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molecules:ism:propin [2020/03/10 14:45] – mueller | molecules:ism:propin [2021/06/14 15:11] – mueller | ||
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in: M.A. Gordon, L.E. Snyder (Eds.), Molecules in the Galactic Environment, | in: M.A. Gordon, L.E. Snyder (Eds.), Molecules in the Galactic Environment, | ||
- | The //J// = 5 – 4 transition with //K// = 0 was observed with the 36 foot (11 m) NRAO dish at 85457.3 MHz toward Sagittarius B. | + | The //J// = 5 – 4 transition with //K// = 0 was observed with the 36 foot (11 m) NRAO dish at 85457.3 MHz toward Sagittarius B.\\ |
J. M. Hollis, L. E. Snyder, D. H. Blake, F. J. Lovas, R. D. Suenram, and B. L. Ulich\\ | J. M. Hollis, L. E. Snyder, D. H. Blake, F. J. Lovas, R. D. Suenram, and B. L. Ulich\\ | ||
identified the //J// = 9 – 8 transitions with //K// = 0 to 3 near 153.8 GHz employing the same instrument in their report on\\ | identified the //J// = 9 – 8 transitions with //K// = 0 to 3 near 153.8 GHz employing the same instrument in their report on\\ | ||
**[[https:// | **[[https:// | ||
- | // | + | // |
E. Churchwell and J. M. Hollis\\ | E. Churchwell and J. M. Hollis\\ | ||
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**[[https:// | **[[https:// | ||
// | // | ||
- | These three high-mass star-forming regions were studied with the same instrument covering the //J// = 5 – 4 and 6 – 5 transitions. | + | These three high-mass star-forming regions were studied with the same instrument covering the //J// = 5 – 4 and 6 – 5 transitions.\\ |
Further sources, including the dark Taurus Molecular Cloud 1 (TMC-1), were studied by\\ | Further sources, including the dark Taurus Molecular Cloud 1 (TMC-1), were studied by\\ | ||
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J. Askne, B. Höglund, Å. Hjalmarson, and W. M. Irvine\\ | J. Askne, B. Höglund, Å. Hjalmarson, and W. M. Irvine\\ | ||
**[[https:// | **[[https:// | ||
- | //Astron. Astrophys.// | + | //Astron. Astrophys.// |
B. E. Turner, E. Herbst, and R. Terzieva\\ | B. E. Turner, E. Herbst, and R. Terzieva\\ | ||
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**[[https:// | **[[https:// | ||
// | // | ||
- | Propyne was detected in the sources CB 17 and CB 228; only an upper limit was determined for CB 24. | + | Propyne was detected in the sources CB 17 and CB 228; only an upper limit was determined for CB 24.\\ |
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**[[https:// | **[[https:// | ||
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
- | refers to the methyl deuterated isotopolog, which was detected with the IRAM 30 m dish in TMC-1. | + | refers to the methyl deuterated isotopolog, which was detected with the IRAM 30 m dish in TMC-1.\\ |
A. J. Markwick, S. B. Charnley, H. M. Butner, T. J. Millar\\ | A. J. Markwick, S. B. Charnley, H. M. Butner, T. J. Millar\\ | ||
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**[[https:// | **[[https:// | ||
// | // | ||
- | The authors used the OSO 20 m dish for a detection in TMC-1. | + | The authors used the OSO 20 m dish for a detection in TMC-1.\\ |
+ | |||
+ | M. Agúndez, E. Roueff, C. Cabezas, J. Cernicharo, and N. Marcelino\\ | ||
+ | reported on the\\ | ||
+ | **[[https:// | ||
+ | //Astron. Astrophys.// | ||
+ | The identifications were made in the course of a molecular line survey of L483 at 3 mm carried out with the IRAM 30 m radio telescope. The survey samples cold material; the presence of the embedded Class 0 infrared source IRAS 18148−0440 is not visible in these data. 9 and 8 //a//-type transition frequencies with 4 ≤ //J// ≤ 7 and // | ||
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- | Contributor(s): | + | Contributor(s): |
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