The ALMA-PILS survey: propyne (CH₃CCH) in IRAS 16293–2422

Calcutt, H.; Willis, E. R.; Jørgensen, J. K.; Bjerkeli, P.; Ligterink, N. F. W.; Coutens, A.; Müller, H. S. P.; Garrod, R. T.; Wampfler, S. F.; Drozdovskaya, M. N. (2019). The ALMA-PILS survey: propyne (CH₃CCH) in IRAS 16293–2422. Astronomy and astrophysics, 631(A137), A137. EDP Sciences 10.1051/0004-6361/201936323

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Context. Propyne (CH₃CCH), also known as methyl acetylene, has been detected in a variety of environments, from Galactic star-forming regions to extragalactic sources. These molecules are excellent tracers of the physical conditions in star-forming regions, allowing the temperature and density conditions surrounding a forming star to be determined.

Aims. This study explores the emission of CH₃CCH in the low-mass protostellar binary, IRAS 16293–2422, and examines the spatial scales traced by this molecule, as well as its formation and destruction pathways.

Methods. Atacama Large Millimeter/submillimeter Array (ALMA) observations from the Protostellar Interferometric Line Survey (PILS) were used to determine the abundances and excitation temperatures of CH₃CCH towards both protostars. This data allows us to explore spatial scales from 70 to 2400 au. This data is also compared with the three-phase chemical kinetics model MAGICKAL, to explore the chemical reactions of this molecule.

Results. CH₃CCH is detected towards both IRAS 16293A and IRAS 16293B, and is found the hot corino components, one around each source, in the PILS dataset. Eighteen transitions above 3σ are detected, enabling robust excitation temperatures and column densities to be determined in each source. In IRAS 16293A, an excitation temperature of 90 K and a column density of 7.8 × 10¹⁵ cm⁻² best fits the spectra. In IRAS 16293B, an excitation temperature of 100 K and 6.8 × 10¹⁵ cm⁻² best fits the spectra. The chemical modelling finds that in order to reproduce the observed abundances, both gas-phase and grain-surface reactions are needed. The gas-phase reactions are particularly sensitive to the temperature at which CH4 desorbs from the grains.

Conclusions. CH₃CCH is a molecule whose brightness and abundance in many different regions can be utilised to provide a benchmark of molecular variation with the physical properties of star-forming regions. It is essential when making such comparisons, that the abundances are determined with a good understanding of the spatial scale of the emitting region, to ensure that accurate abundances are derived.

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