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| molecules:ism:arh-plus [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:arh-plus [2019/10/18 13:20] (current) – mueller |
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| The //J// = 1 – 0 and 2 – 1 transitions of <sup>36</sup>ArH<sup>+</sup> were detected in emission with the SPIRE instrument on the //Herschel// satellite toward the Crab Nebula supernova remnant, also known as M 1, by:\\ | The //J// = 1 – 0 and 2 – 1 transitions of <sup>36</sup>ArH<sup>+</sup> were detected in emission with the SPIRE instrument on the //Herschel// satellite toward the Crab Nebula supernova remnant, also known as M 1, by:\\ |
| M. J. Barlow, B. M. Swinyard, P. J. Owen, J. Cernicharo, H. L. Gomez, R. J. Ivison, O. Krause, T. L. Lim, M. Matsuura, S. Miller, G. Olofsson, and E. T. Polehampton,\\ | M. J. Barlow, B. M. Swinyard, P. J. Owen, J. Cernicharo, H. L. Gomez, R. J. Ivison, O. Krause, T. L. Lim, M. Matsuura, S. Miller, G. Olofsson, and E. T. Polehampton,\\ |
| **[[http://dx.doi.org/10.1126/science.1243582|Detection of a Noble Gas Molecular Ion, <sup>36</sup>ArH<sup>+</sup>, in the Crab Nebula]]**\\ | **[[https://doi.org/10.1126/science.1243582|Detection of a Noble Gas Molecular Ion, <sup>36</sup>ArH<sup>+</sup>, in the Crab Nebula]]**\\ |
| //Science// **342**, (2013) 1343.\\ | //Science// **342**, (2013) 1343.\\ |
| <sup>40</sup>Ar is the most abundant isotope on Earth, but it is almost exclusively formed in the radioactive decay of <sup>40</sup>K. Interestingly, the only other feature seen clearly in the entire spectrum was the strongest fine structure component of OH<sup>+</sup>, there is also a hint of the next weaker FS component. | <sup>40</sup>Ar is the most abundant isotope on Earth, but it is almost exclusively formed in the radioactive decay of <sup>40</sup>K. Interestingly, the only other feature seen clearly in the entire spectrum was the strongest fine structure component of OH<sup>+</sup>, there is also a hint of the next weaker FS component. |
| P. Schilke, D. A. Neufeld, H. S. P. Müller, C. Comito, E. A. Bergin, D. C. Lis, M. Gerin, J. H. Black, M. Wolfire, N. Indriolo, J. C. Pearson, K. M. Menten, B. Winkel, Á. Sánchez-Monge, T. Möller, B. Godard, and E. Falgarone,\\ | P. Schilke, D. A. Neufeld, H. S. P. Müller, C. Comito, E. A. Bergin, D. C. Lis, M. Gerin, J. H. Black, M. Wolfire, N. Indriolo, J. C. Pearson, K. M. Menten, B. Winkel, Á. Sánchez-Monge, T. Möller, B. Godard, and E. Falgarone,\\ |
| reported on\\ | reported on\\ |
| **[[http://dx.doi.org/10.1051/0004-6361/201423727|Ubiquitous argonium (ArH<sup>+</sup>) in the diffuse interstellar medium: A molecular tracer of almost purely atomic gas]]**\\ | **[[https://doi.org/10.1051/0004-6361/201423727|Ubiquitous argonium (ArH<sup>+</sup>) in the diffuse interstellar medium: A molecular tracer of almost purely atomic gas]]**\\ |
| //Astron. Astrophys.// **566** (2014), Art. No. A29.\\ | //Astron. Astrophys.// **566** (2014), Art. No. A29.\\ |
| The 1 – 0 transition was observed in absorprtion with HIFI on board of the //Herschel// satellite toward numerous prominent continuum sources, first, and most notably, toward Sagittarius B2(M), then Sgr B2(N), and later also toward W51e, W49N, W31C, and G34.26+0.15. Interestingly, the molecule displays absorption at velocities associated with diffuse molecular clouds on the line of sight toward the contiunuum sources, but is conspicuously absent (at least in most cases) at the velocity of the corresponding continuum source itself. Model calculations indicate that ArH<sup>+</sup> resides mostly in very atomic diffuse molecular clouds with a molecular fraction of around 0.001 to 0.0001 or less. It is thus a very good tracer of such interstellar material. Moreover, it is also a good indicator of the cosmic ray ionization rate in addition to or instead of OH<sup>+</sup>, H<sub>2</sub>O<sup>+</sup>, or H<sub>3</sub><sup>+</sup>.\\ | The 1 – 0 transition was observed in absorprtion with HIFI on board of the //Herschel// satellite toward numerous prominent continuum sources, first, and most notably, toward Sagittarius B2(M), then Sgr B2(N), and later also toward W51e, W49N, W31C, and G34.26+0.15. Interestingly, the molecule displays absorption at velocities associated with diffuse molecular clouds on the line of sight toward the contiunuum sources, but is conspicuously absent (at least in most cases) at the velocity of the corresponding continuum source itself. Model calculations indicate that ArH<sup>+</sup> resides mostly in very atomic diffuse molecular clouds with a molecular fraction of around 0.001 to 0.0001 or less. It is thus a very good tracer of such interstellar material. Moreover, it is also a good indicator of the cosmic ray ionization rate in addition to or instead of OH<sup>+</sup>, H<sub>2</sub>O<sup>+</sup>, or H<sub>3</sub><sup>+</sup>.\\ |
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| Contributor(s): H. S. P. Müller; 12, 2013; 06, 2014 | Contributor(s): H. S. P. Müller; 12, 2013; 06, 2014 |
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