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Full-Text Articles in Physical Sciences and Mathematics
Submillimeter Wave Astronomy Satellite Observations Of Extended Water Emission In Orion, Ronald L. Snell, Je Howe, Mln Ashby, Ea Bergin, G Chin, Nr Erickson, Pf Goldsmith, M Harwit, Sc Kleiner, Dg Koch, Da Neufeld, Bm Patten, R Plume, R Schieder, Jr Stauffer, V Tolls, Z Wang, G Winnewisser, Yf Zhang, Gj Melnick
Submillimeter Wave Astronomy Satellite Observations Of Extended Water Emission In Orion, Ronald L. Snell, Je Howe, Mln Ashby, Ea Bergin, G Chin, Nr Erickson, Pf Goldsmith, M Harwit, Sc Kleiner, Dg Koch, Da Neufeld, Bm Patten, R Plume, R Schieder, Jr Stauffer, V Tolls, Z Wang, G Winnewisser, Yf Zhang, Gj Melnick
Astronomy Department Faculty Publication Series
We have used the Submillimeter Wave Astronomy Satellite to map the ground-state 110 → 101 transition of ortho-H2O at 557 GHz in the Orion molecular cloud. H2O emission was detected in Orion over an angular extent of about 20', or nearly 3 pc. The water emission is relatively weak, with line widths (3-6 km s-1) and VLSR velocities (9-11 km s-1) consistent with an origin in the cold gas of the molecular ridge. We find that the ortho-H2O abundance relative to H2 in the extended gas …
Water Abundance In Molecular Cloud Cores, Ronald L. Snell, Je Howe, Mln Ashby, Ea Bergin, G Chin, Nr Erickson, Pf Goldsmith, M Harwit, Sc Kleiner, Dg Koch, Da Neufeld, Bm Patten, R Plume, R Schieder, Jr Stauffer, V Tolls, Z Wang, G Winnewisser, Yf Zhang, Gj Melnick
Water Abundance In Molecular Cloud Cores, Ronald L. Snell, Je Howe, Mln Ashby, Ea Bergin, G Chin, Nr Erickson, Pf Goldsmith, M Harwit, Sc Kleiner, Dg Koch, Da Neufeld, Bm Patten, R Plume, R Schieder, Jr Stauffer, V Tolls, Z Wang, G Winnewisser, Yf Zhang, Gj Melnick
Astronomy Department Faculty Publication Series
We present Submillimeter Wave Astronomy Satellite (SWAS) observations of the 110 → 101 transition of ortho-H2O at 557 GHz toward 12 molecular cloud cores. The water emission was detected in NGC 7538, ρ Oph A, NGC 2024, CRL 2591, W3, W3OH, Mon R2, and W33 and was not detected in TMC-1, L134N, and B335. We also present a small map of the H2O emission in S140. Observations of the H218O line were obtained toward S140 and NGC 7538, but no emission was detected. The abundance of ortho-H2O …
The Distribution Of Water Emission In M17sw, Ronald L. Snell, Je Howe, Mln Ashby, Ea Bergin, G Chin, Nr Erickson, Pf Goldsmith, M Harwit, Sc Kleiner, Dg Koch, Da Neufeld, Bm Patten, R Plume, R Schieder, Jr Stauffer, V Tolls, Z Wang, G Winnewisser, Yf Zhang, Gj Melnick
The Distribution Of Water Emission In M17sw, Ronald L. Snell, Je Howe, Mln Ashby, Ea Bergin, G Chin, Nr Erickson, Pf Goldsmith, M Harwit, Sc Kleiner, Dg Koch, Da Neufeld, Bm Patten, R Plume, R Schieder, Jr Stauffer, V Tolls, Z Wang, G Winnewisser, Yf Zhang, Gj Melnick
Astronomy Department Faculty Publication Series
We present a 17-point map of the M17SW cloud core in the 110 → 101 transition of ortho-H2O at 557 GHz obtained with Submillimeter Wave Astronomy Satellite. Water emission was detected in 11 of the 17 observed positions. The line widths of the H2O emission vary between 4 and 9 km s-1 and are similar to other emission lines that arise in the M17SW core. A direct comparison is made between the spatial extent of the H2O emission and the 13CO J = 5 → 4 emission; the good …
Extended [C I] And (Co)-C-13 (5 -> 4) Emission In M17sw, Je Howe, Mln Ashby, Ea Bergin, G Chin, Nr Erickson, Pf Goldsmith, M Harwit, Dj Hollenbach, Mj Kaufman, Sc Kleiner, Dg Koch, Da Neufeld, Bm Patten, R Plume, R Schieder, Ronald L. Snell, Jr Stauffer, V Tolls, Z Wang, G Winnewisser, Yf Zhang, Gj Melnick
Extended [C I] And (Co)-C-13 (5 -> 4) Emission In M17sw, Je Howe, Mln Ashby, Ea Bergin, G Chin, Nr Erickson, Pf Goldsmith, M Harwit, Dj Hollenbach, Mj Kaufman, Sc Kleiner, Dg Koch, Da Neufeld, Bm Patten, R Plume, R Schieder, Ronald L. Snell, Jr Stauffer, V Tolls, Z Wang, G Winnewisser, Yf Zhang, Gj Melnick
Astronomy Department Faculty Publication Series
We mapped a 13 × 22 pc region in emission from 492 GHz [C I] and, for the first time, 551 GHz 13CO (5 → 4) in the giant molecular cloud M17SW. The morphologies of the [C I] and 13CO emission are strikingly similar. The extent and intensity of the [C I] and 13CO (5 → 4) emission is explained as arising from photodissociation regions on the surfaces of embedded molecular clumps. Modeling of the 13CO (5 → 4) emission in comparison to 13CO (1 → 0) indicates a temperature gradient across the cloud, peaking …