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| molecules:ism:h3-plus [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:h3-plus [2020/09/18 14:11] (current) – [On the Detection of H2D+] mueller |
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| T. R. Geballe and T. Oka\\ | T. R. Geballe and T. Oka\\ |
| used the United Kingdom InfraRed Telescope (UKIRT) for the\\ | used the United Kingdom InfraRed Telescope (UKIRT) for the\\ |
| **[[http://dx.doi.org/10.1038/384334a0|Detection of H<sub>3</sub><sup>+</sup> in Interstellar Space]]**\\ | **[[https://doi.org/10.1038/384334a0|Detection of H<sub>3</sub><sup>+</sup> in Interstellar Space]]**\\ |
| //Nature// **384**, 334–335 (1996).\\ | //Nature// **384**, 334–335 (1996).\\ |
| They detected the lowest //para// transitions R(1,1)<sup>+</sup> and R(1,1)<sup>–</sup> and the lowest //ortho// transition R(1,0) of the degenerate //ν//<sub>2</sub> band near 2700 cm<sup>–1</sup> in absorption in the dense molecular clouds RAFGL (or CRL) 2136 and W33A which both surround deeply embedded young stellar objects. CRL 2136 is also known as IRAS 18196-1331 or OH 17.6+0.2; W33A is also known as IRAS 18117-1753. | They detected the lowest //para// transitions R(1,1)<sup>+</sup> and R(1,1)<sup>–</sup> and the lowest //ortho// transition R(1,0) of the degenerate //ν//<sub>2</sub> band near 2700 cm<sup>–1</sup> in absorption in the dense molecular clouds RAFGL (or CRL) 2136 and W33A which both surround deeply embedded young stellar objects. CRL 2136 is also known as IRAS 18196-1331 or OH 17.6+0.2; W33A is also known as IRAS 18117-1753. |
| B. J. McCall, T. R. Geballe, K. H. Hinkle, and T. Oka\\ | B. J. McCall, T. R. Geballe, K. H. Hinkle, and T. Oka\\ |
| reported on the\\ | reported on the\\ |
| **[[http://dx.doi.org/10.1126/science.279.5358.1910|Detection of H<sub>3</sub><sup>+</sup> in the Diffuse Interstellar Medium Toward Cygnus OB2 No. 12]]**\\ | **[[https://doi.org/10.1126/science.279.5358.1910|Detection of H<sub>3</sub><sup>+</sup> in the Diffuse Interstellar Medium Toward Cygnus OB2 No. 12]]**\\ |
| //Science// **279**, 1910–1913 (1998).\\ | //Science// **279**, 1910–1913 (1998).\\ |
| UKIRT was again employed to detect the same three rovibrational transitions as above. The source is also known as VI Cygni 12 or IRC +40430 or IRAS 20308+4104. The authors found surprisingly high column densities of the molecular cation. Similar findings were made in other diffuse molecular clouds. An explanation was found by\\ | UKIRT was again employed to detect the same three rovibrational transitions as above. The source is also known as VI Cygni 12 or IRC +40430 or IRAS 20308+4104. The authors found surprisingly high column densities of the molecular cation. Similar findings were made in other diffuse molecular clouds. An explanation was found by\\ |
| B. J. McCall, A. J. Huneycutt, R. J. Saykally, T. R. Geballe, N. Djuric, G. H. Dunn, J. Semaniak, O. Novotny, A. Al-Khalili, A. Ehlerding, F. Hellberg, S. Kalhori, A. Neau, R. Thomas, F. Österdahl, and M. Larsson,\\ | B. J. McCall, A. J. Huneycutt, R. J. Saykally, T. R. Geballe, N. Djuric, G. H. Dunn, J. Semaniak, O. Novotny, A. Al-Khalili, A. Ehlerding, F. Hellberg, S. Kalhori, A. Neau, R. Thomas, F. Österdahl, and M. Larsson,\\ |
| who derived\\ | who derived\\ |
| **[[http://dx.doi.org/10.1038/nature01498|An Enhanced Cosmic-ray Flux towards ζ Persei Inferred from a Laboratory Study of the H<sub>3</sub><sup>+</sup>–e<sup>–</sup> Recombination Rate]]**\\ | **[[https://doi.org/10.1038/nature01498|An Enhanced Cosmic-ray Flux towards ζ Persei Inferred from a Laboratory Study of the H<sub>3</sub><sup>+</sup>–e<sup>–</sup> Recombination Rate]]**\\ |
| //Nature// **422**, 500–502 (2003). | //Nature// **422**, 500–502 (2003). |
| |
| Hot H<sub>3</sub><sup>+</sup> was detected in the Central Molecular Zone (CMZ), a region of radius ∼150 pc at the Galactic center both in diffuse molecular clouds via the metastable R(3,3)<sup>l</sup> transition at 2829.9 cm<sup>–1</sup> by\\ | Hot H<sub>3</sub><sup>+</sup> was detected in the Central Molecular Zone (CMZ), a region of radius ∼150 pc at the Galactic center both in diffuse molecular clouds via the metastable R(3,3)<sup>l</sup> transition at 2829.9 cm<sup>–1</sup> by\\ |
| M. Goto, B. J. McCall, T. R. Geballe, T. Usuda, N. Kobayashi, H. Terada, and T. Oka,\\ | M. Goto, B. J. McCall, T. R. Geballe, T. Usuda, N. Kobayashi, H. Terada, and T. Oka,\\ |
| **[[http://cdsads.u-strasbg.fr/abs/2002PASJ...54..951G|Absorption Line Survey of H<sub>3</sub><sup>+</sup> toward the Galactic Center Sources I. GCS 3–2 and GC IRS3]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/2002PASJ...54..951G|Absorption Line Survey of H<sub>3</sub><sup>+</sup> toward the Galactic Center Sources I. GCS 3–2 and GC IRS3]]**\\ |
| //Publ. Astron. Soc. Japan// **44**, 951–961 (2002)\\ | //Publ. Astron. Soc. Japan// **44**, 951–961 (2002)\\ |
| using the Subaru IRCS; and also in dense molecular clouds via the metastable R(2,2)<sup>l</sup> transition at 2762.1 cm<sup>–1</sup> in addition to R(3,3)<sup>l</sup> by\\ | using the Subaru IRCS; and also in dense molecular clouds via the metastable R(2,2)<sup>l</sup> transition at 2762.1 cm<sup>–1</sup> in addition to R(3,3)<sup>l</sup> by\\ |
| M. Goto, T. Usuda, T. Nagata, T. R. Geballe, B. J. McCall, N. Indriolo, H. Suto, T. Henning, C. P. Morong, and T. Oka,\\ | M. Goto, T. Usuda, T. Nagata, T. R. Geballe, B. J. McCall, N. Indriolo, H. Suto, T. Henning, C. P. Morong, and T. Oka,\\ |
| **[[http://dx.doi.org/10.1086/591657|Absorption Line Survey of H<sub>3</sub><sup>+</sup> toward the Galactic Center Sources. II. Eight Infrared Sources within 30 pc of the Galactic Center]]**\\ | **[[https://doi.org/10.1086/591657|Absorption Line Survey of H<sub>3</sub><sup>+</sup> toward the Galactic Center Sources. II. Eight Infrared Sources within 30 pc of the Galactic Center]]**\\ |
| //Astrophys. J.// **688**, 306–319 (2008).\\ | //Astrophys. J.// **688**, 306–319 (2008).\\ |
| As it turned out, some velocity components toward GC IRS3 include dense molecular clouds because of the presence of this high density indicating transition, whereas it is absent in other velocity components. Subaru IRCS and UKIRT were employed in this study. | As it turned out, some velocity components toward GC IRS3 include dense molecular clouds because of the presence of this high density indicating transition, whereas it is absent in other velocity components. Subaru IRCS and UKIRT were employed in this study. |
| R. Stark, F. F. S. van der Tak, and E. van Dishoek\\ | R. Stark, F. F. S. van der Tak, and E. van Dishoek\\ |
| used the JCMT 15 m radio telescope for the\\ | used the JCMT 15 m radio telescope for the\\ |
| **[[http://dx.doi.org/10.1086/312182|Detection of Interstellar H<sub>2</sub>D<sup>+</sup> Emission]]**\\ | **[[https://doi.org/10.1086/312182|Detection of Interstellar H<sub>2</sub>D<sup>+</sup> Emission]]**\\ |
| //Astrophys. J.// **521**, L67–L70 (1999).\\ | //Astrophys. J.// **521**, L67–L70 (1999).\\ |
| The 1<sub>1,0</sub> – 1<sub>1,1</sub> //ortho// transition at 372421.385 MHz was detected toward the young stellar object NGC 1333 IRAS 4A.\\ | The 1<sub>1,0</sub> – 1<sub>1,1</sub> //ortho// transition at 372421.385 MHz was detected toward the young stellar object NGC 1333 IRAS 4A.\\ |
| P. Caselli, F. F. S. van der Tak, C. Ceccarelli, and A. Bacmann\\ | P. Caselli, F. F. S. van der Tak, C. Ceccarelli, and A. Bacmann\\ |
| used the CSO 14.4 m dish to detect the same line and concluded\\ | used the CSO 14.4 m dish to detect the same line and concluded\\ |
| **[[http://dx.doi.org/10.1051/0004-6361:20030526|Abundant H<sub>2</sub>D<sup>+</sup> in the Pre-stellar Core L1544]]**\\ | **[[https://doi.org/10.1051/0004-6361:20030526|Abundant H<sub>2</sub>D<sup>+</sup> in the Pre-stellar Core L1544]]**\\ |
| //Astron. Astrophys.// **403**, L37–L41 (2003).\\ | //Astron. Astrophys.// **403**, L37–L41 (2003).\\ |
| Several further reports appeared. | Several further reports appeared. |
| There is a second rotational ground state transition of //ortho//-H<sub>2</sub>D<sup>+</sup>, the 2<sub>1,2</sub> – 1<sub>1,1</sub> transition at 2363.243 GHz. It was detected in absorption with ISO by\\ | There is a second rotational ground state transition of //ortho//-H<sub>2</sub>D<sup>+</sup>, the 2<sub>1,2</sub> – 1<sub>1,1</sub> transition at 2363.243 GHz. It was detected in absorption with ISO by\\ |
| J. Cernicharo, E. Polehampton, and J. R. Goicoechea:\\ | J. Cernicharo, E. Polehampton, and J. R. Goicoechea:\\ |
| **[[http://dx.doi.org/10.1086/512857|Far-Infrared Detection of H<sub>2</sub>D<sup>+</sup> toward Sgr B2]]**\\ | **[[https://doi.org/10.1086/512857|Far-Infrared Detection of H<sub>2</sub>D<sup>+</sup> toward Sgr B2]]**\\ |
| //Astrophys. J.// **657**, L21–L24 (2007). | //Astrophys. J.// **657**, L21–L24 (2007). |
| |
| S. Brünken, O. Sipilä, E. T. Chambers, J. Harju, P. Caselli, O. Asvany, C. E. Honingh, T. Kamiński, K. M. Menten, J. Stutzki, and S. Schlemmer,\\ | S. Brünken, O. Sipilä, E. T. Chambers, J. Harju, P. Caselli, O. Asvany, C. E. Honingh, T. Kamiński, K. M. Menten, J. Stutzki, and S. Schlemmer,\\ |
| used the GREAT instrument on board the SOFIA aircraft observatory to detect the 1<sub>0,1</sub> – 0<sub>0,0</sub> ground state transition of //para//-H<sub>2</sub>D<sup>+</sup> at 1370.085 GHz in absorption toward IRAS 16293-2422 and to deduce\\ | used the GREAT instrument on board the SOFIA aircraft observatory to detect the 1<sub>0,1</sub> – 0<sub>0,0</sub> ground state transition of //para//-H<sub>2</sub>D<sup>+</sup> at 1370.085 GHz in absorption toward IRAS 16293-2422 and to deduce\\ |
| **[[http://dx.doi.org/10.1038/nature13924|H<sub>2</sub>D<sup>+</sup> observations give an age of at least one million years for a cloud core forming Sun-like stars]]**\\ | **[[https://doi.org/10.1038/nature13924|H<sub>2</sub>D<sup>+</sup> observations give an age of at least one million years for a cloud core forming Sun-like stars]]**\\ |
| //Nature// **516**, 219–221 (2014). | //Nature// **516**, 219–221 (2014).\\ |
| | See also the **[[https://www.mpifr-bonn.mpg.de/pressreleases/2014/11|MPIfR press release]]** (in English; **[[https://www.mpifr-bonn.mpg.de/pressemeldungen/2014/11|German version]]** also available) or the **[[https://portal.uni-koeln.de/universitaet/aktuell/presseinformationen/detail/das-alter-von-stellaren-kinderstuben|Universität zu Köln press release]]** (in German). |
| |
| ==== On the Detection of HD2+ ==== | ==== On the Detection of HD2+ ==== |
| C. Vastel, T. G. Phillips, and H. Yoshida\\ | C. Vastel, T. G. Phillips, and H. Yoshida\\ |
| used the CSO 10.4 m radio telescope for the\\ | used the CSO 10.4 m radio telescope for the\\ |
| **[[http://dx.doi.org/10.1086/421265|Detection of D<sub>2</sub>H<sup>+</sup> in the Dense Interstellar Medium]]**\\ | **[[https://doi.org/10.1086/421265|Detection of D<sub>2</sub>H<sup>+</sup> in the Dense Interstellar Medium]]**\\ |
| //Astrophys. J.// **606**, L127–L130 (2004).\\ | //Astrophys. J.// **606**, L127–L130 (2004).\\ |
| The 1<sub>1,0</sub> – 1<sub>0,1</sub> //para// transition at 691660.483 MHz was barely detected in emission toward the prestellar core IRAS 16293-2422E.\\ | The 1<sub>1,0</sub> – 1<sub>0,1</sub> //para// transition at 691660.483 MHz was barely detected in emission toward the prestellar core IRAS 16293-2422E.\\ |
| B. Parise, A. Belloche, F. Du, R. Güsten, and K. M. Menten\\ | B. Parise, A. Belloche, F. Du, R. Güsten, and K. M. Menten\\ |
| observed the same line with the APEX 12 m radio telescope in the H-MM1 prestellar core located in the Ophiuchus L1688 cloud and found\\ | observed the same line with the APEX 12 m radio telescope in the H-MM1 prestellar core located in the Ophiuchus L1688 cloud and found\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201015475|Extended Emission of HD<sub>2</sub><sup>+</sup> in a Pre-stellar Core]]**\\ | **[[https://doi.org/10.1051/0004-6361/201015475|Extended Emission of HD<sub>2</sub><sup>+</sup> in a Pre-stellar Core]]**\\ |
| //Astron. Astrophys.// **526**, Art. No. A31 (2011). | //Astron. Astrophys.// **526**, Art. No. A31 (2011). |
| |
| J. Harju, O. Sipilä, S. Brünken, S. Schlemmer, P. Caselli, M. Juvela, K. M. Menten, J. Stutzki, O. Asvany, T. Kamiński, Y. Okada, and R. Higgins\\ | J. Harju, O. Sipilä, S. Brünken, S. Schlemmer, P. Caselli, M. Juvela, K. M. Menten, J. Stutzki, O. Asvany, T. Kamiński, Y. Okada, and R. Higgins\\ |
| used the GREAT instrument on board the SOFIA aircraft observatory to detect the 1<sub>1,1</sub> – 0<sub>0,0</sub> ground state transition of //ortho//-H<sub>2</sub>D<sup>+</sup> at 1476.606 GHz in absorption toward IRAS 16293-2422\\ | used the GREAT instrument on board the SOFIA aircraft observatory to detect the 1<sub>1,1</sub> – 0<sub>0,0</sub> ground state transition of //ortho//-H<sub>2</sub>D<sup>+</sup> at 1476.606 GHz in absorption toward IRAS 16293-2422\\ |
| **[[http://dx.doi.org/10.3847/1538-4357/aa6c69|Detection of Interstellar //Ortho//-D<sub>2</sub>H<sup>+</sup> with SOFIA]]**\\ | **[[https://doi.org/10.3847/1538-4357/aa6c69|Detection of Interstellar //Ortho//-D<sub>2</sub>H<sup>+</sup> with SOFIA]]**\\ |
| //Astrophys. J.// **840**, Art. No. 63 (2017). | //Astrophys. J.// **840**, Art. No. 63 (2017). |
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| Contributor(s): H. S. P. Müller; 4, 2004; 01, 2014; 12, 2015; 05, 2017 | Contributor(s): H. S. P. Müller; 4, 2004; 01, 2014; 12, 2015; 05, 2017 |
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