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molecules:ism:h2o [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:h2o [2024/03/22 13:44] – mueller |
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===== Water, H2O, in the Interstellar Medium ===== | ===== Water, H2O, in the Interstellar Medium ===== |
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The observation of water, H<sub>2</sub>O, by radioastronomy is often hampered because of the presence of water in Earth's amosphere. Only comparatively weak transitions can be detected as there will be non-zero transmittance at these frequencies through the atmosphere. Nevertheless, water was one of the first molecules to be detected in the interstellar medium. The //J<sub>K<sub>a</sub>K<sub>c</sub></sub>// = 6<sub>16</sub> – 5<sub>23</sub> //ortho// rotational transition of water, H<sub>2</sub>O, was observed in Orion, SgrB2, and W49 displaying maser activity:\\ | The observation of water, H<sub>2</sub>O, by radioastronomy is often hampered because of the presence of water in Earth's amosphere. Only comparatively weak transitions can be detected as there will be non-zero transmittance at these frequencies through the atmosphere. Nevertheless, water was one of the first molecules to be detected in the interstellar medium. The //J<sub>KaKc</sub>// = 6<sub>16</sub> – 5<sub>23</sub> //ortho// rotational transition of water, H<sub>2</sub>O, was observed in Orion, SgrB2, and W49 displaying maser activity:\\ |
A. C. Cheung, D. M. Rank, C. H. Townes, D. D. Thornton, and W. J. Welch,\\ | A. C. Cheung, D. M. Rank, C. H. Townes, D. D. Thornton, and W. J. Welch,\\ |
**[[http://dx.doi.org/10.1038/221626a0|Detection of Water in Interstellar Regions by its Microwave Radiation]]**\\ | **[[https://doi.org/10.1038/221626a0|Detection of Water in Interstellar Regions by its Microwave Radiation]]**\\ |
//Nature// **221**, 626–628 (1969).\\ | //Nature// **221**, 626–628 (1969).\\ |
At the observed intensity levels, the detection could be viewed as secure. In the meantime, many additional transitions have been reported. | At the observed intensity levels, the detection could be viewed as secure. In the meantime, many additional transitions have been reported.\\ |
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Singly deterated water, HDO, was reported first by\\ | Singly deterated water, HDO, was reported first by\\ |
B. E. Turner, N. Fourikis, M. Morris, P. Palmer, and B. Zuckerman,\\ | B. E. Turner, N. Fourikis, M. Morris, P. Palmer, and B. Zuckerman,\\ |
**[[http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1975ApJ...198L.125T|Microwave Detection of Interstellar HDO]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1975ApJ...198L.125T|Microwave Detection of Interstellar HDO]]**\\ |
//Astrophys. J.// **198**, L125–L128 (1975).\\ | //Astrophys. J.// **198**, L125–L128 (1975).\\ |
The 1<sub>11</sub> – 1<sub>10</sub> transition was observed in emission toward Orion KL. Several other transitions have been reported in the meantime. | The 1<sub>11</sub> – 1<sub>10</sub> transition was observed in emission toward Orion KL. Several other transitions have been reported in the meantime.\\ |
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H<sub>2</sub><sup>18</sup>O was detected in emission through its 3<sub>13</sub> – 2<sub>20</sub> transition toward G34.3+0.2:\\ | H<sub>2</sub><sup>18</sup>O was detected in emission through its 3<sub>13</sub> – 2<sub>20</sub> transition toward G34.3+0.2:\\ |
T. Jacq, C. Henkel, C. M. Walmsley, P. R. Jewell, and A. Baudry,\\ | T. Jacq, C. Henkel, C. M. Walmsley, P. R. Jewell, and A. Baudry,\\ |
**[[http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1988A%26A...199L...5J|H<sub>2</sub><sup>18</sup>O in Hot Dense Molecular Cloud Cores]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1988A%26A...199L...5J|H<sub>2</sub><sup>18</sup>O in Hot Dense Molecular Cloud Cores]]**\\ |
//Astron. Astrophys.// **199**, L5–L8 (1988).\\ | //Astron. Astrophys.// **199**, L5–L8 (1988).\\ |
Emission features were also detected toward Orion KL, Sgr B2(N), and W51 e1/e2, but not unambiguous because possible overlap with lines of other molecules. In the meantime, other transitions have been detected, too. | Emission features were also detected toward Orion KL, Sgr B2(N), and W51 e1/e2, but not unambiguous because possible overlap with lines of other molecules. In the meantime, other transitions have been detected, too.\\ |
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H<sub>2</sub><sup>17</sup>O was detected in emission through its 1<sub>10</sub> – 1<sub>10</sub> transition toward Orion KL:\\ | H<sub>2</sub><sup>17</sup>O was detected in emission through its 1<sub>10</sub> – 1<sub>10</sub> transition toward Orion KL:\\ |
Å. Hjalmarson, P. Bergman, N. Biver, H.-G. Flor&eacite;n, U. Frisk, T. Hasegawa, K. Justtanont, B. Larsson, S. Lundin, M. Olberg, H. Olofsson, G. Persson, G. Rydbeck, A. Sandqvist,\\ | Å. Hjalmarson, P. Bergman, N. Biver, H.-G. Flor&eacite;n, U. Frisk, T. Hasegawa, K. Justtanont, B. Larsson, S. Lundin, M. Olberg, H. Olofsson, G. Persson, G. Rydbeck, A. Sandqvist,\\ |
**[[http://dx.doi.org/10.1016/j.asr.2005.06.014|Recent Astronomy Highlights from the Odin Satellite]]**\\ | **[[https://doi.org/10.1016/j.asr.2005.06.014|Recent Astronomy Highlights from the Odin Satellite]]**\\ |
//Adv. Space Res.// **36**, 1031–1047 (2005). | //Adv. Space Res.// **36**, 1031–1047 (2005).\\ |
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The 1<sub>10</sub> – 1<sub>10</sub> transition of doubly deuterated water was detected in emission and absorption toward IRAS 16293-2422, a low-mass protostellar binary system:\\ | The 1<sub>10</sub> – 1<sub>10</sub> transition of doubly deuterated water was detected in emission and absorption toward IRAS 16293-2422, a low-mass protostellar binary system:\\ |
H. M. Butner, S. B. Charnley, C. Ceccarelli, S. D. Rodgers, J. R. Pardo, B. Parise, J. Cernicharo, and G. R. Davis,\\ | H. M. Butner, S. B. Charnley, C. Ceccarelli, S. D. Rodgers, J. R. Pardo, B. Parise, J. Cernicharo, and G. R. Davis,\\ |
**[[http://dx.doi.org/10.1086/517883|Discovery of Interstellar Heavy Water]]**\\ | **[[https://doi.org/10.1086/517883|Discovery of Interstellar Heavy Water]]**\\ |
//Astrophys. J.// **659**, L137–L140 (2007). | //Astrophys. J.// **659**, L137–L140 (2007).\\ |
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Water in its //v//<sub>2</sub> = 1 excited vibrational state were detected in emission first towards VY CMa and W Hya:\\ | E. A. Bergin, T. G. Phillips, C. Comito, //et al.//\\ |
| presented in their account on\\ |
| **[[https://doi.org/10.1051/0004-6361/201015071|//Herschel// observations of EXtra-Ordinary Sources (HEXOS): The present and future of spectral surveys with //Herschel///HIFI]]**\\ |
| //Astron. Astrophys.// **521**, Art. No. L20 (2010)\\ |
| also an account of the detection of HD<sup>18</sup>O toward Orion KL. Four low-lying transitions were observed in emission. The derived D/H ration with respect to HDO is ~0.02.\\ |
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| Water in its //v//<sub>2</sub> = 1 excited vibrational state were detected in emission first toward two O-rich late-type stars VY CMa and W Hya:\\ |
K. M. Menten and G. J. Melnick,\\ | K. M. Menten and G. J. Melnick,\\ |
**[[http://dx.doi.org/10.1086/185465|Hot Water around Late-Type Stars – Detection of Two Millimeter-Wave Emission Lines from the //v//<sub>2</sub> Vibrationally Excited State]]**\\ | **[[https://doi.org/10.1086/185465|Hot Water around Late-Type Stars – Detection of Two Millimeter-Wave Emission Lines from the //v//<sub>2</sub> Vibrationally Excited State]]**\\ |
//Astrophys. J.// **341**, L91–L94 (1989). | //Astrophys. J.// **341**, L91–L94 (1989).\\ |
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| E. D. Tenenbaum, J. L. Dodd, S. N. Milam, N. J. Woolf, and L. M. Ziurys\\ |
| describe in their work on\\ |
| **[[https://doi.org/10.1088/2041-8205/720/1/L102|Comparative Spectra of Oxygen-rich Versus Carbon-rich Circumstellar Shells: VY Canis Majoris and IRC +10216 at 215−285 GHz]]**\\ |
| //Astrophys. J. Lett.// **720**, L102–L107 (2010).\\ |
| the detection of the 6<sub>5,2</sub> – 7<sub>4,3</sub> transition of H<sub>2</sub>O in its //v//<sub>2</sub> = 2 state near 268.149 GHz.\\ |
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---- | T. Kamiński, H. S. P. Müller, M. R. Schmidt, I. Cherchneff, K. T. Wong, S. Brünken, K. M. Menten, J. M. Winters, C. A. Gottlieb, and N. A. Patel\\ |
| mentioned in their account on\\ |
| **[[https://doi.org/10.1051/0004-6361/201629838|An observational study of dust nucleation in Mira (o Ceti) — II. Titanium oxides are negligible for nucleation at high temperatures]]**\\ |
| //Astron. Astrophys.// **599**, Art. No. A59 (2017)\\ |
| the identification of highly rotationally and vibrationally excited lines of H<sub>2</sub>O, among them a formally ro-vibrational transition //v//<sub>1</sub> = 1 – //v//<sub>3</sub> = 1, 12<sub>3,9</sub> – 11<sub>5,6</sub> near 345.67 GHz.\\ |
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Contributor(s): H. S. P. Müller; 04, 2007 | A. Baudry, K. T. Wong, S. Etoka, A. M. S. Richards, H. S. P. Müller, F. Herpin, T. Danilovich, M. D. Gray, S. Wallström, D. Gobrecht, T. Khouri, L. Decin, C. A. Gottlieb, K. M. Menten, W. Homan, T. J. Millar, M. Montargès, B. Pimpanuwat, J. M. C. Plane, and P. Kervella\\ |
| detected in their investigation\\ |
| **[[https://doi.org/10.1051/0004-6361/202245193|ATOMIUM: Probing the inner wind of evolved O-rich stars |
| with new, highly excited H<sub>2</sub>O and OH lines]]**\\ |
| //Astron. Astrophys.// **674**, Art. No. A125 (2023)\\ |
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| Contributor(s): H. S. P. Müller; 04, 2007; 03, 2024 |
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