molecules:ism:po

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molecules:ism:po [2019/10/18 13:03] – muellermolecules:ism:po [2024/08/21 16:33] (current) – mueller
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 **[[https://doi.org/10.1086/521361|Identification of Phosphorus Monoxide (//X// <sup>2</sup>Π<sub>r</sub>) in VY Canis Majoris: Detection of the First P–O Bond in Space]]**\\ **[[https://doi.org/10.1086/521361|Identification of Phosphorus Monoxide (//X// <sup>2</sup>Π<sub>r</sub>) in VY Canis Majoris: Detection of the First P–O Bond in Space]]**\\
 //Astrophys. J.// **666**, L29–L32 (2007).\\ //Astrophys. J.// **666**, L29–L32 (2007).\\
-The //J// = 5.5 – 4.5 and 6.5 – 5.5 transitions were detected in emission near 240 and 284 GHz with resolved splitting of the λ-doubling. The number of observed lines is probably the minimum number for the unambiguous detection of a diatomic molecule. The abundance is about the same as for the PN molecule. Interestingly, it is the first molecule to be detected in an oxygen-rich circumstellar envelope prior to anywhere else in space.+The //J// = 5.5 – 4.5 and 6.5 – 5.5 transitions were detected in emission near 240 and 284 GHz with resolved splitting of the λ-doubling. The number of observed lines is probably the minimum number for the unambiguous detection of a diatomic molecule. The abundance is about the same as for the PN molecule. Interestingly, it is the first molecule to be detected in an oxygen-rich circumstellar envelope prior to anywhere else in space.\\ 
 +\\
  
 E. De Beck, T. Kaminski, N. A. Patel, K. H. Young, C. A. Gottlieb, K. M. Menten, and L. Decin\\ E. De Beck, T. Kaminski, N. A. Patel, K. H. Young, C. A. Gottlieb, K. M. Menten, and L. Decin\\
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 **[[https://doi.org/10.1051/0004-6361/201321349|PO and PN in the Wind of the Oxygen-rich AGB Star IK Tauri]]**\\ **[[https://doi.org/10.1051/0004-6361/201321349|PO and PN in the Wind of the Oxygen-rich AGB Star IK Tauri]]**\\
 //Astron. Astrophys.// **558**, Art. No. A132 (2013).\\ //Astron. Astrophys.// **558**, Art. No. A132 (2013).\\
-Several lines of four rotational transitions were detected with modest to good signal-to-noise ratio using the IRAM 30 m telescope and the SMA. PN was considerably more abundant than PO.+Several lines of four rotational transitions were detected with modest to good signal-to-noise ratio using the IRAM 30 m telescope and the SMA. PN was considerably more abundant than PO.\\ 
 +\\
  
 V. M. Rivilla, F. Fontani, M. T. Beltrán, A. Vasyunin, P. Caselli, J. Martín-Pintado, and R. Cesaroni\\ V. M. Rivilla, F. Fontani, M. T. Beltrán, A. Vasyunin, P. Caselli, J. Martín-Pintado, and R. Cesaroni\\
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 **[[https://doi.org/10.3847/0004-637X/826/2/161|First Detections of the Key Prebiotic Molecule PO in Star-forming Regions]]**\\ **[[https://doi.org/10.3847/0004-637X/826/2/161|First Detections of the Key Prebiotic Molecule PO in Star-forming Regions]]**\\
 //Astrophys. J.// **826**, Art. No. 161 (2016).\\ //Astrophys. J.// **826**, Art. No. 161 (2016).\\
-Three transitions where observed with the IRAM 30 m telescope toward W51 and W3(OH). Hyperfine splitting and λ-doubling were resolved. Signal was detected in all cases with no or only marginal blending in some lines and pronounced to severe blending for others. PO was in both cases more abundant than PN.+Three transitions where observed with the IRAM 30 m telescope toward W51 and W3(OH). Hyperfine splitting and λ-doubling were resolved. Signal was detected in all cases with no or only marginal blending in some lines and pronounced to severe blending for others. PO was in both cases more abundant than PN.\\ 
 +\\
  
 B. Lefloch, C. Vastel, S. Viti, I. Jimenez-Serra, C. Codella, L. Podio, C. Ceccarelli, E. Mendoza, J.R.D. Lepine, R. Bachiller,\\ B. Lefloch, C. Vastel, S. Viti, I. Jimenez-Serra, C. Codella, L. Podio, C. Ceccarelli, E. Mendoza, J.R.D. Lepine, R. Bachiller,\\
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 **[[https://doi.org/10.1093/mnras/stw1918|Phosphorus-bearing Molecules in Solar-type Star Forming Regions: First PO Detection]]**\\ **[[https://doi.org/10.1093/mnras/stw1918|Phosphorus-bearing Molecules in Solar-type Star Forming Regions: First PO Detection]]**\\
 //Mon. Not. R. Astron. Soc.// **462**, 3937–3944 (2016).\\ //Mon. Not. R. Astron. Soc.// **462**, 3937–3944 (2016).\\
-Several lines of PO were detected with the IRAM 30 m telescope toward L1157-B1 with an abundance ratio to PN of 3 : 1.+Several lines of PO were detected with the IRAM 30 m telescope toward L1157-B1 with an abundance ratio to PN of 3 : 1.\\ 
 +\\
  
 +S. H. J. Wallström, T. Danilovich, H. S. P. Müller, C. A. Gottlieb, S. Maes, M. Van de Sande, L. Decin, A. M. S. Richards, A. Baudry, J. Bolte, T. Ceulemans, F. De Ceuster, A. de Koter, I. El Mellah, M. Esseldeurs, S. Etoka, D. Gobrecht, E. Gottlieb, M. Gray, F. Herpin, M. Jeste, D. Kee, P. Kervella, T. Khouri, E. Lagadec, J. Malfait, L. Marinho, I. McDonald, K. M. Menten, T. J. Millar, M. Montargès, J. A. Nuth, J. M. C. Plane, R. Sahai, L. B. F. M. Waters, K. T. Wong, J. Yates, and A. Zijlstra\\
 +reported on\\
 +**[[https://doi.org/10.1051/0004-6361/202347632|ATOMIUM: Molecular Inventory of 17 Oxygen-rich Evolved Stars Observed with ALMA]]**\\
 +//Astron. Astrophys.// **681**, Art. No. A50 (2024).\\
 +The authors detect in their ALMA measurements in Band 6 vibrationally excited PO toward AH Sco, IRC+10011, IRC−10529,
 +R Hya, and S Pav. The Ω = 3/2, //J// = 11/2 − 9/2, //F// = 6 − 5 and 5 − 4 lines near 239.9 GHz with unresolved Λ-doubling were detected near the //v// = 0, Ω = 1/2, //J// = 11/2 − 9/2, //F// = 6 − 5 and 5 − 4 //e//-lines near 240.0 GHz; the //f//-lines were not covered.\\
 +\\
  
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-Contributor(s): H. S. P. Müller; 08, 2007; 08; 2016+Contributor(s): H. S. P. Müller; 08, 2007; 08; 2016; 09, 2024
  
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