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molecules:ism:h2o [2024/03/22 11:42] – mueller | molecules:ism:h2o [2024/03/22 13:44] – mueller |
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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)\\ |
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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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