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molecules:ism:formamid [2019/03/14 11:42] – update reference admin | molecules:ism:formamid [2019/10/23 22:03] (current) – mueller | ||
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Formamide, HC(O)NH< | Formamide, HC(O)NH< | ||
R. H. Rubin, G. W. Swenson, Jr., R. C. Solomon, and H. L. Flygare,\\ | R. H. Rubin, G. W. Swenson, Jr., R. C. Solomon, and H. L. Flygare,\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
// | // | ||
They detected all three Δ// | They detected all three Δ// | ||
The detection of a second, related, 1 – 1 transition toward Sgr B2 and Sgr A was reported by\\ | The detection of a second, related, 1 – 1 transition toward Sgr B2 and Sgr A was reported by\\ | ||
C. A. Gottlieb, P. Palmer, L. J. Richard, and B. Zuckerman\\ | C. A. Gottlieb, P. Palmer, L. J. Richard, and B. Zuckerman\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
// | // | ||
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A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, H. S. P. Müller, J. M. Lykke, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, | A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, H. S. P. Müller, J. M. Lykke, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, | ||
reported on\\ | reported on\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
Carrying out a line survey toward IRAS 16293-2422 between 329 and 363 GHz, a deuteration degree of about two percent was derived for source B and for all three isotopomers assuming a < | Carrying out a line survey toward IRAS 16293-2422 between 329 and 363 GHz, a deuteration degree of about two percent was derived for source B and for all three isotopomers assuming a < | ||
+ | |||
+ | A. Belloche, R. T. Garrod, H. S. P. Müller, K. M. Menten, I. Medvedev, J. Thomas, and Z. Kisiel\\ | ||
+ | reported on\\ | ||
+ | **[[https:// | ||
+ | //Astron. Astrophys.// | ||
+ | In the course of a new unbiased line survey toward the high-mass star-forming region Sagittarius (Sgr) B2(N) close to the Galactic center, HC(< | ||
The molecule was also detected in several other hot core sources, such as Orion KL, G327.3–0.6, | The molecule was also detected in several other hot core sources, such as Orion KL, G327.3–0.6, | ||
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C. Kahane, C. Ceccarelli, A. Faure, and E. Caux\\ | C. Kahane, C. Ceccarelli, A. Faure, and E. Caux\\ | ||
gave an account on the\\ | gave an account on the\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
The protostar is the usual suspect, IRAS 16293–2422. | The protostar is the usual suspect, IRAS 16293–2422. | ||
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V. Thiel, A. Belloche, K. M. Menten, R. T. Garrod, and H. S. P. Müller,\\ | V. Thiel, A. Belloche, K. M. Menten, R. T. Garrod, and H. S. P. Müller,\\ | ||
reported on\\ | reported on\\ | ||
- | [[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
Four low-//J// //a//-type transitions of formamide were detected with ALMA between 84.5 and 105.5 GHz in absorption in two velocity components corresponding to Galactic center diffuse clouds. The absorption was detected toward the ultracompact H II region K4 in the Sagittarius B2(N) complex.\\ | Four low-//J// //a//-type transitions of formamide were detected with ALMA between 84.5 and 105.5 GHz in absorption in two velocity components corresponding to Galactic center diffuse clouds. The absorption was detected toward the ultracompact H II region K4 in the Sagittarius B2(N) complex.\\ | ||
V. Thiel, A. Belloche, K. M. Menten, A. Giannetti, H. Wiesemeyer, B. Winkel, P. Gratier, H. S. P. Müller, D. Colombo, and R. T. Garrod,\\ | V. Thiel, A. Belloche, K. M. Menten, A. Giannetti, H. Wiesemeyer, B. Winkel, P. Gratier, H. S. P. Müller, D. Colombo, and R. T. Garrod,\\ | ||
continued their investigation of\\ | continued their investigation of\\ | ||
- | [[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
Their statement above was modified such that these complex organic molecules reside in translucent clouds rather than in diffuse and translucent molecular clouds. | Their statement above was modified such that these complex organic molecules reside in translucent clouds rather than in diffuse and translucent molecular clouds. | ||
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R. A. Motiyenko, B. Tercero, J. Cernicharo, and L. Margulès\\ | R. A. Motiyenko, B. Tercero, J. Cernicharo, and L. Margulès\\ | ||
described the\\ | described the\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Astron. Astrophys.// | //Astron. Astrophys.// | ||
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Contributor(s): | Contributor(s): | ||
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