A Line Survey of Orion-KL from 607 to 725 GHz

By Peter Schilke, D. J. Benford, Todd R. Hunter, D. Lis, T. Phillips. 2001

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Resetting chemical clocks of hot cores based on S-bearing molecules (2004, unknown): “The SO, SO2, H2S and OCS column densities have been derived by Schilke et al. (2001) and Sutton et al. (1995) to be 2.3 × 1017, 6 × 1016, 1.2 × 1016 cm−2 and 9 × 1015 cm−2, respectively.”
A line confusion limited millimeter survey of Orion KL I. Sulfur carbon chains - I. Sulfur carbon chains (2010, background): “This CS column density is about 10-30 times larger than found in many previous stud- ies (Blake et al., 1987; Lee et al., 2001; Schilke et al., 2001).”
Hot corinos in NGC 1333-IRAS4B and IRAS2A (2006, background): “Indeed, high energy transitions are more easily detected in high than low mass protostars (e.g., Comito et al. 2005; Schilke et al. 2001, 1997; Blake et al. 1995), which support the above interpretation.”
Testing grain-surface chemistry in massive hot-core regions (2007, background): “Many line surveys have been performed to study the molecular composition of high mass star forming regions (e.g., Blake et al. 1987; Sutton et al. 1995; Helmich & van Dishoeck 1997; Schilke et al. 1997; Nummelin et al. 2000; Gibb et al. 2000a; Schilke et al. 2001).”
2018 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules (2018, result): “SiH (silicon hydride) Schilke et al. (2001) reported the tentative detection of two features in a CSO line survey of Orion that were coincident with transitions of SiH.”