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| DC Field | Value | Language |
|---|---|---|
| dc.creator | Cernicharo, José | - |
| dc.creator | Goicoechea, Javier R. | - |
| dc.creator | Pardo Carrión, Juan Ramón | - |
| dc.creator | Asensio Ramos, Andrés | - |
| dc.date | 2008-01-03T16:14:27Z | - |
| dc.date | 2008-01-03T16:14:27Z | - |
| dc.date | 2006-05-10 | - |
| dc.date.accessioned | 2017-01-31T00:59:39Z | - |
| dc.date.available | 2017-01-31T00:59:39Z | - |
| dc.identifier | The Astrophysical Journal, 642: 940-953 (2006) | - |
| dc.identifier | 1538-4357 | - |
| dc.identifier | http://hdl.handle.net/10261/2652 | - |
| dc.identifier | 10.1086/501425 | - |
| dc.identifier.uri | http://dspace.mediu.edu.my:8181/xmlui/handle/10261/2652 | - |
| dc.description | Several condensations heated externally by nearby hot stars are present in the Sgr B2 region for which H2O far-IR lines are expected to probe only an external low-density and high temperature section. Millimeter-wave lines can penetrate deeper into them (higher densities and lower Tk). We have conducted a study combining H2O lines in both spectral regions using the ISO (far-IR lines) and the IRAM 30m telescope (183 GHz line). The far-IRH2O lines, seen in absorption, are optically thick. They form in the outermost gas in front of the far-IR continuum sources, probing a maximum visual extinction of ~5–10 mag. IR photons from the dust play a dominant role in their excitation. We conclude, based on observations of the COJ = 7-6 line at 806.65 GHz, and the lack of emission from the far-IR CO lines, that the gas density has to be below ~10^4 cm^-3. Using the gas kinetic temperature and density derived from OH, CO, and other molecular species, we derive a water column density of (9 ± 3) x 10^16 cm^-2 in the absorbing gas, implying an abundance of ~(1-2) x 10^-5 in this region. The resulting relatively low H2O/OH abundance ratio, ~2–4, is a signature of UV photon-dominated surface layers traced by far-IR observations. As a consequence, the temperature of the absorbing gas is high, Tk ~ 300-500 K, which allows very efficient neutral-neutral reactions producing H2O and OH. Finally, the 183.31 GHz data allow one to trace the inner, denser (n(H2) > 10^5-10^6 cm^-3), and colder (Tk ~ 40K) gas. The emission is very strong toward the cores with an estimated water vapor abundance of a few x 10^-7. There is also moderate extended emission around Sgr B2 main condensations, in agreement with the water vapor abundance derived from far-IR H2O lines. | - |
| dc.description | We thank Spanish DGES and PNIE for funding support under grants PANAYA2000-1784, ESP2001-4516, AYA2002-10113-E, ESP2002-01627,AYA2003-02785-E and AYA2004-05792. CSO observations were supported by NSF grant AST-9980846. J.R.G. was also supported by the French Direction de la Recherche in the latest stages of the work. | - |
| dc.description | Peer reviewed | - |
| dc.format | 1372655 bytes | - |
| dc.format | application/pdf | - |
| dc.language | eng | - |
| dc.publisher | American Astronomical Society | - |
| dc.publisher | University of Chicago Press | - |
| dc.rights | openAccess | - |
| dc.subject | Infrared: ISM | - |
| dc.subject | ISM: individual (Sgr B2) | - |
| dc.subject | ISM: lines and bands | - |
| dc.subject | ISM: molecules | - |
| dc.subject | Radiative transfer | - |
| dc.title | Warm Water Vapor around Sagittarius B2 | - |
| dc.type | Artículo | - |
| Appears in Collections: | Digital Csic | |
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