2002Watanabe et al 2004). Methylamine CH 3 NH 2 is the simplest member of the primary alkylamine family and has been detected in gas phase by its 2 02 → 1 10 A a state transition in the direction of Sgr B2 and Ori A (Fourikis et al 1974). In addition, results from the stardust mission support its presence in cometary cores (Elsila et al 2009).…”

Section: Introductionmentioning

confidence: 99%

Formaldehyde and methylamine reactivity in interstellar ice analogues as a source of molecular complexity at low temperature

Vinogradoff

Duvernay

Danger

et al. 2012

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Aims. The aim of this work is to consolidate the knowledge of ice evolution during the star formation process by investigating the influence of thermal reactions as a source of molecular complexity in the ISM. In this study, we are interested in the thermal reactivity between two interstellar molecules, formaldehyde (H 2 CO) and methylamine (CH 3 NH 2 ) in water ice analogues. Methods. We used Fourier transform infrared spectroscopy, mass spectrometry, and B3LYP calculations to investigate the thermal reaction between formaldehyde and methylamine ( 14 N and 15 N) at low temperature in water ice analogues. Results. We demonstrate that methylamine and formaldehyde quickly react in water ice analogues for astronomically relevant temperatures and form N-methylaminomethanol CH 3 NHCH 2 OH. The measured activation energy of this reaction, 1.1 ± 0.05 kJ mol −1 (1.8 ± 0.08 kJ mol −1 with methylamine 15 N), allows the reaction to proceed in interstellar ices, when the ices are gently warmed, as it occurs in young stellar objects, in photo-dissociation regions, or in comets. Therefore, CH 3 NHCH 2 OH is likely to be found in these objects. This hypothesis is confirmed by numerical simulations that clearly show that the formation of N-methylaminomethanol is likely at low temperature. Isotopic experiments as well as photochemical studies have also been performed to better characterise the ice evolution induced by heat and ultraviolet radiation during star formation.

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“…Methylamine is an astrophysical important molecule, which has been detected by millimeter wave observations of the Sagittarius B2 and Orion A molecular clouds (Kaifu et al 1974;Fourikis et al 1974). Methylamine can be produced inside icy grains from the vacuum ultraviolet photolysis of other relatively abundant molecules, i.e., methane (CH 4 ) and ammonia (NH 3 ) (Garder & McNesby 1980;Ogura et al 1988), or methylium ion (CH + 3 ) and ammonia (NH 3 ) (Herbst 1985), or from a hydrogenation series based on the cyanide radical (CN), hydrogen cyanide (HCN), and methanimine (H 2 C = NH) (Godfrey et al 1973).…”

Section: Introductionmentioning

confidence: 99%

Methylammonium methylcarbamate thermal formation in interstellar ice analogs: a glycine salt precursor in protostellar environments

Bossa¹,

Duvernay²,

Theulé³

et al. 2009

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Context. Analyses of dust cometary grains collected by the Stardust spacecraft have shown the presence of amines and amino acids molecules, and among them glycine (NH 2 CH 2 COOH). We show how the glycine molecule could be produced in the protostellar environments before its introduction into comets. Aims. We study the evolution of the interstellar ice analogues affected by both thermal heating and vacuum ultraviolet (VUV) photons, in addition to the nature of the formed molecules and the confrontation of our experimental results with astronomical observations. Methods. Infrared spectroscopy and mass spectrometry are used to monitor the evolution of the H 2 O:CO 2 :CH 3 NH 2 and CO 2 :CH 3 NH 2 ice mixtures during both warming processes and VUV photolysis. Results. We first show how carbon dioxide (CO 2 ) and methylamine (CH 3 NH 2 ) thermally react in water-dominated ice to form methylammonium methylcarbamate [CH 3 NH + 3 ][CH 3 NHCOO − ] noted C. We then determine the reaction rate and activation energy. We show that C thermal formation can occurs in the 50-70 K temperature range of a protostellar environment. Secondly, we report that a VUV photolysis of a pure C sample produces a glycine salt, methylammonium glycinate [CH 3 NH + 3 ][NH 2 CH 2 COO − ] noted G. We propose a scenario explaining how C and subsequently G can be synthesized in interstellar ices and precometary grains. Conclusions. [CH 3 NH + 3 ][CH 3 NHCOO − ] could be readily formed and would act as a glycine salt precursor in protostellar environments dominated by thermal and UV processing. We propose a new pathway leading to a glycine salt, which is consistent with the detection of glycine and methylamine within the returned samples of comet 81P/Wild 2 from the Stardust mission.

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Detection of Interstellar Methylamine by its 2_{02}->1_{10} A_{a^{-}} State Transition

Cited by 76 publications

References 0 publications

The complexity of Orion: an ALMA view

The complexity of Orion: an ALMA view

Formaldehyde and methylamine reactivity in interstellar ice analogues as a source of molecular complexity at low temperature

Methylammonium methylcarbamate thermal formation in interstellar ice analogs: a glycine salt precursor in protostellar environments

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