Identified lines of HOCH 2 CN towards SMM1. The observed spectrum is plotted in black, with the best-fit synthetic spectrum overplotted in blue (N T = (7.4±0.9)×10 14 cm −2 , T ex = 260±45 K). The transition is indicated at the top of each panel and the upper state energy is given in the top left of each panel.

Identified lines of HOCH 2 CN towards SMM1. The observed spectrum is plotted in black, with the best-fit synthetic spectrum overplotted in blue (N T = (7.4±0.9)×10 14 cm −2 , T ex = 260±45 K). The transition is indicated at the top of each panel and the upper state energy is given in the top left of each panel.

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Methyl isocyanate (CH$_{3}$NCO) and glycolonitrile (HOCH$_{2}$CN) are isomers and prebiotic molecules that are involved in the formation of peptide structures and the nucleobase adenine, respectively. ALMA observations of the intermediate-mass Class 0 protostar Serpens SMM1-a and ALMA-PILS data of the low-mass Class 0 protostar IRAS~16293B are used...

Contexts in source publication

Context 1
... the spectra of SMM1-a, multiple unblended rotational lines of the isomers HOCH 2 CN and CH 3 NCO ν=0 are found. Moment 0 maps (the spatial mapping of the integrated line intensity of a single rotational line) of both species show that most emission originates from SMM1-a, see Fig. 2. The identified lines towards SMM1-a are presented in Figs. 4 Table 5. Following the procedure detailed in Sect. 2.3, the best-fit parameters of these species are determined. For undetected species, upper limit column densities are determined by assuming T ex = 200 K, which is chosen as a representative excitation temperature from the molecules that are detected. The fit parameters are presented ...
Context 2
... with a very different physical structure and can therefore not directly be compared with the hot core and corino sources. The highest ratio is found towards G10.47+0.03, but the analysis of HNCO in this source is likely performed on optically thick HNCO lines and the analysis seems to underestimate the HNCO column density in this source (see Fig. 4 in Gorai et al. 2020). Removing these results from the analysis, a correlation between CH 3 NCO and HNCO is found, which may indicate a chemical link between CH 3 NCO and HNCO. Furthermore, this correlation spans a variety of sources of different masses and over four order of magnitude in luminosities. This results in different ...