Observation of interstellar ammonia ice

Knacke, R. F.; McCorkle, S.; Puetter, R. C.; Erickson, E. F.; Kraetschmer, W.

doi:10.1086/160241

Cited by 75 publications

(46 citation statements)

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“…Using a mixing ratio of 6.7 × 10 −6 (Sada et al, 2005), we find that C 2 H 6 condenses out of the atmosphere at 10 mbar. (Geballe et al, 1988) and a laboratory spectrum of NH 3 ice particles (Knacke et al, 1982). The approximate match between the albedo feature at 2.96 µm and the NH 3 ice particle spectrum suggests the possibility of NH 3 ice particles in the saturnian clouds.…”

Section: Observations Data Reduction and Model Constructionmentioning

confidence: 77%

High-resolution spectroscopy of Saturn at 3 microns: CH4, CH3D, C2H2, C2H6, PH3, clouds, and haze

Kim

Geballe

et al. 2006

Icarus

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Section: Observations Data Reduction and Model Constructionmentioning

confidence: 77%

High-resolution spectroscopy of Saturn at 3 microns: CH4, CH3D, C2H2, C2H6, PH3, clouds, and haze

Kim

Geballe

et al. 2006

Icarus

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“…Earlier detections in a number of sources (Hagen et al 1980, Knacke et al 1982 could not be confirmed by later observations (Knacke & McCorkle 1987;Smith et al 1989). A detection in HH 100-IRS by Graham & Chen (1991) could not be confirmed by Whittet et al (1996).…”

Section: Introductionmentioning

confidence: 80%

Detection of solid ammonia, methanol, and methane with ISOPHOT

Gürtler¹,

Klaas

Henning

et al. 2002

A&A

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Abstract. We report on a search for the NH 3 inversion band at 9.0 µm, the CH 4 band at 7.7 µm, and the CH 3 OH band at 9.7 µm in the spectra of 10 heavily obscured stellar objects taken with the spectrophotometer ISOPHOT-S aboard the Infrared Space Observatory (ISO). Four of them show indications of the NH 3 inversion band at 9.0 µm superimposed on the always strong silicate band. The results show that ammonia ice may be abundant in some cool and dense molecular circumstellar regions. The 9.7 µm band of solid CH 3 OH was detected in 5 of the sources, and also the 7.7 µm band of solid CH 4 was found in 5 sources. The PHT-S detections were cross-checked against ISO-SWS spectra from archive data. Considering the different beam sizes (24 × 24 versus 14 × 20 ), there is good agreement.

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“…NH 3 After N 2 , the most abundant nitrogen bearing molecule is certainly the ammonia one. Knacke et al (1982) were among the firsts to claim for an identification of NH 3 in interstellar grains from an infrared absorption at 2.97 µm (NH stretching mode), a detection refuted later on Knacke and McCorkle (1987). Hagen et al (1983) show that the H 2 O stretching mode profile is best reproduced with an ice containing a significant fraction of ammonia.…”

Section: Ch 3 Ohmentioning

confidence: 93%

The Ice Survey Opportunity of ISO

Dartois

2005

Space Sci Rev

120

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The instruments on board the Infrared Space Observatory have for the first time allowed a complete low (PHOT, CVF) to medium resolution (SWS) spectroscopic harvest, from 2.5 to 45 µm, of interstellar dust. Amongst the detected solids present in starless molecular clouds surrounding recently born stellar and still embedded objects or products of the chemistry in some mass loss envelopes, the so-called "ice mantles" are of specific interest. They represent an interface between the very refractory carbonaceous and silicates materials that built the first grains with the rich chemistry taking place in the gas phase. Molecules condense, react on ices, are subjected to UV and cosmic ray irradiation at low temperatures, participating efficiently to the evolution toward more complex molecules, being in constant interaction in an ice layer. They also play an important role in the radiative transfer of molecular clouds and strongly affect the gas phase chemistry. ISO results shed light on many other species than H 2 O ice. The detection of these van der Waal's solids is mainly performed in absorption. Each ice feature observed by ISO spectrometer is an important species, with abundance in the 10 −4 -10 −7 range with respect to H 2 . Such high abundances represent a substantial reservoir of matter that, once released later on, replenishes the gas phase and feeds the ladder of molecular complexity. Medium resolution spectroscopy also offers the opportunity to look at individual line profiles of the ice features, and therefore to progressively reveal the interactions taking place in the mantles.This article will give a view on selected results to avoid to overlap with the numerous reviews the reader is invited to consult (e.g. van Dishoeck, in press;Gibb et al., 2004.). Ices EverywhereInterstellar ices have been observed with ISO-SWS in many different lines of sight among which the most common are: r OH-IR (and by extension, evolved stars circumstellar shells) which are oxygen rich post main sequence stars loosing mass at a high rate. The dust and molecules formed in this mass loss ejecta feed a circumstellar shell, opaque to visible light and therefore re-emitting in the infrared. In these lines of sight, H 2 O is likely to be the only ice present on dust grains, generally in crystalline Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA.

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Observation of interstellar ammonia ice

Cited by 75 publications

References 0 publications

High-resolution spectroscopy of Saturn at 3 microns: CH4, CH3D, C2H2, C2H6, PH3, clouds, and haze

High-resolution spectroscopy of Saturn at 3 microns: CH4, CH3D, C2H2, C2H6, PH3, clouds, and haze

Detection of solid ammonia, methanol, and methane with ISOPHOT

The Ice Survey Opportunity of ISO

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