Ice absorption features in the 5-8 μm region toward embedded protostars

By J. Keane, A. Tielens, A. Boogert, W. Schutte, D. Whittet. 2001

200 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/3e84f58b2f7605b4e640843cddaeccd80c7b6d68

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Citations in the corpus

Observations of the Icy Universe (2015, background): “For example, toward the MYSO S140 IRS1, the column densities derived for all CO2 bands over the 2-15 µm wavelength range are in good agreement (Keane et al., 2001a).”
Spatially Resolved Chemistry in Nearby Galaxies. I. The Center of IC 342 (2004, background): “Grim & Greenberg 1987; Demyk et al. 1998; Novozamsky, Schutte, & Keane 2001), which forms either from UV photolysis of CO + NH3 (eg., Grim & Greenberg 1987; Schutte & Greenberg 1997) or by acid-base reactions between HNCO and NH3 (eg., Keane et al. 2001).”
Interstellar Ice: The Infrared Space Observatory Legacy (2004, methodology): “—(1) Gibb et al. 2001; (2) this work; (3) Brooke et al. 1996; (4) Gerakines et al. 1999; (5) Boogert et al. 2000; (6) Gibb & Whittet 2002; (7) Keane et al. 2001c. GIBB ET AL.52 Vol. 151 emission and coincident with an H ii region (IRS 1), greatest molecular densities occurring just beyond the…”
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).”
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).”
Organic molecules in protoplanetary disks around T Tauri and Herbig Ae stars (2004, background): “Both CH3OH and H2CO have been detected in icy mantles, with the CH3OH abundance varying strongly from source to source (Dartois et al. 1999, Keane et al. 2001, Pontoppidan et al. 2003).”
UV-photoprocessing of interstellar ice analogs: New infrared spectroscopic results (2003, background): “Instead, the spectrum of our samples is dominated by the XCOO− feature at 1586 cm−1, which was not detected in the ice spectra towards protostars (Keane et al. 2001).”
Resetting chemical clocks of hot cores based on S-bearing molecules (2004, unknown): “…the major mantle components are relatively well constrained by the observations and we took the observed abundances (with respect to H2) in high mass protostars: H2O: 10−4 (Schutte et al. 1996), H2CO: 4×10−6 (Keane et al. 2001), CH3OH: 4×10−6 (Chiar et al. 1996) and CH4: 10−6 (Boogert et al. 1998).”
Efficient Formation of Formaldehyde and Methanol by the Addition of Hydrogen Atoms to CO in H2O-CO Ice at 10 K (2002, background): “These values are reasonable when compared with the observed abundances in objects toward high-mass protostars (e.g., Keane et al. 2001).”
The Organic Refractory Material in the Diffuse Interstellar Medium: Mid-Infrared Spectroscopic Constraints (2002, background): “The detection of the aromatic band near 6 km detected along several lines of sight through the DISM (Schutte et al. 1998 ; Keane et al. 2001) supports this view of the organic component of DISM dust.”
A 3-5 mu m VLT spectroscopic survey of embedded young low mass stars I - Structure of the CO ice (2003, methodology): “Similar approaches to the analysis of ice bands were used by Keane et al. (2001) for the 6.85µm band, Boogert et al. (2002a) for the CO band and Thi (2002) for the 3.08 µm water band, although for smaller samples or for individual sources.”
The c2d Spitzer Spectroscopic Survey of Ices around Low-Mass Young Stellar Objects. I. H2O and the 5-8 μm Bands (2007, methodology): “The final spectra do not show any significant differences with respect to the data published in Keane et al. (2001b).”
Hydrogenation reactions in interstellar CO ice analogues A combined experimental/theoretical approach (2009, background): “In space, the H2CO/CH3OH ice ratio has been determined directly for only three high-mass young stellar objects (YSOs): W 33A, NGC 7538 IRS9, and AFGL 70009S, with inferred ratios ranging from 0.09 to 0.51 (Keane et al. 2001; Gibb et al. 2004).”
ISO Spectroscopy of Gas and Dust: From Molecular Clouds to Protoplanetary Disks (2004, methodology): “ISO’s main contributions have been of three types: (i) Detections of new interstellar molecules not seen prior to ISO (e.g., CO2, HF, CH3; see Figure 5); (ii) Infrared detections of molecules seen previously at other wavelengths (e.g., H2O, SO2, HD); (iii) Infrared bands of molecules observed previo”
Testing grain-surface chemistry in massive hot-core regions (2007, background): “The H2CO abundance of ∼2 × 10−6, although more uncertain, is also larger by an order of magnitude (Keane et al. 2001).”
Water and astrobiology (2007, unknown): “H2CO can be found at up to 10% (Boogert et al., 1996, 1997, 1998; Keane et al., 2001).”