Abstract
Context. Methanol, one of the simplest complex organic molecules in the interstellar medium, has been shown to be present and extended in cold environments such as starless cores. Studying the physical conditions at which CH3OH starts its efficient formation is important to understand the development of molecular complexity in star-forming regions. Aims. We aim to study methanol emission across several starless cores and investigate the physical conditions at which methanol starts to be efficiently formed, as well as how the physical structure of the cores and their surrounding environment affect its distribution. Methods. Methanol and C18O emission lines at 3 mm have been observed with the IRAM 30 m telescope within the large programme Gas phase Elemental abundances in Molecular CloudS towards 66 positions across 12 starless cores in the Taurus Molecular Cloud. A non-LTE (local thermodynamic equilibrium) radiative transfer code was used to compute the column densities in all positions. We then used state-of-the-art chemical models to reproduce our observations. Results. We have computed N(CH3OH)/N(C18O) column density ratios for all the observed offsets, and the following two different behaviours can be recognised: the cores where the ratio peaks at the dust peak and the cores where the ratio peaks with a slight offset with respect to the dust peak (~10 000 AU). We suggest that the cause of this behaviour is the irradiation on the cores due to protostars nearby which accelerate energetic particles along their outflows. The chemical models, which do not take irradiation variations into account, can reproduce the overall observed column density of methanol fairly well, but they cannot reproduce the two different radial profiles observed. Conclusions. We confirm the substantial effect of the environment on the distribution of methanol in starless cores. We suggest that the clumpy medium generated by protostellar outflows might cause a more efficient penetration of the interstellar radiation field in the molecular cloud and have an impact on the distribution of methanol in starless cores. Additional experimental and theoretical work is needed to reproduce the distribution of methanol across starless cores.
Highlights
Methanol, CH3OH, and even more complex organic molecules (COMs) have been widely observed in star-forming regions
This holds if we consider B213 and Taurus Molecular Cloud-1 (TMC-1) separately or if we consider solely the column density of methanol instead of the column density ratio with respect to C18O
In the case of multiple velocity components reported for methanol and C18O in Table B.1, we assumed that most of the dust emission comes from the fibre with a larger methanol column density
Summary
CH3OH, and even more complex organic molecules (COMs) have been widely observed in star-forming regions. COMs are defined as organic molecules with ≥6 atoms (van Dishoeck 2009), and their formation is considered to be the first step in the chemical complexity that will eventually be inherited by forming planets in the process of star and planetary system formation. In the past decade several papers have reported on the detection of methanol and other COMs towards starless cores showing that COMs are present and their emission is extended in cold and shielded environments (Bacmann et al 2012; Bizzocchi et al 2014; Vastel et al 2014; JiménezSerra et al 2016; Scibelli & Shirley 2020; Scibelli et al 2021). Starless cores provide the ingredients that will eventually buildup a planet, both the organic as well as the refractory material. Based on observations carried out with the IRAM NOEMA interferometer.
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