An Inventory of Interstellar Ices toward the Embedded Protostar W33A

Gibb, E. L.; Whittet, D. C. B.; Schütte, W. A.; Boogert, A. C. A.; Chiar, J. E.; Ehrenfreund, P.; Gerakines, P. A.; Keane, J. V.; Tielens, A. G. G. M.; Dishoeck, E. F. van; Kerkhof, O.

doi:10.1086/308940

Cited by 396 publications

(474 citation statements)

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“…The observed composition of interstellar ice mantles demonstrates the dominance of this type of reaction (Gibb et al 2000).…”

Section: Solid Phase Processesmentioning

confidence: 72%

The chemistry of high-mass star formation

Tak¹,

Floris²

2005

Proc. IAU

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Abstract. This paper reviews the chemistry of star-forming regions, with an emphasis on the formation of high-mass stars. We first outline the basic molecular processes in dense clouds, their implementation in chemical models, and techniques to measure molecular abundances. Then, recent observational, theoretical and laboratory developments are reviewed on the subjects of hot molecular cores, cosmic-ray ionization, depletion and deuteration, and oxygen chemistry. The paper concludes with a summary of outstanding problems and future opportunities.

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“…The observed composition of interstellar ice mantles demonstrates the dominance of this type of reaction (Gibb et al 2000).…”

Section: Solid Phase Processesmentioning

confidence: 72%

The chemistry of high-mass star formation

Tak¹,

Floris²

2005

Proc. IAU

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“…2,3 Observed infrared (IR) spectra reveal that H 2 O and CO are the most abundant molecules in the icy mantles in the ISM. [2][3][4][5][6][7][8][9][10] Recent ground and space based observations have also detected heavy water (D 2 O) in the ISM. 11,12 a) Author to whom correspondence should be addressed.…”

Section: Introductionmentioning

confidence: 99%

Molecular dynamics simulations of D2O ice photodesorption

Arasa

Andersson

Cuppen

et al. 2011

The Journal of Chemical Physics

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(2010)]. The main conclusions are the same, but the average D atom photodesorption probability is smaller than that of the H atom (by about a factor of 0.9) because D has lower kinetic energy than H, whereas the average OD radical photodesorption probability is larger than that of OH (by about a factor of 2.5-2.9 depending on ice temperature) because OD has higher translational energy than OH for every ice temperature studied. The average D 2 O photodesorption probability is larger than that of H 2 O (by about a factor of 1.4-2.3 depending on ice temperature), and this is entirely due to a larger contribution of the D 2 O kick-out mechanism. This is an isotope effect: the kick-out mechanism is more efficient for D 2 O ice, because the D atom formed after D 2 O photodissociation has a larger momentum than photogenerated H atoms from H 2 O, and D transfers momentum more easily to D 2 O than H to H 2 O. The total (OD + D 2 O) yield has been compared with experiments and the total (OH + H 2 O) yield from previous simulations. We find better agreement when we compare experimental yields with calculated yields for D 2 O ice than when we compare with calculated yields for H 2 O ice.

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“…Some ice bands, such as CO and CO 2 , cannot be fitted by a single laboratory ice mixture, but seem to trace molecules in two or more ice phases, often referred to as polar Gibb et al (2000), and Boogert et al (2008). The 3 µm portions of the spectra have been binned to increase the S/N.…”

Section: Ice Identificationsmentioning

confidence: 99%

Ices in Starless and Starforming Cores

et al. 2011

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Abstract. Icy grain mantles are commonly observed through infrared spectroscopy toward dense clouds, cloud cores, protostellar envelopes and protoplanetary disks. Up to 80% of the available oxygen, carbon and nitrogen are found in such ices; the most common ice constituents -H 2 O, CO2 and CO -are second in abundance only to H2 in many star forming regions. In addition to being a molecular reservoir, ice chemistry is responsible for much of the chemical evolution from H2 O to complex, prebiotic molecules. Combining the exisiting ISO, Spitzer, VLT and Keck ice data results in a large sample of ice sources (∼80) that span all stages of star formation and a large range of protostellar luminosities (<0.1-10 5 L ). Here we summarize the different techniques that have been applied to mine this ice data set on information on typical ice compositions in different environments and what this implies about how ices form and evolve during star and planet formation. The focus is on how to maximize the use of empirical constraints from ice observations, followed by the application of information from experiments and models. This strategy is used to identify ice bands and to constrain which ices form early during cloud formation, which form later in the prestellar core and which require protostellar heat and/or UV radiation to form. The utility of statistical tests, survival analysis and ice maps is highlighted; the latter directly reveals that the prestellar ice formation takes place in two phases, associated with H 2 O and CO ice formation, respectively, and that most protostellar ice variation can be explained by differences in the prestellar CO ice formation stage. Finally, special attention is paid to the difficulty of observing complex ices directly and how gas observations, experiments and models help in constraining this ice chemistry stage.

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An Inventory of Interstellar Ices toward the Embedded Protostar W33A

Cited by 396 publications

References 44 publications

The chemistry of high-mass star formation

The chemistry of high-mass star formation

Molecular dynamics simulations of D2O ice photodesorption

Ices in Starless and Starforming Cores

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