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--- molecules:ism:h2o [2019/02/25 22:38] – external edit 127.0.0.1
+++ molecules:ism:h2o [2024/03/22 13:53] (current) – mueller
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 ===== Water, H2O, in the Interstellar Medium =====
-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,\\
-**[[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).\\
-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.\\
+\\
 Singly deterated water, HDO, was reported first by\\
 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).\\
-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.\\
+\\
 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,\\
-**[[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).\\
-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.\\
+\\
 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,\\
-**[[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).\\
+\\
 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,\\
-**[[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).\\
+\\
-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.\\
+\\
+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,\\
-**[[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).\\
+\\
+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.\\
+\\
-----
+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.\\
+\\
-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)\\
+highly rotationally or vibrationally excited lines of H<sub>2</sub>O, of which 9 are new detections. The lines were obtained in selected ranges in the frequency region betweeb 222 and 269 GHz. Three of the lines involve the second triad, consisting of the states //v//<sub>2</sub> = //v//<sub>3</sub> = 1, //v//<sub>1</sub> = //v//<sub>2</sub> = 1, and //v//<sub>2</sub> = 3.\\
+\\
+----
+Contributor(s): H. S. P. Müller; 04, 2007; 03, 2024
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