Astronomy and Astrophysics, volume 626A, 132-132 (2019/6-1)
Molecular analysis of a high-mass prestellar core candidate in W43-MM1.
MOLET J., BROUILLET N., NONY T., GUSDORF A., MOTTE F., DESPOIS D., LOUVET F., BONTEMPS S. and HERPIN F.
Abstract (from CDS):
Context. High-mass analogues of low-mass prestellar cores are searched for to constrain the models of high-mass star formation. Several high-mass cores, at various evolutionary stages, have been recently identified towards the massive star-forming region W43-MM1 and amongst them a high-mass prestellar core candidate.
Aims. We aim to characterise the chemistry in this high-mass prestellar core candidate, referred to as W43-MM1 core #6, and its environment.
Methods. Using ALMA high-spatial resolution data of W43-MM1, we have studied the molecular content of core #6 and a neighbouring high-mass protostellar core, referred to as #3, which is similar in size and mass to core #6. We first subtracted the continuum emission using a method based on the density distribution of the intensities on each pixel. Then, from the distribution of detected molecules, we identified the molecules centred on the prestellar core candidate (core #6) and those associated to shocks related to outflows and filament formation. Then we constrained the column densities and temperatures of the molecules detected towards the two cores.
Results. While core #3 appears to contain a hot core with a temperature of about 190K, core #6 seems to have a lower temperature in the range from 20 to 90K from a rotational diagram analysis. We have considered different source sizes for core #6 and the comparison of the abundances of the detected molecules towards the core with various interstellar sources shows that it is compatible with a core of size 1000 au with T=20-90K or a core of size 500 au with T∼80K.
Conclusions. Core #6 of W43-MM1 remains one of the best high-mass prestellar core candidates even if we cannot exclude that it is at the very beginning of the protostellar phase of high-mass star formation.
© J. Molet et al. 2019
stars: formation - stars: massive - ISM: abundances - ISM: molecules - radio lines: ISM
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