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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,\\ |
| **[[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]]**\\ | **[[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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| | 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)\\ |
| | 10 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.\\ |
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| Contributor(s): H. S. P. Müller; 04, 2007 | Contributor(s): H. S. P. Müller; 04, 2007; 03, 2024 |
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