Detection of interstellar SiS and a study of the IRC +10216 molecular envelope.

Morris, M.; Gilmore, W.; Palmer, Patrick; Turner, B. E.; Zuckerman, B.

doi:10.1086/181846

Cited by 106 publications

(64 citation statements)

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“…Since the detection of HC 3 N in the interstellar (Turner 1971) and circumstellar medium (Morris et al 1975(Morris et al , 1976, the synthesis of complex hydrocarbons has been a basic topic in the study of the chemistry of organic molecular species in the dense and cold ISM clouds (Herbst & Leung 1989) and in the chemistry of the external layers of circumstellar envelopes Cherchneff, Glassgold, & Mamon 1993). In all these models, C 3 plays an important role in the growth of carbon chains.…”

Section: Discussionmentioning

confidence: 99%

“…Cyanopolyynes, HC N ( , 5), are abundant molecules in sources n = 1 2nϩ1 like TMC-1 and IRC ϩ10216 (Turner 1971;Morris et al 1975Morris et al , 1976Broten et al 1978;Bell et al 1982Bell et al , 1997. Long carbonchain radicals have been detected in the same sources through their pure rotational spectrum at radio wavelengths (C 5 H, C 6 H, C 7 H, C 8 H, H 2 C 3 , and H 2 C 4 ; Cernicharo et al 1986Cernicharo et al , 1987Guélin et al 1987;Cernicharo & Guélin 1996;Guélin et al 1997).…”

Section: Introductionmentioning

confidence: 99%

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Far-infrared Detection of C[TINF]3[/TINF] in Sagittarius B2 and IRC +10216

Cernicharo¹,

Goicoechea²,

Caux³

2000

The Astrophysical Journal

137

162

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We report on the detection of nine lines of the n 2 bending mode of triatomic carbon, C 3 , in the direction of Sagittarius B2. The R(4) and R(2) lines of C 3 have been also detected in the carbon-rich star IRC ϩ10216. The abundances of C 3 in the direction of Sgr B2 and IRC ϩ10216 are Ӎ and Ӎ10 Ϫ6 , respectively. In Ϫ83 # 10 Sgr B2 we have also detected the 2 3 -1 2 line of NH with an abundance of a few times 10 Ϫ9 . Polyatomic molecules will have a weak contribution from their pure rotational spectrum to the emission/absorption in the far-infrared. We suggest, however, that they could be, through their low-lying vibrational bending modes, the dominant carriers of emission/absorption in the spectrum of bright far-infrared sources.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Far-infrared Detection of C[TINF]3[/TINF] in Sagittarius B2 and IRC +10216

Cernicharo¹,

Goicoechea²,

Caux³

2000

The Astrophysical Journal

137

162

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“…SiS was first detected towards the carbon-rich star IRCþ10216 a few years after SiO was detected [13], but it has now been observed towards several oxygen-rich stars [12]. Its lines are so intense towards IRCþ10216 that SiS has now been observed in the three lowest vibrationally excited states of the main isotopic species, and in the ground vibrational state [14] of six rare isotopic species, including the doubly substituted species 29 Si 34 S and 30 Si 34 S. Millimetre-wave interferometric measurements in IRCþ 10216 show that SiS is localized near the central star rather than in the outer circumstellar shell [15].…”

Section: Sismentioning

confidence: 99%

Silicon molecules in space and in the laboratory

2003

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Despite the highly non-volatile nature of Si, silicon bearing molecules are a significant trace constituent of the gas associated with late-type stars and star forming regions, representing nearly 10% of the molecular species that have been identified in space. The early astronomical detection of SiO and its remarkable maser emission stimulated laboratory studies of other small silicon species that were crucial to the astronomical identifications. Although the pace of this laboratory work until recently has been slow, the application of Fourier transform microwave spectroscopy to supersonic molecular beams has overcome many experimental difficulties, yielding the detection of more than 20 new silicon chains and rings of astronomical interest during the past three years. Three of these, the rhomboidal ring SiC 3 and the isovalent linear molecules SiCN and SiNC, have now been found in space, and with dedicated searches other recently discovered silicon molecules may soon be found. A number of exotic silicon molecules of astronomical and chemical interest should be amenable to laboratory detection with present techniques.

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“…It is necessary to life as we know it, gives rise to novel chemistry in extreme environments like hot springs and black smokers on Earth, heavily influences the atmospheric chemistry of Venus (Krasnopolsky 2007(Krasnopolsky , 2012 as well as the surface chemistry of Io, and is present in various terrestrial pollutants (Tchir & Spratley 1975;Hawkins & Downs 1984). Consequently, sulfur cannot be neglected for astrochemical analysis, and an understanding for its importance in the chemistry of space has been continually growing since various molecular sulfur detections began in the 1970s (Morris et al 1975;Henkel et al 1983;Johansson et al 1984;Ziurys et al 1984;Cernicharo et al 1987Cernicharo et al , 2000Kaifu et al 1987;Saito et al 1987;Turner 1987Turner , 1992Kahane et al 1988;Martín-Pintado et al 1992;Boyle et al 1994;Turner et al 1998;Schilke et al 2001Schilke et al , 2003Mauersberger et al 2004;Sakai et al 2007;Finney et al 2016).…”

Section: Introductionmentioning

confidence: 99%

On the Detectability of the HSS, HSO, and HOS Radicals in the Interstellar Medium

Fortenberry

Francisco

2017

ApJ

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HSS has yet to be observed in the gas phase in the interstellar medium (ISM). HSS has been observed in cometary material and in high abundance. However, its agglomeration to such bodies or dispersal from them has not been observed. Similarly, HSO and HOS have not been observed in the ISM, either, even though models support their formation from reactions of known sulfur monoxide and hydrogen molecules, among other pathways. Consequently, this work provides high-level, quantum chemical rovibrational spectroscopic constants and vibrational frequencies in order to assist in interstellar searches for these radical molecules. Furthermore, the HSO −HOS isomerization energy is determined to be 3.63 kcal mol −1 , in line with previous work, and the dipole moment of HOS is 36% larger at 3.87 D than HSO, making the less stable isomer more rotationally intense. Finally, the S−S bond strength in HSS is shown to be relatively weak at 30% of the typical disulfide bond energy. Consequently, HSS may degrade into SH and sulfur atoms, making any ISM abundance of HSS likely fairly low, as recent interstellar surveys have observed.

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Detection of interstellar SiS and a study of the IRC +10216 molecular envelope.

Cited by 106 publications

References 0 publications

Far-infrared Detection of C[TINF]3[/TINF] in Sagittarius B2 and IRC +10216

Far-infrared Detection of C[TINF]3[/TINF] in Sagittarius B2 and IRC +10216

Silicon molecules in space and in the laboratory

On the Detectability of the HSS, HSO, and HOS Radicals in the Interstellar Medium

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