Probable detection of interstellar methylamine-D /CH3NHD/

Fourikis, N.; Takagi, Kojiro; Saito, Shuji

doi:10.1086/182369

Cited by 12 publications

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“…CH 3 NH 2 was first observed by Kaifu et al (1974Kaifu et al ( , 1975 toward Sgr B2(OH). Fourikis et al (1974) also detected this species in the southern region of Sgr B2 and Fourikis et al (1977) later found deuterated methyl amine (CH 3 NHD) at that position, as well. Later surveys conducted by Turner (1989) toward Sgr B2(OH) and Nummelin et al (1998) in Sgr B2(N) also found spectral lines of CH 3 NH 2 .…”

Section: Introductionmentioning

confidence: 83%

INSIGHTS INTO SURFACE HYDROGENATION IN THE INTERSTELLAR MEDIUM: OBSERVATIONS OF METHANIMINE AND METHYL AMINE IN Sgr B2(N)

Halfen

Ilyushin

Ziurys

2013

ApJ

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Multiple observations of methanimine (CH 2 NH) and methyl amine (CH 3 NH 2 ) have been performed toward Sgr B2(N) at 1, 2, and 3 mm using the Submillimeter Telescope and the 12 m antenna of the Arizona Radio Observatory. In the frequency range 68-280 GHz, 23 transitions of CH 2 NH and 170 lines of CH 3 NH 2 have been observed as individual, distinguishable features, although some are partially blended with other lines. For CH 2 NH, the line profiles indicate V LSR = 64.2 ± 1.4 km s −1 and ΔV 1/2 = 13.8 ± 2.8 km s −1 , while V LSR = 63.7 ± 1.6 km s −1 and ΔV 1/2 = 15.1 ± 3.0 km s −1 for CH 3 NH 2 , parameters that are very similar to those of other organic species in Sgr B2(N). From these data, rotational diagrams were constructed for both species. In the case of CH 2 NH, a rotational temperature of T rot = 44 ± 13 K and a column density of N tot = (9.1 ± 4.4) × 10 14 cm −2 were determined from the analysis. For CH 3 NH 2 , T rot = 159 ± 30 K and N tot = (5.0 ± 0.9) × 10 15 cm −2 , indicating that this species is present in much warmer gas than CH 2 NH. The fractional abundances for CH 2 NH and CH 3 NH 2 were established to be f (H 2 ) ≈ 3.0 × 10 −10 and f (H 2 ) ≈ 1.7 × 10 −9 , respectively. It has been proposed that CH 2 NH is formed on grains via hydrogenation of HCN; further hydrogenation of CH 2 NH on surfaces leads to CH 3 NH 2 . However, given the dissimilarity between the rotational temperatures and distributions of CH 2 NH and CH 3 NH 2 in Sgr B2, it is improbable that these species are closely related synthetically, at least in this source. Both CH 2 NH and CH 3 NH 2 are more likely created by neutral-neutral processes in the gas phase.

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Section: Introductionmentioning

confidence: 83%

INSIGHTS INTO SURFACE HYDROGENATION IN THE INTERSTELLAR MEDIUM: OBSERVATIONS OF METHANIMINE AND METHYL AMINE IN Sgr B2(N)

Halfen

Ilyushin

Ziurys

2013

ApJ

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“…Gasphase chemistry of the D enrichment of interstellar species has been studied extensively (e.g., Roberts and Miller 2000;Gerlich and Schlemmer 2002;Osamura et al 2005), and the importance of grain-surface reactions for D enrichment has recently become well understood through various experimental studies (Nagaoka et al 2005(Nagaoka et al , 2007Hidaka et al 2009;Oba et al 2012) and theoretical models (Stantcheva and Herbst 2003;Taquet et al 2012). Fourikis et al (1977) reported the probable detection of deuterated methylamine CH 3 NHD toward Sgr B2; however, it was later not detected in the same target by another group (MacLeod et al 1979). Although deuterated methylamine such as CH 2 DNH 2 and CH 3 NHD has never been detected in space, it should be reasonable to consider that interstellar methylamine is deuterated to some extent.…”

Section: Introductionmentioning

confidence: 99%

“…Fourikis et al. () reported the probable detection of deuterated methylamine CH 3 NHD toward Sgr B2; however, it was later not detected in the same target by another group (MacLeod et al. ).…”

Section: Introductionmentioning

confidence: 99%

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Hydrogen isotopic substitution of solid methylamine through atomic surface reactions at low temperatures: A potential contribution to the D/H ratio of methylamine in molecular clouds

Oba

Chigai

Osamura

et al. 2013

Meteorit & Planetary Scien

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Abstract-We experimentally studied hydrogen (H)-deuterium (D) substitution reactions of solid methylamine (CH 3 NH 2 ) under astrophysically relevant conditions. We also calculated the potential energy surface for the H-D substitution reactions of methylamine isotopologues using quantum chemical methods. Despite the relatively large energy barrier of more than 18 kJ mol À1 , CH 3 NH 2 reacted with D atoms to yield deuterated methylamines at 10 K, suggesting that the H-D substitution reaction proceeds through quantum tunneling. Deuterated methylamines reacted with H atoms as well. On the basis of present results, we propose that methylamine has potential for D enrichment through atomic surface reactions on interstellar grains at very low temperatures in molecular clouds. D enrichment would occur in particular in the methyl group of methylamine.

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“…Recently, methylamine has been detected in a spiral galaxy with a high redshift of 0.89, located in front of the quasar PKS 1830-211 (Muller et al 2011). Also Fourikis et al (1977) reported probable detection of deuterated methyl amine (CH 3 NHD) in the southern region of Sgr B2.…”

Section: Introductionmentioning

confidence: 97%

Millimeter and submillimeter wave spectra of¹³C methylamine

Motiyenko

Margulès

Ilyushin

et al. 2016

A&A

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Context. Methylamine (CH 3 NH 2 ) is a light molecule of astrophysical interest, which has an intensive rotational spectrum that extends in the submillimeter wave range and far beyond, even at temperatures characteristic for the interstellar medium. It is likely for 13 C isotopologue of methylamine to be identified in astronomical surveys, but there is no information available for the 13 CH 3 NH 2 millimeter and submillimeter wave spectra. Aims. In this context, to provide reliable predictions of 13 CH 3 NH 2 spectrum in millimeter and submillimeter wave ranges, we have studied rotational spectra of the 13 C methylamine isotopologue in the frequency range from 48 to 945 GHz. Methods. The spectrum of 13 C methylamine was recorded using conventional absorption spectrometers. The analysis of the rotational spectrum of 13 C methylamine in the ground vibrational state was performed on the basis of the group-theoretical high-barrier tunneling Hamiltonian that was developed for methylamine. The available multiple observations of the parent methylamine species toward Sgr B2(N) at 1, 2, and 3 mm using the Submillimeter Telescope and the 12 m antenna of the Arizona Radio Observatory were used to make a search for interstellar 13 CH 3 NH 2 .Results. In the recorded spectra, we have assigned 2721 rotational transitions that belong to the ground vibrational state of the 13 CH 3 NH 2 . These measurements were fitted to the Hamiltonian model that uses 75 parameters to achieve an overall weighted rms deviation of 0.73. On the basis of these spectroscopic results, predictions of transition frequencies in the frequency range up to 950 GHz with J ≤ 50 and K a ≤ 20 are presented. The search for interstellar 13 C methylamine in available observational data was not successful and therefore only an upper limit of 6.5 × 10 14 cm −2 can be derived for the column density of 13 CH 3 NH 2 toward Sgr B2(N), assuming the same source size, temperature, linewidth, and systemic velocity as for parent methylamine isotopic species.

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Probable detection of interstellar methylamine-D /CH3NHD/

Cited by 12 publications

References 0 publications

INSIGHTS INTO SURFACE HYDROGENATION IN THE INTERSTELLAR MEDIUM: OBSERVATIONS OF METHANIMINE AND METHYL AMINE IN Sgr B2(N)

INSIGHTS INTO SURFACE HYDROGENATION IN THE INTERSTELLAR MEDIUM: OBSERVATIONS OF METHANIMINE AND METHYL AMINE IN Sgr B2(N)

Hydrogen isotopic substitution of solid methylamine through atomic surface reactions at low temperatures: A potential contribution to the D/H ratio of methylamine in molecular clouds

Millimeter and submillimeter wave spectra of¹³C methylamine

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Probable detection of interstellar methylamine-D /CH3NHD/

Cited by 12 publications

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INSIGHTS INTO SURFACE HYDROGENATION IN THE INTERSTELLAR MEDIUM: OBSERVATIONS OF METHANIMINE AND METHYL AMINE IN Sgr B2(N)

INSIGHTS INTO SURFACE HYDROGENATION IN THE INTERSTELLAR MEDIUM: OBSERVATIONS OF METHANIMINE AND METHYL AMINE IN Sgr B2(N)

Hydrogen isotopic substitution of solid methylamine through atomic surface reactions at low temperatures: A potential contribution to the D/H ratio of methylamine in molecular clouds

Millimeter and submillimeter wave spectra of13C methylamine

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Millimeter and submillimeter wave spectra of¹³C methylamine