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molecules:ism:h2co [2019/02/25 22:38] – external edit 127.0.0.1 | molecules:ism:h2co [2019/10/22 17:05] (current) – mueller |
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L. E. Snyder, D. Buhl, B. Zuckerman, and P. Palmer\\ | L. E. Snyder, D. Buhl, B. Zuckerman, and P. Palmer\\ |
reported on the\\ | reported on the\\ |
**[[http://dx.doi.org/10.1103/PhysRevLett.22.679|Microwave Detection of Interstellar Formaldehyde]]**\\ | **[[https://doi.org/10.1103/PhysRevLett.22.679|Microwave Detection of Interstellar Formaldehyde]]**\\ |
//Phys. Rev. Lett.// **22**, 679–681 (1969).\\ | //Phys. Rev. Lett.// **22**, 679–681 (1969).\\ |
The 1<sub>1,0</sub> – 1<sub>1,1</sub> transition near 4830 MHz was detected in absorption with the 43 m NRAO telescope toward numerous continuum sources: M17, W3, W3(OH), W49, NGC 2024, DR 21, W43, W44, W51, Sgr A, Sgr B2, W33, NGC 6334, Cas A, and 3C 123. Formaldehyde was only the third poly-atomic molecule detected in space, the fourth molecule by radio astronomy, and the seventh molecule in space. | The 1<sub>1,0</sub> – 1<sub>1,1</sub> transition near 4830 MHz was detected in absorption with the 43 m NRAO telescope toward numerous continuum sources: M17, W3, W3(OH), W49, NGC 2024, DR 21, W43, W44, W51, Sgr A, Sgr B2, W33, NGC 6334, Cas A, and 3C 123. Formaldehyde was only the third poly-atomic molecule detected in space, the fourth molecule by radio astronomy, and the seventh molecule in space. |
P. Palmer, B. Zuckerman, D. Buhl, and L. E. Snyder\\ | P. Palmer, B. Zuckerman, D. Buhl, and L. E. Snyder\\ |
studied\\ | studied\\ |
**[[http://cdsads.u-strasbg.fr/abs/1969ApJ...156L.147P|Formaldehyde Absorption in Dark Nebulae]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1969ApJ...156L.147P|Formaldehyde Absorption in Dark Nebulae]]**\\ |
//Astrophys. J.// **156**, L147–L150 (1969).\\ | //Astrophys. J.// **156**, L147–L150 (1969).\\ |
The same transition was detected in several positions of Heiles' Cloud 2 with <sup>1</sup>H hyperfine structure resolved in part. | The same transition was detected in several positions of Heiles' Cloud 2 with <sup>1</sup>H hyperfine structure resolved in part. |
A. Heithausen, U. Mebold, and H. W. de Vries\\ | A. Heithausen, U. Mebold, and H. W. de Vries\\ |
performed\\ | performed\\ |
**[[http://cdsads.u-strasbg.fr/abs/1987A%26A...179..263H|A Survey of Formaldehyde in High Galactic Latitudes]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1987A%26A...179..263H|A Survey of Formaldehyde in High Galactic Latitudes]]**\\ |
//Astron. Astrophys.// **179**, 263–267 (1987),\\ | //Astron. Astrophys.// **179**, 263–267 (1987),\\ |
with the Effelsberg 100 m telescope which led to the detection of H<sub>2</sub>CO in translucent clouds. | with the Effelsberg 100 m telescope which led to the detection of H<sub>2</sub>CO in translucent clouds. |
A. G. Nash\\ | A. G. Nash\\ |
studied\\ | studied\\ |
**[[http://cdsads.u-strasbg.fr/abs/1990ApJS...72..303N|The abundance ratio of formaldehyde to ammonia in molecular clouds observed toward radio continuum sources]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1990ApJS...72..303N|The abundance ratio of formaldehyde to ammonia in molecular clouds observed toward radio continuum sources]]**\\ |
//Astrophys. J. Suppl. Ser.// **72**, 303–322 (1990),\\ | //Astrophys. J. Suppl. Ser.// **72**, 303–322 (1990),\\ |
which led to the detection of H<sub>2</sub>CO in diffuse clouds. The Effelsberg 100 m telescope and the 43 m NRAO dish were employed. | which led to the detection of H<sub>2</sub>CO in diffuse clouds. The Effelsberg 100 m telescope and the 43 m NRAO dish were employed. |
J. Cernicharo, M. Guélin, J. Penalver, J. Martín-Pintado, and R. Mauersberger\\ | J. Cernicharo, M. Guélin, J. Penalver, J. Martín-Pintado, and R. Mauersberger\\ |
identified\\ | identified\\ |
**[[http://cdsads.u-strasbg.fr/abs/1989A%26A...222L...1C|A 200 km/s molecular outflow in the protoplanetary nebula CRL 618]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1989A%26A...222L...1C|A 200 km/s molecular outflow in the protoplanetary nebula CRL 618]]**\\ |
//Astron. Astrophys.// **222**, L1–L4 (1989)\\ | //Astron. Astrophys.// **222**, L1–L4 (1989)\\ |
in the course of a 3 and 1.3 mm line survey using the IRAM 30 m telescope. The C-rich PPN is also known as V353 Aur. | in the course of a 3 and 1.3 mm line survey using the IRAM 30 m telescope. The C-rich PPN is also known as V353 Aur. |
M. Lindqvist, H. Olofsson, A. Winnberg, and L.-Å. Nyman\\ | M. Lindqvist, H. Olofsson, A. Winnberg, and L.-Å. Nyman\\ |
investigated\\ | investigated\\ |
**[[http://cdsads.u-strasbg.fr/abs/1992A%26A...263..183L|Carbon-bearing molecules in the envelopes around oxygen-rich stars – First detection of formaldehyde in an oxygen-rich circumstellar envelope]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1992A%26A...263..183L|Carbon-bearing molecules in the envelopes around oxygen-rich stars – First detection of formaldehyde in an oxygen-rich circumstellar envelope]]**\\ |
//Astron. Astrophys.// **263**, 183–189 (1992).\\ | //Astron. Astrophys.// **263**, 183–189 (1992).\\ |
The O-rich CSE was that of the PPN QX Pup, also known as OH231.8+4.2. | The O-rich CSE was that of the PPN QX Pup, also known as OH231.8+4.2. |
K. E. S. Ford, D. A. Neufeld, P. Schilke, and G. J. Melnick\\ | K. E. S. Ford, D. A. Neufeld, P. Schilke, and G. J. Melnick\\ |
reported on the\\ | reported on the\\ |
**[[http://dx.doi.org/10.1086/423886|Detection of Formaldehyde toward the Extreme Carbon Star IRC+10216]]**\\ | **[[https://doi.org/10.1086/423886|Detection of Formaldehyde toward the Extreme Carbon Star IRC+10216]]**\\ |
//Astrophys. J.// **614**, 990–1006 (2004).\\ | //Astrophys. J.// **614**, 990–1006 (2004).\\ |
The source, also known as CW Leo, is an asymptotic giant branch (AGB) star, which is the evolutionary phase prior to the PPN and PN phases. | The source, also known as CW Leo, is an asymptotic giant branch (AGB) star, which is the evolutionary phase prior to the PPN and PN phases. |
L. Velilla Prieto, C. Sánchez Contreras, J. Cernicharo, M. Agúndez, G. Quintana-Lacaci, V. Bujarrabal, J. Alcolea, C. Balanca, F. Herpin, K. M. Menten, and F. Wyrowski\\ | L. Velilla Prieto, C. Sánchez Contreras, J. Cernicharo, M. Agúndez, G. Quintana-Lacaci, V. Bujarrabal, J. Alcolea, C. Balanca, F. Herpin, K. M. Menten, and F. Wyrowski\\ |
mentioned the detection of H<sub>2</sub>CO in the envelope of an O-rich AGB star in\\ | mentioned the detection of H<sub>2</sub>CO in the envelope of an O-rich AGB star in\\ |
**[[http://dx.doi.org/10.1051/0004-6361/201628776|The millimeter IRAM-30 m line survey toward IK Tauri]]**\\ | **[[https://doi.org/10.1051/0004-6361/201628776|The millimeter IRAM-30 m line survey toward IK Tauri]]**\\ |
//Astron. Astrophys.// **597**, Art. No. A25 (2017). | //Astron. Astrophys.// **597**, Art. No. A25 (2017). |
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D. Downes, T. L. Wilson\\ | D. Downes, T. L. Wilson\\ |
in their work on\\ | in their work on\\ |
**[[http://cdsads.u-strasbg.fr/abs/1974ApJ...191L..77D|Formaldehyde Line Emission at 4.8 GHz near NGC 7538]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1974ApJ...191L..77D|Formaldehyde Line Emission at 4.8 GHz near NGC 7538]]**\\ |
//Astrophys. J.// **614**, L77–L78 (1974)\\ | //Astrophys. J.// **614**, L77–L78 (1974)\\ |
employing the Effelsberg 100 m telescope. | employing the Effelsberg 100 m telescope. |
B. Zuckerman, P. Palmer, L. E. Snyder, and D. Buhl\\ | B. Zuckerman, P. Palmer, L. E. Snyder, and D. Buhl\\ |
reported on the\\ | reported on the\\ |
**[[http://cdsads.u-strasbg.fr/abs/1969ApJ...157L.167Z|Detection of Interstellar H<sub>2</sub><sup>13</sup>C<sup>16</sup>O]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1969ApJ...157L.167Z|Detection of Interstellar H<sub>2</sub><sup>13</sup>C<sup>16</sup>O]]**\\ |
//Astrophys. J.// **157**, L167–L171 (1969)\\ | //Astrophys. J.// **157**, L167–L171 (1969)\\ |
in Sgr B2, Sgr A, and possibly W51 using the NRAO 43 m telecope. | in Sgr B2, Sgr A, and possibly W51 using the NRAO 43 m telecope. |
F. F. Gardner, J. C. Ribes, and B. F. C. Cooper\\ | F. F. Gardner, J. C. Ribes, and B. F. C. Cooper\\ |
reported on the\\ | reported on the\\ |
**[[http://cdsads.u-strasbg.fr/abs/1971ApL.....9..181G|Detection of the <sup>18</sup>O Isotop(ologu)e of Formaldehyde at 4388 MHz]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1971ApL.....9..181G|Detection of the <sup>18</sup>O Isotop(ologu)e of Formaldehyde at 4388 MHz]]**\\ |
//Astrophys. Lett.// **157**, 181–183 (1971)\\ | //Astrophys. Lett.// **157**, 181–183 (1971)\\ |
in Sgr B2 using the Parkes 64 m telescope. | in Sgr B2 using the Parkes 64 m telescope. |
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W. D. Langer, M. A. Frerking, R. A. Linke, and R. W. Wilson, reported on the\\ | W. D. Langer, M. A. Frerking, R. A. Linke, and R. W. Wilson, reported on the\\ |
**[[http://cdsads.u-strasbg.fr/abs/1979ApJ...232L.169L|Detection of Deuterated Formaldehyde in Interstellar Clouds]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1979ApJ...232L.169L|Detection of Deuterated Formaldehyde in Interstellar Clouds]]**\\ |
//Astrophys. J.// **157**, L167–L171 (1969).\\ | //Astrophys. J.// **157**, L167–L171 (1969).\\ |
The Bell Lab. 7 m telescope was used to detect the 2<sub>0,2</sub> – 1<sub>0,1</sub> transition near 128813 MHz in emission toward the dark clouds L134 N and Heiles' Cloud 2. | The Bell Lab. 7 m telescope was used to detect the 2<sub>0,2</sub> – 1<sub>0,1</sub> transition near 128813 MHz in emission toward the dark clouds L134 N and Heiles' Cloud 2. |
B. E. Turner\\ | B. E. Turner\\ |
reported on the\\ | reported on the\\ |
**[[http://cdsads.u-strasbg.fr/abs/1990ApJ...362L..29T|Detection of doubly deuterated interstellar formaldehyde (D<sub>2</sub>CO) – an indicator of active grain surface chemistry]]**\\ | **[[https://ui.adsabs.harvard.edu/abs/1990ApJ...362L..29T|Detection of doubly deuterated interstellar formaldehyde (D<sub>2</sub>CO) – an indicator of active grain surface chemistry]]**\\ |
//Astrophys. J.// **362**, L29–L33 (1990).\\ | //Astrophys. J.// **362**, L29–L33 (1990).\\ |
Four transition were detected in emission in the Compact Ridge of Orion KL using the NRAO 12 m telescope. | Four transition were detected in emission in the Compact Ridge of Orion KL using the NRAO 12 m telescope. |
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Contributor(s): H. S. P. Müller; 01, 2017; 03, 2018 | Contributor(s): H. S. P. Müller; 01, 2017; 03, 2018 |
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