Formamide, HC(O)NH2, is a fairly typical hot core molecule
that is quite abundant. The first transition of this molecule was
detected toward Sgr B2 and likely toward Sgr A by
R. H. Rubin, G. W. Swenson, Jr., R. C. Solomon, and H. L. Flygare,
Microwave Detection of Interstellar Formamide
Astrophys. J. 169, L39–L43 (1971).
They detected all three ΔF = 0 hyperfine components of the Ka = 1, J = 2 – 2 transition near 4619 MHz. Only the strongest component, overlapped in part with the H112α transition, was tentatively detected toward Sgr A.
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
Studies of Interstellar Formamide
Astrophys. J. 182, 699–710 (1973).
Detection of the 13C Isotope of Formamide in the Galactic Center
was described by
B. Lazareff, R. Lucas, and P. Encrenaz,
Astron. Astrophys. 70, L77–L78 (1978).
The F = 2 – 2 HFS component of the J = 1 – 1 transitions was observed near 1571 GHz toward Sgr B2.
The molecule was also detected in several other hot core sources, such as Orion KL, G327.3–0.6, G34_3+0.15, and NGC 6334(I).
C. Kahane, C. Ceccarelli, A. Faure, and E. Caux reported on
Detection of Formamide, the Simplest but Crucial Amide, in a Solar-type Protostar
Astrophys. J. 763, Art. No. L38 (2013).
The Solar proto-star is the usual suspect, IRAS 16293–2422.
R. A. Motiyenko, B. Tercero, J. Cernicharo, and L. Margulès
reported on the
Rotational Spectrum of Formamide up to 1 THz and First ISM Detection of its v12 Vibrational State
Astron. Astrophys. 548, Art. No. A71 (2012).
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, C. Favre,
E. C. Fayolle, R. T. Garrod, S. K. Jacobsen, N. F. W. Ligterink, K. I. Öberg,
M. V. Persson, E. F. van Dishoeck, and S. F. Wampfler
The ALMA-PILS Survey: First Detections of Deuterated Formamide and Deuterated Isocyanic Acid in the Interstellar Medium
Astron. Astrophys. 590, Art. No. L6 (2016).
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 12C/13C ratio of 68 because lines of the main isotopolog are frequently affected by optical depth effects.