THE SPITZER ICE LEGACY: ICE EVOLUTION FROM CORES TO PROTOSTARS
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02139 (United States)
- IPAC, NASA Herschel Science Center, California Institute of Technology, Pasadena, CA 91125 (United States)
- Space Telescope Science Institute, Baltimore, MD 21218 (United States)
- Leiden Observatory, Leiden University, 2300 RA Leiden (Netherlands)
- Centre d'Etude Spatiale des Rayonnements (CESR), CNRS-UMR 5187, 31028 Toulouse Cedex 4 (France)
- California Institute of Technology, Division of Geological and Planetary Sciences, Pasadena, CA 91125 (United States)
- Department of Astronomy, University of Texas at Austin, Austin, TX 78712 (United States)
Ices regulate much of the chemistry during star formation and account for up to 80% of the available oxygen and carbon. In this paper, we use the Spitzer c2d Legacy ice survey, complimented with data sets on ices in cloud cores and high-mass protostars, to determine standard ice abundances and to present a coherent picture of the evolution of ices during low- and high-mass star formation. The median ice composition H{sub 2}O:CO:CO{sub 2}:CH{sub 3}OH:NH{sub 3}:CH{sub 4}:XCN is 100:29:29:3:5:5:0.3 and 100:13:13:4:5:2:0.6 toward low- and high-mass protostars, respectively, and 100:31:38:4:-:-:- in cloud cores. In the low-mass sample, the ice abundances with respect to H{sub 2}O of CH{sub 4}, NH{sub 3}, and the component of CO{sub 2} mixed with H{sub 2}O typically vary by <25%, indicative of co-formation with H{sub 2}O. In contrast, some CO and CO{sub 2} ice components, XCN, and CH{sub 3}OH vary by factors 2-10 between the lower and upper quartile. The XCN band correlates with CO, consistent with its OCN{sup -} identification. The origin(s) of the different levels of ice abundance variations are constrained by comparing ice inventories toward different types of protostars and background stars, through ice mapping, analysis of cloud-to-cloud variations, and ice (anti-)correlations. Based on the analysis, the first ice formation phase is driven by hydrogenation of atoms, which results in an H{sub 2}O-dominated ice. At later prestellar times, CO freezes out and variations in CO freezeout levels and the subsequent CO-based chemistry can explain most of the observed ice abundance variations. The last important ice evolution stage is thermal and UV processing around protostars, resulting in CO desorption, ice segregation, and the formation of complex organic molecules. The distribution of cometary ice abundances is consistent with the idea that most cometary ices have a protostellar origin.
- OSTI ID:
- 21587338
- Journal Information:
- Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 740; ISSN ASJOAB; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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