Differences
This shows you the differences between two versions of the page.
Next revision | Previous revision | ||
molecules:ism:c3_aldehydes [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:c3_aldehydes [2021/07/14 10:59] (current) – mueller | ||
---|---|---|---|
Line 3: | Line 3: | ||
Interestingly, | Interestingly, | ||
W. M. Irvine, R. D. Brown, D. M. Cragg, P. Friberg, P. D. Godfrey, N. Kaifu, H. E. Matthews, M. Ohishi, H. Suzuki, and H. Takeo,\\ | W. M. Irvine, R. D. Brown, D. M. Cragg, P. Friberg, P. D. Godfrey, N. Kaifu, H. E. Matthews, M. Ohishi, H. Suzuki, and H. Takeo,\\ | ||
- | **[[http://cdsads.u-strasbg.fr/ | + | **[[https://ui.adsabs.harvard.edu/ |
// | // | ||
- | The three //J// = 2 – 1 //a//-type transitions around 18.5 GHz were detected with the 43 m NRAO dish. In addition, the 4< | + | The three //J// = 2 – 1 //a//-type transitions around 18.5 GHz were detected with the 43 m NRAO dish. In addition, the 4< |
+ | \\ | ||
The detection of all three aldehydes, propynal, propenal (CH< | The detection of all three aldehydes, propynal, propenal (CH< | ||
J. M. Hollis, P. R. Jewell, F. J. Lovas, A. Remijan, and H. Møllendal, | J. M. Hollis, P. R. Jewell, F. J. Lovas, A. Remijan, and H. Møllendal, | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
- | Absorption as well as emission lines were detected with the 100 m GBT dish between 18 and 26 GHz. This indicates that the molecules reside in the colder and less dense envelope of Sgr B2(N). While the detection of propanal appears to be secure, only two propenal lines have been detected thus far. Therefore, the detection of propenal should be viewed with some caution.However, | + | Absorption as well as emission lines were detected with the 100 m GBT dish between 18 and 26 GHz. This indicates that the molecules reside in the colder and less dense envelope of Sgr B2(N). While the detection of propanal appears to be secure, only two propenal lines have been detected thus far. Therefore, the detection of propenal should be viewed with some caution.However, |
+ | \\ | ||
All three molecule were also reportedly detected in up to three Galactic center molecular clouds which have low dust temperatures (10–20 K), | All three molecule were also reportedly detected in up to three Galactic center molecular clouds which have low dust temperatures (10–20 K), | ||
M. A. Requena-Torres, | M. A. Requena-Torres, | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
- | Two lines each were detected in one source, zero to two lines each in the other two sources. Some caution concerning this report may be useful. | + | Two lines each were detected in one source, zero to two lines each in the other two sources. Some caution concerning this report may be useful.\\ |
+ | \\ | ||
J.-C. Loison, M. Agúndez, N. Marcelino, V. Wakelam, K. M. Hickson, J. Cernicharo, M. Gerin, E. Roueff, and M. Guélin\\ | J.-C. Loison, M. Agúndez, N. Marcelino, V. Wakelam, K. M. Hickson, J. Cernicharo, M. Gerin, E. Roueff, and M. Guélin\\ | ||
reported on\\ | reported on\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
//Mon. Not. R. Astron. Soc.// **456**, 4101–4110 (2016).\\ | //Mon. Not. R. Astron. Soc.// **456**, 4101–4110 (2016).\\ | ||
- | The molecule | + | Propynal |
+ | \\ | ||
J. M. Lykke, A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, R. T. Garrod, H. S. P. Müller, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, | J. M. Lykke, A. Coutens, J. K. Jørgensen, M. H. D. van der Wiel, R. T. Garrod, H. S. P. Müller, P. Bjerkeli, T. L. Bourke, H. Calcutt, M. N. Drozdovskaya, | ||
reported on\\ | reported on\\ | ||
- | **[[http://dx.doi.org/ | + | **[[https:// |
// | // | ||
- | This report is the first one on the detection of warm (~125 K) propanal in the ISM as well as on the detection of propanal around a low-mass protostar. The Protostellar Interferometric Line Survey (PILS) was carried out with ALMA in its Band 7 (329 – 363 GHz). A total of 44 lines were assigned to propanal. | + | This report is the first one on the detection of warm (~125 K) propanal in the ISM as well as on the detection of propanal around a low-mass protostar. The Protostellar Interferometric Line Survey (PILS) was carried out with ALMA in its Band 7 (329 – 363 GHz). A total of 44 lines were assigned to propanal.\\ |
+ | \\ | ||
+ | S. Manigand, A. Coutens, J.-C. Loison, V. Wakelam, H. Calcutt, H. S. P. Müller, J. K. Jørgensen, V. Taquet, S. F. Wampfler, T. L. Bourke, B. M. Kulterer, E. F. van Dishoeck, M. N. Drozdovskaya, | ||
+ | reported on\\ | ||
+ | **[[https:// | ||
+ | // | ||
+ | This report is actually the first one on an umambiguous (i.e. multi line) detection of propenal in the ISM. It is also the first one on the detection of warm (~125 K) propenal in the ISM and on the detection of propanal around a low-mass protostar. The Protostellar Interferometric Line Survey (PILS) was carried out with ALMA in its Band 7 (329 – 363 GHz) with additional observations in Band 6. A total of 15 different unblended (with respect to a different molecule) lines were identified.\\ | ||
---- | ---- | ||
- | Contributor(s): | + | Contributor(s): |
---- | ---- | ||