Astonomical and laboratory detection of the SiC radical

Cernicharo, J.; Gottlieb, C. A.; Guèlin, M.; Thaddeus, P.; Vrtilek, J. M.

doi:10.1086/185449

Cited by 278 publications

(199 citation statements)

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“…We 1 01 estimate that a maximum error of ‫50.0ע‬ in (H 2 18 O) results t from uncertainties in the continuum level. The ortho-H 2 18 O column densities that we obtained are in acceptable agreement with results derived previously by Cernicharo et al (1997) from ISO observations of the 2 12 -1 01 line of ortho-H 2 18 O obtained at much lower spectral resolution.…”

Section: Water At Lsr Velocities In Thesupporting

confidence: 92%

“…In addition, observations from the Kuiper Airborne Observatory (KAO) have permitted the detection of foreground absorption by the species CH (Stacey, Lugten, & Genzel 1987) and H 2 18 O (Zmuidzinas et al 1995) that are inaccessible from the ground. Furthermore, recent Infrared Space Observatory (ISO) observations toward Sgr B2 have led to the detection of foreground atomic oxygen (Baluteau et al 1997) and H 2 16 O (Cernicharo et al 1997) absorption at far-infrared wavelengths.…”

Section: Introductionmentioning

confidence: 99%

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Observations of Absorption by Water Vapor toward Sagittarius B2

Neufeld

Ashby

Bergin

et al. 2000

The Astrophysical Journal

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We have observed the 1 10 -1 01 pure rotational transitions of both H 2 16 O and H 2 18 O toward Sagittarius B2 using the Submillimeter Wave Astronomy Satellite. The spectra thereby obtained show a complex pattern of absorption and-in the case of H 2 16 O-emission, with numerous features covering a wide range of LSR velocities (Ϫ130 to 130 km s Ϫ1 ) and representing absorption both in gas associated with Sgr B2 as well as by several components of foreground gas along the line of sight. The ortho-water abundance derived for the absorbing foreground gas is ∼ relative to H 2 . Ϫ76 # 10

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Section: Water At Lsr Velocities In Thesupporting

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Observations of Absorption by Water Vapor toward Sagittarius B2

Neufeld

Ashby

Bergin

et al. 2000

The Astrophysical Journal

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“…-Millar (1980) predicted SiC to be an abundant form of silicon in dense clouds on the basis of gas-phase chemistry models. This molecule was detected by Cernicharo et al (1989) towards the envelope of the red giant star IRC+101216, but not in Orion (see Schilke et al 1997 for the attempts of detection in this source). We obtained an upper limit for its total column density of 1.3 × 10 14 cm −2 providing an abundance ratio of N(SiO)/N(SiC) > ∼ 57.…”

Section: Other Silicon-bearing Moleculesmentioning

confidence: 99%

“…(1) Langhoff & Bauschlicher (1990); (2) Cernicharo et al (1989) and Bogey et al (1990); (3) Suenram et al (1989); (4) Gottlieb et al (1989) and Suenram et al (1989); (5) Alberts et al (1990); (6) Apponi et al (1999b); (7) Gordon et al (2000); (8) Ohishi et al (1989) and Gordon et al (2000); (9) Kerkines & Mavridis (2005); (10) Saito et al (1983) and Bizzocchi et al (2006); (11) Apponi et al (2000); (12) Apponi et al (2000) and McCarthy et al (2001); (13) McCarthy et al (1999); (14) McCarthy et al (2000); (15) Vasiliev et al (1997); (16) McCarthy & Thaddeus (2003a); (17) Botschwina (2005); (18) Sanz et al (2005); (19) Botschwina et al (2002); (20) Gabriel (1993); …”

Section: Other Silicon-bearing Moleculesmentioning

confidence: 99%

A line-confusion limited millimeter survey of Orion KL

Tercero

Vincent

Cernicharo

et al. 2011

A&A

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Aims. We present a study of the silicon-bearing species detected in a line-confusion limited survey towards Orion KL performed with the IRAM 30-m telescope. The analysis of the line survey is organized by families of molecules. Our aim is to derive physical and chemical conditions for each family taking all observed lines into account from all isotopologs of each species. The large number of transitions in different vibrationally excited states covered by our data, which range from 80 to 280 GHz, let us provide reliable source-average column densities (hence, isotopolog abundances and vibrational temperatures) for the detected molecules. In addition, we provide a wide study of the physical properties of the source based on the different spectral components found in the emission lines. Methods. We modeled the lines of the detected molecules using a radiative transfer code, which permit us to choose between large velocity gradient (LVG) and local thermodynamic equilibrium (LTE) approximations depending on the physical conditions of the gas. We used appropriate collisional rates for the LVG calculations. To qualitatively investigate the origin of the SiS and SiO emissions in Orion KL we ran a grid of chemical models.Results. For the v = 1 state of SiO, we detected the J = 2−1 line and, for the first time in this source, emission in the J = 4−3 transition, both of them showing a strong masering effect. For SiO v = 0, we detected 28 SiO, 29 SiO, and 30 SiO; in addition, we have mapped the J = 5−4 SiO line. For SiS, we have detected the main species, 29 SiS, and SiS v = 1. Unlikely other species detected in Orion KL (IRc2), the emission peak of SiS appears at a velocity of 15.5 km s −1 . A study of the 5−4 SiO line around IRc2 shows this feature as an extended component that probably arises from the interaction of the outflow with the ambient cloud. We derive an SiO/SiS column density ratio of 13 in the plateau component, four times lower than the cosmic O/S ratio 48. In addition, we provide upper limits to the column density of several non-detected silicon-bearing species. The results of our chemical models show that while it is possible to reproduce SiO in the gas phase (as well as on the grains), SiS is a product of surface reactions, most likely involving direct reactions of sulfur with silicon.

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“…Prior to this, lines of gaseous SiC in the 3 Π ground electronic state were observed in the 157-283 GHz range with single antennas [8,9,10], at low angular resolution of typically 10 −30 . Figure 1 shows the SiC spectrum and map of the 315 GHz line observed with the SMA at 3 resolution.…”

Section: Silicon Carbide and Silicon Nitride In Irc+10216mentioning

confidence: 99%

Probing the dust formation zone in IRC+10216 with the SMA

Patel¹

2014

Proceedings of the Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments — PoS(LCDU2013)

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Submillimeter imaging of high-excitation molecular rotational lines provides a powerful probe of the dust formation and acceleration region (R ≤ 5 × 10 16 cm) in the extreme carbon-rich star IRC+10216. We present Submillimeter Array (SMA) observations of several rotational lines of SiCC from our 345 and 400 GHz spectral-line surveys, showing a progression from rectangular to narrow triangular line-profiles, and spatially extended to point-like unresolved emission, as a function of increasing energy E u . Maps of SiC and SiN emission show asymmetrical extended shell-like structures. These results are compared with published chemical model calculations of the radial abundances of molecules believed to be relevant for dust formation.

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Astonomical and laboratory detection of the SiC radical

Cited by 278 publications

References 0 publications

Observations of Absorption by Water Vapor toward Sagittarius B2

Observations of Absorption by Water Vapor toward Sagittarius B2

A line-confusion limited millimeter survey of Orion KL

Probing the dust formation zone in IRC+10216 with the SMA

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