Seeds of Life in Space (SOLIS)

V. Methanol and acetaldehyde in the protostellar jet-driven shocks L1157-B0 and B1

¹ INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
e-mail: codella@arcetri.astro.it
² Univ. Grenoble Alpes, CNRS, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG), 38000 Grenoble, France
³ Dipartimento di Chimica, Biologia e Biotecnologie, Via Elce di Sotto 8, 06123 Perugia, Italy
⁴ Max-Planck-Institut für extraterrestrische Physik (MPE), Giessenbachstrasse 1, 85748 Garching, Germany
⁵ National Astronomical Observatory of China, Datun Road 20, Chaoyang, Beijing 100012, PR China
⁶ CAS Key Laboratory of FAST, NAOC, Chinese Academy of Sciences, Chaoyang, PR China
⁷ National Astronomical Observatory of Japan, 2 Chome-21-1 Osawa, Mitaka-shi, Tokyo-to 181-0015, Japan
⁸ Institut de Radioastronomie Millimétrique, 300 rue de la Piscine, Domaine Universitaire de Grenoble, 38406 Saint-Martin d’Hères, France

Received: 18 September 2019
Accepted: 23 December 2019

Abstract

Context. It is nowadays clear that a rich organic chemistry takes place in protostellar regions. However, the processes responsible for it, that is, the dominant formation routes to interstellar complex organic molecules, are still a source of debate. Two paradigms have been evoked: the formation of these molecules on interstellar dust mantles and their formation in the gas phase from simpler species previously synthesised on the dust mantles.

Aims. In the past, observations of protostellar shocks have been used to set constraints on the formation route of formamide (NH₂CHO), exploiting its observed spatial distribution and comparison with astrochemical model predictions. In this work, we follow the same strategy to study the case of acetaldehyde (CH₃CHO).

Methods. To this end, we used the data obtained with the IRAM-NOEMA interferometer in the framework of the Large Program SOLIS to image the B0 and B1 shocks along the L1157 blueshifted outflow in methanol (CH₃OH) and acetaldehyde line emission.

Results. We imaged six CH₃OH and eight CH₃CHO lines which cover upper-level energies up to ~30 K. Both species trace the B0 molecular cavity as well as the northern B1 portion, that is, the regions where the youngest shocks (~1000 yr) occurred. The CH₃OH and CH₃CHO emission peaks towards the B1b clump, where we measured the following column densities and relative abundances: 1.3 × 10¹⁶ cm⁻² and 6.5 × 10⁻⁶ (methanol), and 7 × 10¹³ cm⁻² and 3.5 × 10⁻⁸ (acetaldehyde). We carried out a non-LTE (non-Local Thermodinamic Equilibrium) Large Velocity Gradient (LVG) analysis of the observed CH₃OH line: the average kinetic temperature and density of the emitting gas are T_kin ~ 90 K and n_H2 ~ 4 × 10⁵ cm⁻³, respectively. The CH₃OH and CH₃CHO abundance ratio towards B1b is 190, varying by less than a factor three throughout the whole B0–B1 structure.

Conclusions. Comparison of astrochemical model predictions with the observed methanol and acetaldehyde spatial distribution does not allow us to distinguish whether acetaldehyde is formed on the grain mantles or in the gas phase, as its gas-phase formation, which is dominated by the reaction of ethyl radical (CH₃CH₂) with atomic oxygen, is very fast. Observations of acetaldehyde in younger shocks, for example those of ~10² yr old, and/or of the ethyl radical, whose frequencies are not presently available, are necessary to settle the issue.