An Inventory of Interstellar Ices toward the Embedded Protostar W33A

By E. Gibb, D. Whittet, W. Schutte, A. Boogert, J. Chiar, P. Ehrenfreund, P. Gerakines, J. Keane, A. Tielens, E. V. van Dishoeck and 1 more. 2000

367 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/55c923e8b3adf1492cf9b1c7102da3166aabd996

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Citations in the corpus

WFCAM, Spitzer/IRAC and SCUBA observations of the massive star-forming region DR21/W75 - I. The collimated molecular jets (2006, background): “For targets with photometry in only two IRAC bands we do not derive values for α, since the 8.0µm magnitudes may be compromised by deep silicate absorption in these luminous, embedded sources (e.g Gibb et al. 2000).”
SPITZER SAGE SURVEY OF THE LARGE MAGELLANIC CLOUD. III. STAR FORMATION AND ∼1000 NEW CANDIDATE YOUNG STELLAR OBJECTS (2008, background): “…aromatic hydrocarbon (PAH) emission which can be important in sources with hot central stars, though the contribution is lower and often non-existent in more embedded sources (Gibb et al. 2000; Keane et al. 2001), which we are more sensitive due to our color–magnitude selections (Section 2.3.1).”
Non-thermal desorption from interstellar dust grains via exothermic surface reactions (2007, background): “Bergin et al. (2005);5 data collated by Gibb et al. (2000) One possible reason for the failure of our models is a lack of gas-phase carbon; Smith et al. (2004) tested increases inthe C”
Reaction Networks for Interstellar Chemical Modelling: Improvements and Challenges (2010, background): “…triggered by photon irradiation, particle bombardment or thermal processing, has been raised, both to understand the composition of icy mantles (Gibb et al. 2000) and to find an alternative to gas-phase processes, which can fail to reconcile model predictions with observations for some…”
Hot corinos in NGC 1333-IRAS4B and IRAS2A (2006, background): “Data are taken from Gibb et al. (2000a) and references therein, and from Ikeda et al. (2001).”
A Spitzer IRS Low-Resolution Spectroscopic Search for Buried AGNs in Nearby Ultraluminous Infrared Galaxies: A Constraint on Geometry between Energy Sources and Dust (2007, methodology): “We ascribe the dips to the 6.0 mH2O absorption feature (bending mode), as has been found in both Galactic obscured stars (Gibb et al. 2000;Keane et al. 2001) and obscuredULIRGs (Spoon et al. 2002).”
Interstellar Ice: The Infrared Space Observatory Legacy (2004, methodology): “Points with signal-to-noise ratio of less than 3 or flux density of less than 0.1 Jy were removed (see Gibb et al. 2000 for details).”
ON THE FORMATION OF CO2 AND OTHER INTERSTELLAR ICES (2011, background): “The abundance of NH3 is nevertheless rather high for dark-cloud observational val- ues, although it does not exceed levels observed toward star-forming regions (20 – 30 %, Gibb et al., 2000), after its initial peak.”
From molecular cores to planet-forming disks: An SIRTF legacy program (2003, methodology): “Based on van den Ancker et al. (2000a, 2000b), Gibb et al. (2000), Crovisier et al. (1997), and Malfait et al. (1998). mid-infrared.”
Molecular Depletion and Thermal Balance in Dark Cloud Cores (2000, result): “Most of these results come from infrared spectroscopy, and the Infrared Space Observatory has signiÐcantly expanded this data (see, e.g., Gibb et al. 2000).”
Ice structures, patterns, and processes: A view across the icefields (2012, background): “Spectroscopic surveys show that water, methanol, carbon dioxide, carbon monoxide and ammonia molecules are often present in these mixed ice mantles (Gibb et al., 2000).”
Photodestruction of Relevant Interstellar Molecules in Ice Mixtures (2003, background): “Baratta et al. (2002) measured some absorption coefficients at Ly (but this is more likely an average value over the whole UV range of their lamp) at 12.5 K: H2O (28 104 cm 1), CH4 (19 104 cm 1), CH3OH (12 104 cm 1), or 8:4 10 18, 5:7 10 18, and 3:6 10 18 cm2molecule 1, respectively, assuming an ice”
Ice absorption features in the 5-8 μm region toward embedded protostars (2001, background): “Comparison of the 9 µm inversion mode with various laboratory profiles indicate that the NH3 is most likely frozen in an H2O-rich ice (Lacy et al. 1998; Gibb et al. 2000).”
Resetting chemical clocks of hot cores based on S-bearing molecules (2004, positive): “The lack of an appropriate feature in the ISO spectra of high (Gibb et al. 2000) and low (Boogert et al. 2000) mass protostars sets an upper limit on the mantle H2S abundance which cannot exceed about 10−7 with respect to H2 (van Dishoeck & Blake 1998).”